@article{ ISI:000609014700006, Author = {Datta, Sayantani and Gupta, Anuradha and Kastha, Shilpa and Arun, K. G. and Sathyaprakash, B. S.}, Title = {{Tests of general relativity using multiband observations of intermediate mass binary black hole mergers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2021}}, Volume = {{103}}, Number = {{2}}, Month = {{JAN 20}}, Abstract = {{Observation of gravitational waves (GWs) in two different frequency bands is referred to as multiband GW astronomy. With the planned Laser Interferometric Space Antenna (LISA) operating in the 10(-4)-0.1 Hz range, and third-generation (3G) ground-based detectors such as the Cosmic Explorer (CE) and Einstein Telescope (ET) operating in the 1-10(4) Hz range, multiband GWastronomy could be a reality in the coming decades. In this paper, we present the potential of multiband observations of intermediate-mass binary black holes (IMBBHs) of component masses similar to 10(2)-10(3) M-circle dot to test general relativity (GR). We show that mutiband observations of IMBBHs would permit multiparameter tests of GR-tests where more than one post-Newtonian (PN) coefficient is simultaneously measured-yielding more rigorous constraints on possible modifications to GR. We also find that the improvement due to multibanding can often be much larger than the best of the bounds from either of the two observatories. The origin of this result, as we shall demonstrate, can be traced to the lifting of degeneracies among the various parameters when the information from LISA and 3G is taken together. Abinary of redshifted total mass of 200 M-circle dot gives the best bounds. Such a system at 1 Gpc and mass ratio m(1)/m (2) = 2 would bound the deviations on all the PN coefficients to below 10\% when they are measured individually, and additionally place simultaneous bounds on the first seven PNcoefficients to below 50\%.}}, DOI = {{10.1103/PhysRevD.103.024036}}, Article-Number = {{024036}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000609014700006}}, } @article{ ISI:000610446600004, Author = {Zheng, Xiaogang and Cao, Shuo and Liu, Yuting and Biesiada, Marek and Liu, Tonghua and Geng, Shuaibo and Lian, Yujie and Guo, Wuzheng}, Title = {{Model-independent constraints on cosmic curvature: implication from the future space gravitational-wave antenna DECIGO}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2021}}, Volume = {{81}}, Number = {{1}}, Month = {{JAN 11}}, Abstract = {{In order to estimate cosmic curvature from cosmological probes like standard candles, one has to measure the luminosity distance D-L(z), its derivative with respect to redshift DL `(z) and the expansion rate H(z) at the same redshift. In this paper, we study how such idea could be implemented with future generation of space-based DECi-hertz Interferometer Gravitational-wave Observatory (DECIGO), in combination with cosmic chronometers providing cosmology-independent H(z) data. Our results show that for the Hubble diagram of simulated DECIGO data acting as a new type of standard siren, it would be able to constrain cosmic curvature with the precision of Delta Omega(k) = 0.09 with the currently available sample of 31 measurements of Hubble parameters. In the framework of the third generation ground-based gravitational wave detectors, the spatial curvature is constrained to be Delta Omega(k) = 0.13 for Einstein Telescope (ET). More interestingly, compared to other approaches aiming for model-independent estimations of spatial curvature, our analysis also achieve the reconstruction of the evolution of Omega(k)(z), in the framework of a model-independent method of Gaussian processes (GP) without assuming a specific form. Therefore, one can expect that the newly emerged gravitational wave astronomy can become useful in local measurements of cosmic curvature using distant sources.}}, DOI = {{10.1140/epjc/s10052-020-08796-w}}, Article-Number = {{14}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, Unique-ID = {{ISI:000610446600004}}, } @article{ ISI:000604831200003, Author = {Rowlinson, Samuel and Dmitriev, Artemiy and Jones, Aaron W. and Zhang, Teng and Freise, Andreas}, Title = {{Feasibility study of beam-expanding telescopes in the interferometer arms for the Einstein Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2021}}, Volume = {{103}}, Number = {{2}}, Month = {{JAN 5}}, Abstract = {{The optical design of the Einstein Telescope (ET) is based on a dual-recycled Michelson interferometer with Fabry-Perot cavities in the arms. ET will be constructed in a new infrastructure, allowing us to consider different technical implementations beyond the constraints of the current facilities. In this paper we investigate the feasibility of using beam-expander telescopes in the interferometer arms. We provide an example implementation that matches the optical layout as presented in the ET design update 2020. We further show that the beam-expander telescopes can be tuned to compensate for mode mismatches between the arm cavities and the rest of the interferometer.}}, DOI = {{10.1103/PhysRevD.103.023004}}, Article-Number = {{023004}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Dmitriev, Artemiy/AAE-8933-2021 }}, ORCID-Numbers = {{Dmitriev, Artemiy/0000-0002-0314-956X Jones, Aaron/0000-0002-0395-0680}}, Unique-ID = {{ISI:000604831200003}}, } @article{ ISI:000606812500005, Author = {Di Giovanni, Matteo and Giunchi, Carlo and Saccorotti, Gilberto and Berbellini, Andrea and Boschi, Lapo and Olivieri, Marco and De Rosa, Rosario and Naticchioni, Luca and Oggiano, Giacomo and Carpinelli, Massimo and D'Urso, Domenico and Cuccuru, Stefano and Sipala, Valeria and Calloni, Enrico and Di Fiore, Luciano and Grado, Aniello and Migoni, Carlo and Cardini, Alessandro and Paoletti, Federico and Fiori, Irene and Harms, Jan and Majorana, Ettore and Rapagnani, Piero and Ricci, Fulvio and Punturo, Michele}, Title = {{A Seismological Study of the Sos Enattos Area-the Sardinia Candidate Site for the Einstein Telescope}}, Journal = {{SEISMOLOGICAL RESEARCH LETTERS}}, Year = {{2021}}, Volume = {{92}}, Number = {{1}}, Pages = {{352-364}}, Month = {{JAN}}, Abstract = {{The recent discovery of gravitational waves (GWs) and their potential for cosmic observations prompted the design of the future third-generation GW interferometers, able to extend the observation distance for sources up to the frontier of the Universe. In particular, the European detector Einstein Telescope (ET) has been proposed to reach peak strain sensitivities of about 3 x 10(-25)Hz-(1/2) in the 100 Hz frequency region and to extend the detection band down to 1 Hz. In the bandwidth {[}1,10] Hz, the seismic ambient noise is expected to represent the major perturbation to interferometric measurements, and the site that will host the future detectors must fulfill stringent requirements on seismic disturbances. In this article, we conduct a seismological study at the Italian ET candidate site, the dismissed mine of Sos Enattos in Sardinia. In the range between few mHz to hundreds of mHz, out of the detection bandwidth for ET, the seismic noise is compatible with the new low-noise model (Peterson, 1993); in the {[}0.1,1] Hz bandwidth, we found that seismic noise is correlated with sea wave height in the northwestern Mediterranean Sea. In the {[}1,10] Hz frequency band, noise is mainly due to anthropic activities; within the mine tunnels (similar or equal to 100 m underground), its spectrum is compliant with the requirements of the ET design. Noise amplitude decay with depth is consistent with a dominance of Rayleigh waves, as suggested by synthetic seismograms calculated for a realistic velocity structure obtained from the inversion of phaseand group-velocity dispersion data from array recording of a mine blasting. Further investigations are planned for a quantitative assessment of the principal noise sources and their spatiotemporal variations.}}, DOI = {{10.1785/0220200186}}, ISSN = {{0895-0695}}, EISSN = {{1938-2057}}, Unique-ID = {{ISI:000606812500005}}, } @article{ ISI:000605983200092, Author = {Valiante, Rosa and Colpi, Monica and Schneider, Raffaella and Mangiagli, Alberto and Bonetti, Matteo and Cerini, Giulia and Fairhurst, Stephen and Haardt, Francesco and Mills, Cameron and Sesana, Alberto}, Title = {{Unveiling early black hole growth with multifrequency gravitational wave observations}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2021}}, Volume = {{500}}, Number = {{3}}, Pages = {{4095-4109}}, Month = {{JAN}}, Abstract = {{Third-generation ground-based gravitational wave interferometers, like the Einstein Telescope (ET), Cosmic Explorer, and the Laser Interferometer Space Antenna (LISA), will detect coalescing binary black holes over a wide mass spectrum and across all cosmic epochs. We track the cosmological growth of the earliest light and heavy seeds that swiftly transit into the supermassive domain using a semi-analytical model for the formation of quasars at z = 6.4, 2, and 0.2, in which we follow black hole coalescences driven by triple interactions. We find that light-seed binaries of several 10(2) M-circle dot are accessible to ET with a signal-to-noise ratio (S/N) of 10-20 at 6 < z < 15. They then enter the LISA domain with larger S/N as they grow to a few 10(4) M-circle dot. Detecting their gravitational signal would provide first time evidence that light seeds form, grow, and dynamically pair during galaxy mergers. The electromagnetic emission of accreting black holes of similar mass and redshift is too faint to be detected even for the deepest future facilities. ET will be our only chance to discover light seeds forming at cosmic dawn. At 2 < z < 8, we predict a population of `starved binaries', long-lived marginally growing light-seed pairs, to be loud sources in the ET bandwidth (S/N > 20). Mergers involving heavy seeds (similar to 10(5)-10(6) M-circle dot) would be within reach up to z = 20 in the LISA frequency domain. The lower z model predicts 11.25 (18.7) ET (LISA) events per year, overall.}}, DOI = {{10.1093/mnras/staa3395}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, Unique-ID = {{ISI:000605983200092}}, } @article{ ISI:000606024200001, Author = {Lin, Hai-Nan and Li, Xin and Tang, Li}, Title = {{Strongly lensed gravitational waves as probes to test the cosmic distance duality relation}}, Journal = {{CHINESE PHYSICS C}}, Year = {{2021}}, Volume = {{45}}, Number = {{1}}, Month = {{JAN}}, Abstract = {{The cosmic distance relation (DDR) associates the angular diameters distance (D-A) and luminosity distance (D-L) by a simple formula, i.e., D-L = (1+z+)D-2(A). The strongly lensed gravitational waves (GWs) provide a unique way to measure D-A and D-L simultaneously to the GW source, hence they can be used as probes to test DDR. In this study, we investigated the use of strongly lensed GW events from the future Einstein Telescope to test DDR. We assumed the possible deviation of DDR as (1+z)D-2(A)/D-L = eta(z), and considered two different parametrizations of eta(z), namely, eta(1)(z) = 1 + eta(0)z and eta(2)(z) = 1 eta(0)(z)/(1+z). Numerical simulations showed that, with about 100 strongly lensed GW events observed by ET, the parameter eta(0) was constrained at 1.3\% and 3\% levels for the first and second parametrizations, respectively.}}, DOI = {{10.1088/1674-1137/abc53a}}, Article-Number = {{015109}}, ISSN = {{1674-1137}}, EISSN = {{2058-6132}}, ORCID-Numbers = {{Lin, Hai-Nan/0000-0003-1659-3368}}, Unique-ID = {{ISI:000606024200001}}, } @article{ ISI:000595643500001, Author = {Pagano, G. and Hannuksela, O. A. and Li, T. G. F.}, Title = {{LENSINGGW: a PYTHON package for lensing of gravitational waves}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2020}}, Volume = {{643}}, Month = {{NOV 20}}, Abstract = {{Advanced LIGO and Advanced Virgo might be able to observe the first lensed gravitational waves in the coming years. With the addition of the KAGRA and LIGO India detectors to the detector network and with the future construction of the Einstein Telescope we might be able to observe hundreds of lensed events. Ground-based gravitational-wave detectors can resolve arrival-time differences on the order of the inverse of the observed frequencies. The LIGO and Virgo frequency band spans from a few Hz to a few kHz, therefore the typical time resolution of current interferometers is on the order of milliseconds. When microlenses are embedded in galaxies or galaxy clusters, lensing can become more prominent and result in observable time delays at LIGO and Virgo frequencies. Therefore, gravitational waves might offer an exciting alternative probe of microlensing. However, only a few lensing configurations have currently been worked out in the context of gravitational-wave lensing. In this paper, we present LENSINGGW, a PYTHON package designed to handle both strong lensing and microlensing of compact binaries and the related gravitational-wave signals in the geometrical optics limit. This synergy paves the way for systematic parameter space investigations and for the detection of arbitrary lens configurations and compact sources. Here we focus on the LIGO and Virgo frequencies. We demonstrate the working mechanism of LENSINGGW and its use in studying microlenses that are embedded in galaxies.}}, DOI = {{10.1051/0004-6361/202038730}}, Article-Number = {{A167}}, ISSN = {{0004-6361}}, EISSN = {{1432-0746}}, ORCID-Numbers = {{Hannuksela, Otto Akseli/0000-0002-3887-7137}}, Unique-ID = {{ISI:000595643500001}}, } @article{ ISI:000589610300005, Author = {Kleybolte, L. and Gewecke, P. and Sawadsky, A. and Korobko, M. and Schnabel, R.}, Title = {{Squeezed-Light Interferometry on a Cryogenically Cooled Micromechanical Membrane}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2020}}, Volume = {{125}}, Number = {{21}}, Month = {{NOV 16}}, Abstract = {{Squeezed states of light reduce the signal-normalized photon counting noise of measurements without increasing the light power and enable fundamental research on quantum entanglement in hybrid systems of light and matter. Squeezed states of light have high potential to complement cryogenically cooled sensors, whose thermal noise is suppressed below the quantum noise of light by operation at low temperature. They allow us to reduce the optical heat load on cooled devices by lowering the light power without losing measurement precision. Here, we demonstrate the squeezed-light position sensing of a cryo-cooled micromechanical membrane. The sensing precision is improved by up to 4.8 dB below photon counting noise, limited by optical loss, at a membrane temperature of about 20 K. We prove that realizing a high interference contrast in a cryogenic Michelson interferometer is feasible. Our setup is the first conceptual demonstration towards the envisioned European gravitational-wave detector, the ``Einstein telescope,{''} which is planned to use squeezed states of light together with cryo-cooled mirror test masses.}}, DOI = {{10.1103/PhysRevLett.125.213601}}, Article-Number = {{213601}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Korobko, Mikhail/ABD-8704-2020}}, ORCID-Numbers = {{Korobko, Mikhail/0000-0002-3839-3909}}, Unique-ID = {{ISI:000589610300005}}, } @article{ ISI:000588241100003, Author = {Pan, Zhen and Lyu, Zhenwei and Bonga, Beatrice and Ortiz, Nestor and Yang, Huan}, Title = {{Probing Crust Meltdown in Inspiraling Binary Neutron Stars}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2020}}, Volume = {{125}}, Number = {{20}}, Month = {{NOV 10}}, Abstract = {{Thanks to recent measurements of tidal deformability and radius, the nuclear equation of state and structure of neutron stars are now better understood. Here, we show that through resonant tidal excitations in a binary inspiral, the neutron crust generically undergoes elastic-to-plastic transition, which leads to crust heating and eventually meltdown. This process could induce similar to O(0.1) phase shift in the gravitational waveform. Detecting the timing and induced phase shift of this crust meltdown will shed light on the crust structure, such as the core-crust transition density, which previous measurements are insensitive to. A direct search using GW170817 data has not found this signal, possibly due to limited signal-to-noise ratio. We predict that such a signal may be observable with Advanced LIGO Plus and more likely with third-generation gravitational-wave detectors such as the Einstein Telescope and Cosmic Explorer.}}, DOI = {{10.1103/PhysRevLett.125.201102}}, Article-Number = {{201102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, Unique-ID = {{ISI:000588241100003}}, } @article{ ISI:000584364000013, Author = {Mitman, Keefe and Moxon, Jordan and Scheel, Mark A. and Teukolsky, Saul A. and Boyle, Michael and Deppe, Nils and Kidder, Lawrence E. and Throwe, William}, Title = {{Computation of displacement and spin gravitational memory in numerical relativity}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{10}}, Month = {{NOV 2}}, Abstract = {{We present the first numerical relativity waveforms for binary black hole mergers produced using spectral methods that show both the displacement and the spin memory effects. Explicitly, we use the SXS (Simulating eXtreme Spacetimes) Collaboration's SPEC code to run a Cauchy evolution of a binary black hole merger and then extract the gravitational wave strain using SpECTRE'S version of a Cauchy-characteristic extraction. We fmd that we can accurately resolve the strain's traditional m = 0 memory modes and some of the m not equal 0 oscillatory memory modes that have previously only been theorized. We also perform a separate calculation of the memory using equations for the Bondi-Metzner-Sachs charges as well as the energy and angular momentum fluxes at asymptotic infinity. Our new calculation uses only the gravitational wave strain and two of the Weyl scalars at infinity. Also, this computation shows that the memory modes can be understood as a combination of a memory signal throughout the binary's inspiral and merger phases, and a quasinormal mode signal near the ringdown phase. Additionally, we find that the magnetic memory, up to numerical error, is indeed zero as previously conjectured. Last, we find that signal-to-noise ratios of memory for LIGO, the Einstein Telescope, and the Laser Interferometer Space Antenna with these new waveforms and new memory calculation are larger than previous expectations based on post-Newtonian or minimal waveform models.}}, DOI = {{10.1103/PhysRevD.102.104007}}, Article-Number = {{104007}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Kidder, Lawrence/0000-0001-5392-7342 Mitman, Keefe/0000-0003-0276-3856}}, Unique-ID = {{ISI:000584364000013}}, } @article{ ISI:000610048900003, Author = {Zhang, Sixuan and Cao, Shuo and Zhang, Jia and Liu, Tonghua and Liu, Yuting and Geng, Shuaibo and Lian, Yujie}, Title = {{A model-independent constraint on the Hubble constant with gravitational waves from the Einstein Telescope}}, Journal = {{INTERNATIONAL JOURNAL OF MODERN PHYSICS D}}, Year = {{2020}}, Volume = {{29}}, Number = {{15}}, Month = {{NOV}}, Abstract = {{In this paper, we investigate the expected constraints on the Hubble constant from the gravitational-wave standard sirens, in a cosmological-model-independent way. In the framework of the well-known Hubble law, the GW signal from each detected binary merger in the local universe (z < 0.10) provides a measurement of luminosity distance DL and thus the Hubble constant H-0. Focusing on the simulated data of gravitational waves from the third-generation gravitational wave detector (the Einstein Telescope, ET), combined with the redshifts determined from electromagnetic counter parts and host galaxies, one can expect the Hubble constant to be constrained at the precision of similar to 10(-2) with 20 well-observed binary neutron star (BNS) mergers. Additional standard-siren measurements from other types of future gravitational-wave sources (NS-BH and BBH) will provide more precision constraints of this important cosmological parameter. Therefore, we obtain that future measurements of the luminosity distances of gravitational waves sources will be much more competitive than the current analysis, which makes it expectable more vigorous and convincing constraints on the Hubble constant in a cosmological-model-independent way.}}, DOI = {{10.1142/S0218271820501059}}, Article-Number = {{2050105}}, ISSN = {{0218-2718}}, EISSN = {{1793-6594}}, Unique-ID = {{ISI:000610048900003}}, } @article{ ISI:000593526400001, Author = {Yun, Qian-Yun and Han, Wen-Biao and Wang, Gang and Yang, Shu-Cheng}, Title = {{Estimating up-limits of eccentricities for the binary black holes in the LIGO-Virgo catalog GWTC-1}}, Journal = {{RESEARCH IN ASTRONOMY AND ASTROPHYSICS}}, Year = {{2020}}, Volume = {{20}}, Number = {{11}}, Month = {{NOV}}, Abstract = {{In the first Gravitational-Wave Transient Catalogue of LIGO and Virgo, all events are announced having zero eccentricity. In the present paper, we investigate the performance of SEOBNRE, which is a spin-aligned eccentric waveform model in time-domain. By comparing with all the eccentric waveforms in SXS library, we find that the SEOBNRE coincides perfectly with numerical relativity data. Employing the SEOBNRE, we re-estimate the eccentricities of all black hole merger events. We find that most of these events allow a possibility for existence of initial eccentricities at 10 Hz band, but are totally circularized at the observed frequency (greater than or similar to 20 Hz). The upcoming update of LIGO and the next generation detector like Einstein Telescope will observe the gravitational waves starting at 10 Hz or even lower. If the eccentricity exists at the lower frequency, then it may significantly support the dynamical formation mechanism taking place in globular clusters.}}, DOI = {{10.1088/1674-4527/20/11/183}}, Article-Number = {{183}}, ISSN = {{1674-4527}}, EISSN = {{2397-6209}}, Unique-ID = {{ISI:000593526400001}}, } @article{ ISI:000587752500006, Author = {Yim, Garvin and Jones, I, D.}, Title = {{Transient gravitational waves from pulsar post-glitch recoveries}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{498}}, Number = {{3}}, Pages = {{3138-3152}}, Month = {{NOV}}, Abstract = {{This work explores whether gravitational waves (GWs) from neutron star (NS) mountains can be detected with current second-generation and future third-generation GW detectors. In particular, we focus on a scenario where transient mountains are formed immediately after an NS glitch. In a glitch, an NS's spin frequency abruptly increases and then often exponentially recovers back to, but never quite reaches, the spin frequency prior to the glitch. If the recovery is ascribed to an additional torque due to a transient mountain, we find that GWs from that mountain are marginally detectable with Advanced LIGO at design sensitivity and is very likely to be detectable for third-generation detectors such as the Einstein Telescope. Using this model, we are able to find analytical expressions for the GW amplitude and its duration in terms of observables.}}, DOI = {{10.1093/mnras/staa2534}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Jones, David/0000-0002-0117-7567 Yim, Garvin/0000-0001-8548-9535}}, Unique-ID = {{ISI:000587752500006}}, } @article{ ISI:000587752500068, Author = {Kinugawa, Tomoya and Nakamura, Takashi and Nakano, Hiroyuki}, Title = {{Chirp mass and spin of binary black holes from first star remnants}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{498}}, Number = {{3}}, Pages = {{3946-3963}}, Month = {{NOV}}, Abstract = {{We performed Population III (Pop III) binary evolution using population synthesis simulations for seven different models. We found that Pop III binaries tend to be binary black holes (BBHs) with chirp mass M-chirp similar to 30 M-circle dot and they can merge in the present day, due to a long merger time. The merger rate densities of Pop III BBHs at z = 0 are in the range 3.34-21.2 yr(-1) Gpc(-3) which is consistent with the Advanced Laser Interferometer Gravitational Wave Observatory (aLIGO)/Advanced Virgo (aVIRGO) result of 9.7-101 yr(-1) Gpc(-3). These Pop III binaries might contribute some portion of the massive BBH gravitational wave (GW) sources detected by aLIGO/aVIRGO. We also calculated the redshift dependence of Pop III BBH mergers. We found that Pop III low-spin BBHs tend to merge at low redshift, while Pop III high-spin BBHs merge at high redshift, which can be confirmed by future GW detectors such as Einstein Telescope (ET), Cosmic Explorer (CE), and DECi-hertz Interferometer Gravitational wave Observatory (DECIGO). These detectors can also check the redshift dependence of the BBH merger rate and spin distribution. Our results show that, except for one model, the mean effective spin at z = 0 lies in the range 0.02-0.3, while at z = 10 it is 0.16-0.64. Therefore, massive stellar-mass BBH detection by GWs will be key for stellar evolution study in the early Universe.}}, DOI = {{10.1093/mnras/staa2511}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Kinugawa, Tomoya/0000-0002-3033-4576 Nakano, Hiroyuki/0000-0001-7665-0796}}, Unique-ID = {{ISI:000587752500068}}, } @article{ ISI:000574337700001, Author = {Sullivan, Andrew G. and Veske, Doga and Marka, Zsuzsa and Bartos, Imre and Ballmer, Stefan and Shawhan, Peter and Marka, Szabolcs}, Title = {{Can we use next-generation gravitational wave detectors for terrestrial precision measurements of Shapiro delay?}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2020}}, Volume = {{37}}, Number = {{20}}, Month = {{OCT 22}}, Abstract = {{Shapiro time delay is one of the fundamental tests of general relativity and post-Newtonian theories of gravity. Consequently, its measurements can be used to probe the parameter gamma which is related to spacetime curvature produced by a unit mass in the post-Newtonian formalism of gravity. To date all measurements of time delay have been conducted on astronomical scales. It was asserted in 2010 that gravitational wave detectors on Earth could be used to measure Shapiro delay on a terrestrial scale via massive rotating systems. Building on that work, we consider how measurements of Shapiro delay can be made using next-generation gravitational wave detectors. We perform an analysis for measuring Shapiro delay with the next-generation gravitational wave detectors Cosmic Explorer and Einstein Telescope to determine how precisely the effect can be measured. Using a rotating mass unit design, we find that Cosmic Explorer and Einstein Telescope can measure the Shapiro delay signal with amplitude signal to noise ratios upwards of similar to 28 and similar to 43 in 1 year of integration time, respectively. By measuring Shapiro delay with this technique, next-generation interferometers will allow for terrestrial measurements of gamma in the paramaterized post-Newtonian formalism of gravity with sub-percent precision.}}, DOI = {{10.1088/1361-6382/abb260}}, Article-Number = {{205005}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ORCID-Numbers = {{Veske, Doga/0000-0003-4225-0895 Sullivan, Andrew/0000-0002-9545-7286}}, Unique-ID = {{ISI:000574337700001}}, } @article{ ISI:000579342400003, Author = {Ng, Ken K. Y. and Isi, Maximiliano and Haster, Carl-Johan and Vitale, Salvatore}, Title = {{Multiband gravitational-wave searches for ultralight bosons}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{8}}, Month = {{OCT 19}}, Abstract = {{Gravitational waves may be one of the few direct observables produced by ultralight bosons, conjectured dark matter candidates that could be the key to several problems in particle theory, high-energy physics and cosmology. These axionlike particles could spontaneously form ``clouds{''} around astrophysical black holes, leading to potent emission of continuous gravitational waves that could be detected by instruments on the ground and in space. Although this scenario has been thoroughly studied, it has not been yet appreciated that both types of detector may be used in tandem (a practice known as ``multibanding{''}). In this paper, we show that future gravitational-wave detectors on the ground and in space will be able to work together to detect ultralight bosons with masses 25 less than or similar to mu= (10(-15) eV) less than or similar to 500. In detecting binary-black-hole inspirals, the LISA space mission will provide crucial information enabling future ground-based detectors, like Cosmic Explorer or Einstein Telescope, to search for signals from boson clouds around the individual black holes in the observed binaries. We lay out the detection strategy and, focusing on scalar bosons, chart the suitable parameter space. We study the impact of ignorance about the system's history, including cloud age and black hole spin. We also consider the tidal resonances that may destroy the boson cloud before its gravitational signal becomes detectable by a ground-based follow-up. Finally, we show how to take all of these factors into account, together with uncertainties in the LISA measurement, to obtain boson mass constraints from the ground-based observation facilitated by LISA.}}, DOI = {{10.1103/PhysRevD.102.083020}}, Article-Number = {{083020}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Vitale, Salvatore/0000-0003-2700-0767 Isi Banales, Maximiliano/0000-0001-8830-8672 Ng, Ken K. Y./0000-0003-3896-2259}}, Unique-ID = {{ISI:000579342400003}}, } @article{ ISI:000576167700001, Author = {Calderon Bustillo, Juan and Evans, Christopher and Clark, James A. and Kim, Grace and Laguna, Pablo and Shoemaker, Deirdre}, Title = {{Post-merger chirps from binary black holes as probes of the final black-hole horizon}}, Journal = {{COMMUNICATIONS PHYSICS}}, Year = {{2020}}, Volume = {{3}}, Number = {{1}}, Month = {{OCT 8}}, Abstract = {{The formation of a massive black hole (BH) by coalescence of two BHs is a fascinating cosmological event that leaves a gravitational signal that, if detected, can probe extreme gravity and the BH horizon. The authors report non-trivial features of gravitational wave signals from non-equal mass binaries that could be observed by gravitational wave detectors in the coming years, and describe their connection to the evolving shape of the new-born BH. The merger of a binary black hole gives birth to a highly distorted final black hole. The gravitational radiation emitted as this black hole relaxes presents us with the unique opportunity to probe extreme gravity and its connection with the dynamics of the black hole horizon. Using numerical relativity simulations, we demonstrate a connection between a concrete observable feature in the gravitational waves and geometrical features on the dynamical apparent horizon of the final black hole. Specifically, we show how the line-of-sight passage of a ``cusp{''}-like defect on the horizon of the final black hole correlates with ``chirp{''}-like frequency peaks in the post-merger gravitational-waves. These post-merger chirps should be observed and analyzed as the sensitivity of LIGO and Virgo increase and as future generation detectors, such as LISA and the Einstein Telescope, become operational.}}, DOI = {{10.1038/s42005-020-00446-7}}, Article-Number = {{176}}, ISSN = {{2399-3650}}, Unique-ID = {{ISI:000576167700001}}, } @article{ ISI:000575033700002, Author = {Pacilio, Costantino and Vaglio, Massimo and Maselli, Andrea and Pani, Paolo}, Title = {{Gravitational-wave detectors as particle-physics laboratories: Constraining scalar interactions with a coherent inspiral model of boson-star binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{8}}, Month = {{OCT 5}}, Abstract = {{Gravitational-wave (GW) detections of binary neutron star coalescences play a crucial role to constrain the microscopic interaction of matter at ultrahigh density. Similarly, if boson stars exist in the universe, their coalescence can be used to constrain the fundamental coupling constants of a scalar field theory. We develop the first coherent waveform model for the inspiral of boson stars with quartic interactions. The waveform includes coherently spin-induced quadrupolar and tidal-deformability contributions in terms of the masses and spins of the binary and of a single coupling constant of the theory. We show that future instruments, such as the Einstein Telescope and the Laser Interferometer Space Antenna, can provide strong complementary bounds on bosonic self-interactions while the constraining power of current detectors is marginal.}}, DOI = {{10.1103/PhysRevD.102.083002}}, Article-Number = {{083002}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Pani, Paolo/G-7412-2012}}, ORCID-Numbers = {{Pacilio, Costantino/0000-0002-8140-4992 Maselli, Andrea/0000-0001-8515-8525 Pani, Paolo/0000-0003-4443-1761}}, Unique-ID = {{ISI:000575033700002}}, } @article{ ISI:000604458900036, Author = {Andric, Tomislav and Harms, Jan}, Title = {{Simulations of Gravitoelastic Correlations for the Sardinian Candidate Site of the Einstein Telescope}}, Journal = {{JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH}}, Year = {{2020}}, Volume = {{125}}, Number = {{10}}, Month = {{OCT}}, Abstract = {{Gravity fluctuations produced by ambient seismic fields are predicted to limit the sensitivity of the next generation, gravitational wave detector Einstein Telescope at frequencies below 20Hz. The detector will be hosted in an underground infrastructure to reduce seismic disturbances and associated gravity fluctuations. Additional mitigation might be required by monitoring the seismic field and using the data to estimate the associated gravity fluctuations and to subtract the estimate from the detector data, a technique called coherent noise cancelation. In this paper, we present a calculation of correlations between surface displacement of a seismic field and the associated gravitational fluctuations using the spectral element SPECFEM3D Cartesian software. The model takes into account the local topography at a candidate site of the Einstein Telescope at Sardinia. This paper is a first demonstration of SPECFEM3D's capabilities to provide estimates of gravitoelastic correlations, which are required for an optimized deployment of seismometers for gravity noise cancelation.}}, DOI = {{10.1029/2020JB020401}}, Article-Number = {{e2020JB020401}}, ISSN = {{2169-9313}}, EISSN = {{2169-9356}}, ResearcherID-Numbers = {{Harms, Jan/J-4359-2012}}, ORCID-Numbers = {{Harms, Jan/0000-0002-7332-9806}}, Unique-ID = {{ISI:000604458900036}}, } @article{ ISI:000590148200047, Author = {Scelfo, Giulio and Boco, Lumen and Lapi, Andrea and Viel, Matteo}, Title = {{Exploring galaxies-gravitational waves cross-correlations as an astrophysical probe}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{10}}, Month = {{OCT}}, Abstract = {{Gravitational waves astronomy has opened a new opportunity to study the Universe. Full exploitation of this window can especially be provided by combining data coming from gravitational waves experiments with luminous tracers of the Large Scale Structure, like galaxies. In this work we investigate the cross-correlation signal between gravitational waves resolved events, as detected by the Einstein Telescope, and actively star-forming galaxies. The galaxies distribution is computed through their UV and IR luminosity functions and the gravitational waves events, assumed to be of stellar origin, are self-consistently computed from the aforementioned galaxies distribution. We provide a state-of-the-art treatment both on the astrophysical side, taking into account the impact of the star formation and chemical evolution histories of galaxies, and in computing the cross-correlation signal, for which we include lensing and relativistic effects. We find that the measured cross-correlation signal can be sufficiently strong to overcome the noise and provide a clear signal. As a possible application of this methodology, we consider a proof-of-concept case in which we aim at discriminating a metallicity dependence on the compact objects merger efficiency against a reference case with no metallicity dependence. When considering galaxies with a Star Formation Rate psi > 10 M-circle dot/yr, a Signal-to-Noise ratio around a value of 2-4 is gained after a decade of observation time, depending on the observed fraction of the sky. This formalism can be exploited as an astrophysical probe and could potentially allow to test and compare different astrophysical scenarios.}}, DOI = {{10.1088/1475-7516/2020/10/045}}, Article-Number = {{045}}, ISSN = {{1475-7516}}, Unique-ID = {{ISI:000590148200047}}, } @article{ ISI:000576319700001, Author = {Vartanyan, David and Burrows, Adam}, Title = {{Gravitational Waves from Neutrino Emission Asymmetries in Core-collapse Supernovae}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{901}}, Number = {{2}}, Month = {{OCT}}, Abstract = {{We present a broadband spectrum of gravitational waves (GWs) from core-collapse supernovae (CCSNe) sourced by neutrino emission asymmetries for a series of full 3D simulations. The associated GW strain probes the long-term secular evolution of CCSNe and small-scale turbulent activity and provides insight into the geometry of the explosion. For nonexploding models, both the neutrino luminosity and the neutrino gravitational waveform will encode information about the spiral SASI. The neutrino memory will be detectable for a wide range of progenitor masses for a galactic event. Our results can be used to guide near-future decihertz and long-baseline GW detection programs, including aLIGO, the Einstein Telescope, and DECIGO.}}, DOI = {{10.3847/1538-4357/abafac}}, Article-Number = {{108}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Vartanyan, David/ABB-2901-2020 }}, ORCID-Numbers = {{Vartanyan, David/0000-0003-1938-9282}}, Unique-ID = {{ISI:000576319700001}}, } @article{ ISI:000576189800002, Author = {Fu, Xiangyun and Yang, Jianfei and Chen, Zhaoxia and Zhou, Lu and Chen, Jun}, Title = {{Exploring the potentiality of standard sirens to probe cosmic opacity at high redshifts}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2020}}, Volume = {{80}}, Number = {{9}}, Month = {{SEP 26}}, Abstract = {{In this work, using the Gaussian process, we explore the potentiality of future gravitational wave (GW) measurements to probe cosmic opacity at high redshifts through comparing its opacity-free luminosity distance (LD) with the opacity-dependent one from the combination of Type Ia supernovae (SNIa) and gamma-ray bursts (GRBs). The GW data, SNIa and GRB data are simulated from the measurements of the future Einstein Telescope, the actual Pantheon compilation and the latest observation of GRBs compiled by Amati et al, respectively. A nonparametric method is proposed to probe the spatial homogeneity of cosmic transparency at high redshift by comparing the LD reconstructed from the GW data with that reconstructed from the Pantheon and GRB data. In addition, the cosmic opacity is tested by using the parametrization for the optical depth, and the results show that the constraints on cosmic opacity are more stringent than the previous ones. It shows that the future GW measurements may be used as an important tool to probe the cosmic opacity in the high redshift region.}}, DOI = {{10.1140/epjc/s10052-020-08479-6}}, Article-Number = {{893}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, Unique-ID = {{ISI:000576189800002}}, } @article{ ISI:000571687700002, Author = {Ascenzi, S. and Oganesyan, G. and Salafia, O. S. and Branchesi, M. and Ghirlanda, G. and Dall'Osso, S.}, Title = {{High-latitude emission from the structured jet of gamma-ray bursts observed off-axis}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2020}}, Volume = {{641}}, Month = {{SEP 9}}, Abstract = {{The X-ray emission of gamma-ray burst (GRBs) is often characterized by an initial steep decay followed by a nearly constant emission phase (so-called ``plateau{''}) which can extend up to thousands of seconds. While the steep decay is usually interpreted as the tail of the prompt gamma-ray flash, the long-lasting plateau is commonly associated to the emission from the external shock sustained by energy injection from a long-lasting central engine. A recent study proposed an alternative interpretation, ascribing both the steep decay and the plateau to high-latitude emission (HLE) from a ``structured jet{''} whose energy and bulk Lorentz factor depend on the angular distance from the jet symmetry axis. In this work we expand on this idea and explore more realistic conditions: (a) the finite duration of the prompt emission, (b) the angular dependence of the optical depth, and (c) the dependence of the light curve on the observer viewing angle. We find that, when viewed highly off-axis, the structured jet HLE light curve is smoothly decaying with no clear distinction between the steep and flat phases, as opposed to the on-axis case. For a realistic choice of physical parameters, the effects of a latitude-dependent Thomson opacity and finite duration of the emission have a marginal effect on the overall light-curve evolution. We discuss the possible HLE of GW170817, showing that the emission would have faded away long before the first Swift-XRT observations. Finally, we discuss the prospects for the detection of HLE from off-axis GRBs by present and future wide-field X-ray telescopes and X-ray surveys, such as eROSITA and the mission concept THESEUS.}}, DOI = {{10.1051/0004-6361/202038265}}, Article-Number = {{A61}}, ISSN = {{0004-6361}}, EISSN = {{1432-0746}}, ORCID-Numbers = {{Ascenzi, Stefano/0000-0001-5116-6789}}, Unique-ID = {{ISI:000571687700002}}, } @article{ ISI:000567277400005, Author = {Sharma, Ashish and Harms, Jan}, Title = {{Searching for cosmological gravitational-wave backgrounds with third-generation detectors in the presence of an astrophysical foreground}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{6}}, Month = {{SEP 9}}, Abstract = {{The stochastic cosmological gravitational-wave background (CGWB) provides a direct window to study early universe phenomena and fundamental physics. With the proposed third-generation ground-based gravitational wave detectors, Einstein Telescope (ET) and Cosmic Explorer (CE), we might be able to detect evidence of a CGWB. However, to dig out these prime signals would be a difficult quest as the dominance of the astrophysical foreground from compact-binary coalescence (CBC) will mask this CGWB. In this paper, we study a subtraction-noise projection method, making it possible to reduce the residuals left after subtraction of the astrophysical foreground of CBCs, greatly improving our chances to detect a cosmological background. We carried out our analysis based on simulations of ET and CE and using posterior sampling for the parameter estimation of binary black-hole mergers. We demonstrate the sensitivity improvement of stochastic gravitational-wave searches and conclude that the ultimate sensitivity of these searches will not be limited by residuals left when subtracting the estimated BBH foreground, but by the fraction of the astrophysical foreground that cannot be detected even with third-generation instruments, or possibly by other signals not included in our analysis. We also resolve previous misconceptions of residual noise in the context of Gaussian parameter estimation.}}, DOI = {{10.1103/PhysRevD.102.063009}}, Article-Number = {{063009}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Sharma, Ashish/0000-0003-4982-6156}}, Unique-ID = {{ISI:000567277400005}}, } @article{ ISI:000574919600016, Author = {Yu, Hai and Zhang, Pengjie and Wang, Fa-Yin}, Title = {{Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{497}}, Number = {{1}}, Pages = {{204-209}}, Month = {{SEP}}, Abstract = {{Standard siren cosmology of gravitational wave (GW) merger events relies on the identification of host galaxies and their redshifts. But this can be highly challenging due to numerous candidates of galaxies in the GW localization area. We point out that the number of candidates can be reduced by orders of magnitude for strongly lensed GW events, due to extra observational constraints. For the next-generation GW detectors like Einstein Telescope (ET), we estimate that this number is usually significantly less than one, as long as the GW localization uncertainty is better than similar to 10 deg(2). This implies that the unique identification of the host galaxy of lensed GW event detected by ET and Cosmic Explorer (CE) is possible. This provides us a promising opportunity to measure the redshift of the GW event and facilitate the standard siren cosmology. We also discuss its potential applications in understanding the evolution process and environment of the GW event.}}, DOI = {{10.1093/mnras/staa1952}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Wang, Fayin/B-1479-2009}}, ORCID-Numbers = {{Wang, Fayin/0000-0003-4157-7714}}, Unique-ID = {{ISI:000574919600016}}, } @article{ ISI:000574919600063, Author = {Yang, Weiqiang and Pan, Supriya and Mota, David F. and Du, Minghui}, Title = {{Forecast constraints on anisotropic stress in dark energy using gravitational waves}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{497}}, Number = {{1}}, Pages = {{879-893}}, Month = {{SEP}}, Abstract = {{It is always interesting to investigate how well can a future experiment perform with respect to others (present or future ones). Cosmology is really an exciting field where a lot of puzzles are still unknown. In this paper, we consider a generalized dark energy (DE) scenario where anisotropic stress is present. We constrain this generalized cosmic scenario with an aim to investigate how gravitational waves standard sirens (GWSS) may constrain the anisotropic stress, which, according to the standard cosmological probes, remains unconstrained. In order to do this, we generate the luminosity distance measurements from O(10(3)) mock GW events that match the expected sensitivity of the Einstein Telescope. Our analyses report that, first of all, GWSS can give better constraints on various cosmological parameters compared to the usual cosmological probes, but the viscous sound speed appearing due to the DE anisotropic stress is totally unconstrained even after the inclusion of GWSS.}}, DOI = {{10.1093/mnras/staa1859}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, Unique-ID = {{ISI:000574919600063}}, } @article{ ISI:000571575600001, Author = {Amann, Florian and Bonsignorio, Fabio and Bulik, Tomasz and Bulten, Henk Jan and Cuccuru, Stefano and Dassargues, Alain and DeSalvo, Riccardo and Fenyvesi, Edit and Fidecaro, Francesco and Fiori, Irene and Giunchi, Carlo and Grado, Aniello and Harms, Jan and Koley, Soumen and Kovacs, Laszlo and Losurdo, Giovanni and Mandic, Vuk and Meyers, Patrick and Naticchioni, Luca and Nguyen, Frederic and Oggiano, Giacomo and Olivieri, Marco and Paoletti, Federico and Paoli, Andrea and Plastino, Wolfango and Razzano, Massimiliano and Ruggi, Paolo and Saccorotti, Gilberto and Sintes, Alicia M. and Somlai, Laszlo and Van, Peter and Vasuth, Matyas}, Title = {{Site-selection criteria for the Einstein Telescope}}, Journal = {{REVIEW OF SCIENTIFIC INSTRUMENTS}}, Year = {{2020}}, Volume = {{91}}, Number = {{9}}, Month = {{SEP 1}}, Abstract = {{The Einstein Telescope (ET) is a proposed next-generation, underground gravitational-wave detector to be based in Europe. It will provide about an order of magnitude sensitivity increase with respect to the currently operating detectors and, also extend the observation band targeting frequencies as low as 3 Hz. One of the first decisions that needs to be made is about the future ET site following an in-depth site characterization. Site evaluation and selection is a complicated process, which takes into account science, financial, political, and socio-economic criteria. In this paper, we provide an overview of the site-selection criteria for ET, provide a formalism to evaluate the direct impact of environmental noise on ET sensitivity, and outline the necessary elements of a site-characterization campaign.}}, DOI = {{10.1063/5.0018414}}, Article-Number = {{094504}}, ISSN = {{0034-6748}}, EISSN = {{1089-7623}}, ResearcherID-Numbers = {{Bonsignorio, Fabio/R-7078-2019 Van, Peter/F-8579-2010 Giunchi, Carlo/H-8508-2012 Harms, Jan/J-4359-2012}}, ORCID-Numbers = {{Bonsignorio, Fabio/0000-0002-5802-2814 Van, Peter/0000-0002-9396-4073 Giunchi, Carlo/0000-0002-0174-324X RAZZANO, MASSIMILIANO/0000-0003-4825-1629 Bulik, Tomasz/0000-0003-2045-4803 DeSalvo, Riccardo/0000-0002-4818-0296 Harms, Jan/0000-0002-7332-9806}}, Unique-ID = {{ISI:000571575600001}}, } @article{ ISI:000562631300002, Author = {Chen, Wen-Cong}, Title = {{Constraining the ellipticity of millisecond pulsars with observed spin-down rates}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{4}}, Month = {{AUG 26}}, Abstract = {{A spinning neutron star (NS) that is asymmetric with respect to its spin axis can emit continuous gravitational wave (GW) signals. The spin frequencies and their distribution of radio millisecond pulsars (MSPs) and accreting MSPs provide some evidences of GW radiation, and MSPs are ideal probes detecting high frequency GW signals. It is generally thought that MSPs originate from the recycled process, in which the NS accretes the material and angular momentum from the donor star. The accreted matter would be confined at the polar cap zone by an equatorial belt of compressed magnetic field fixed in the deep crust of the NS, and yields ``magnetic mountain.{''} Based on an assumption that the spin-down rates of three transitional MSPs including PSR J1023 + 0038 are the combinational contribution of the accretion torque, the propeller torque, and the GW radiation torque, in this work we attempt to constrain the ellipticities of MSPs with observed spin-down rates. Assuming some canonical parameters of NSs, the ellipticities of three transitional MSPs and ten redbacks are estimated to be epsilon = (0.9 - 23.4) x 10(-9). The electrical resistivities of three transitional MSPs are also derived to be in the range eta = (1.2 - 15.3) x 10(-31) s, which display an ideal power law relation with the accretion rate. The characteristic strains (h(c) = (0.6 - 2.5) x 10(-27)) of GW signals emitting by these sources are obviously beyond the sensitivity scope of the aLIGO. We expect that the third-generation GW detectors like the Einstein Telescope can seize the GW signals from these sources in the future.}}, DOI = {{10.1103/PhysRevD.102.043020}}, Article-Number = {{043020}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Chen, Wen-Cong/0000-0002-0785-5349}}, Unique-ID = {{ISI:000562631300002}}, } @article{ ISI:000590146600023, Author = {Chen, Zu-Cheng and Huang, Qing-Guo}, Title = {{Distinguishing primordial black holes from astrophysical black holes by Einstein Telescope and Cosmic Explorer}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{8}}, Month = {{AUG}}, Abstract = {{We investigate how the next generation gravitational-wave (GW) detectors, such as Einstein Telescope (ET) and Cosmic Explorer (CE), can be used to distinguish primordial black holes (PBHs) from astrophysical black holes (ABHs). Since a direct detection of subsolar mass black holes can be taken as the smoking gun for PBHs, we estimate the detectable limits of the abundance of sub-solar mass PBHs in cold dark matter by the targeted search for sub-solar mass PBH binaries and binaries containing a sub-solar mass PBH and a super-solar mass PBH, respectively. On the other hand, according to the different redshift evolutions of the merger rate for PBH binaries and ABH binaries, we forecast the detectable event rate distributions for the PBH binaries and ABH binaries by ET and CE respectively, which can serve as a method to distinguish super-solar mass PBHs from ABHs.}}, DOI = {{10.1088/1475-7516/2020/08/039}}, Article-Number = {{039}}, ISSN = {{1475-7516}}, Unique-ID = {{ISI:000590146600023}}, } @article{ ISI:000565732800001, Author = {Rasskazov, Alexander and Fragione, Giacomo and Kocsis, Bence}, Title = {{Binary Intermediate-mass Black Hole Mergers in Globular Clusters}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{899}}, Number = {{2}}, Month = {{AUG}}, Abstract = {{We consider the formation of binary intermediate black holes (BIMBHs) in globular clusters (GC), which could happen either in situ or due to the mergers between clusters. We simulate the evolution of the BIMBH orbit (and its subsequent merger) due to stellar ejections. We also take into account the evaporation of GCs due to the tidal field of the host galaxy and two-body relaxation. Our results show that if at least 10(-3)of all GCs become BIMBH hosts and the BIMBH masses are similar to 1\% of the GC mass, at least one of the inspiraling (or merging) BIMBHs will be detected by LISA during its 4 yr mission lifetime. Most of the detected BIMBHs come (1) from heavy GCs (greater than or similar to 3 x 10(5) M-circle dot), as lower-mass GCs end up being disrupted before their BIMBHs have time to merge, and (2) from redshifts 1 z < 3, assuming that most GCs form aroundz similar to 4 and given that the merger timescale for most BIMBHs is similar to 1 Gyr. If the BIMBH to GC mass ratio is lower (similar to 10(-3)) but the fraction of BIMBH hosts among GCs is higher (greater than or similar to 10(-2)), some of their mergers will also be detected by LIGO, Virgo, and KAGRA and the proposed Einstein Telescope.}}, DOI = {{10.3847/1538-4357/aba2f4}}, Article-Number = {{149}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Kocsis, Bence/C-3061-2013 Fragione, Giacomo/ABC-2055-2020}}, ORCID-Numbers = {{Kocsis, Bence/0000-0002-4865-7517 }}, Unique-ID = {{ISI:000565732800001}}, } @article{ ISI:000561549500001, Author = {Liu, Tonghua and Cao, Shuo and Biesiada, Marek and Liu, Yuting and Geng, Shuaibo and Lian, Yujie}, Title = {{Testing the Cosmic Opacity at Higher Redshifts: Implication from Quasars with Available UV and X-Ray Observations}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{899}}, Number = {{1}}, Month = {{AUG}}, Abstract = {{In this paper, we present a cosmological model-independent test for the cosmic opacity at high redshifts (z similar to 5). We achieve this with the opacity-dependent luminosity distances derived from the nonlinear relation between X-ray and UV emissions of quasars, combined with two types of opacity-independent luminosity distances derived from the Hubble parameter measurements and simulated gravitational wave (GW) events achievable with the Einstein Telescope (ET). In the framework of two phenomenological parameterizations adopted to describe cosmic opacity at high redshifts, our main results show that a transparent universe is supported by the current observational data at a 2 sigma confidence level. However, the derived value of the cosmic opacity is slightly sensitive to the parameterization of tau(z), which highlights the importance of choosing a reliable parameterization to describe the optical depth tau(z) in the early universe. Compared with previous works, the combination of the quasar data and theH(z)/GW observations in similar redshift ranges provides a novel way to confirm a transparent universe (epsilon = 0 at higher redshiftsz similar to 5), with an accuracy of Delta epsilon similar to 10(-2). More importantly, our findings indicate that a strong degeneracy between the cosmic-opacity parameter and the parameters characterizing theL(UV) - L(X)relation of quasars, which reinforces the necessity of proper calibration for this new type of high-redshift standard candle (in a cosmological model-independent way).}}, DOI = {{10.3847/1538-4357/aba0b6}}, Article-Number = {{71}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Cao, Shuo/0000-0002-8870-981X}}, Unique-ID = {{ISI:000561549500001}}, } @article{ ISI:000557219400001, Author = {Braglia, Matteo and Hazra, Dhiraj Kumar and Finelli, Fabio and Smoot, George F. and Sriramkumar, L. and Starobinsky, Alexei A.}, Title = {{Generating PBHs and small-scale GWs in two-field models of inflation}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{8}}, Month = {{AUG}}, Abstract = {{Primordial black holes (PBHs) generated by gravitational collapse of large primordial overdensities can be a fraction of the observed dark matter. In this paper, we introduce a mechanism to produce a large peak in the primordial power spectrum (PPS) in two-field inflationary models characterized by two stages of inflation based on a large non-canonical kinetic coupling. This mechanism is generic to several two-field inflationary models, due to a temporary tachyonic instability of the isocurvature perturbations at the transition between the two stages of inflation. We numerically compute the primordial perturbations from largest scales to the small scales corresponding to that of PBHs using an extension of BINGO (BI-spectra and Non-Gaussianity Operator). Moreover we numerically compute the stochastic background of gravitational waves (SBGW) produced by second order scalar perturbations within frequencies ranging from nano-Hz to KHz that covers the observational scales corresponding to Pulsar Timing Arrays, Square Kilometer Array to that of Einstein telescope. We discuss the prospect of its detection by these proposed and upcoming gravitational waves experiments.}}, DOI = {{10.1088/1475-7516/2020/08/001}}, Article-Number = {{001}}, ISSN = {{1475-7516}}, Unique-ID = {{ISI:000557219400001}}, } @article{ ISI:000551342300003, Author = {Nunes, Rafael C.}, Title = {{Searching for modified gravity in the astrophysical gravitational wave background: Application to ground-based interferometers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{2}}, Month = {{JUL 23}}, Abstract = {{We investigate how the propagation of an astrophysical gravitational wave background (AGWB) is modified over cosmological volumes when considering theories beyond general relativity of the type Horndeski gravity. We first deduce an amplitude correction on the AGWB induced for the presence of a possible running in the Planck mass. Then, we apply the spectral noise density from some ground-based interferometers, namely, the Advanced LIGO (aLIGO), Einstein Telescope (ET) and Cosmic Explore (CE), to evaluate the signal-to-noise ratio as a function of the amplitude of the running of the Planck mass for two different scenarios. We find that for observation time period greater than or similar to 5 yrs and greater than or similar to 1 yr, we can have a significant signal of the AGWB in the band {[}1-100] Hz from the ET and CE sensitivity, respectively. Finally, using Fisher information, we find some forecast bounds, and we deduce less than or similar to 27\% and less than or similar to 18\% correction at 1 sigma confidence level on the amplitude of the running of the Planck mass from ET and CE, respectively. It is clear that a detection of a AGWB in the future can open a new window to probe the nature of gravity with good accuracy.}}, DOI = {{10.1103/PhysRevD.102.024071}}, Article-Number = {{024071}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000551342300003}}, } @article{ ISI:000550997900002, Author = {Grimm, Stefan and Harms, Jan}, Title = {{Multiband gravitational-wave parameter estimation: A study of future detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{2}}, Month = {{JUL 22}}, Abstract = {{The first detection of a gravitational-wave signal of a coalescence of two black holes marked the beginning of the era of gravitational-wave astronomy, which opens exciting new possibilities in the fields of astronomy, astrophysics, and cosmology. The currently operating detectors of the LIGO and Virgo Collaborations are sensitive at relatively high frequencies, from 10 Hz up to about a kHz, and are able to detect gravitational waves emitted in a short time frame of less than a second (binary black holes) to minutes (binary neutron stars). Future missions like Laser Interferometer Space Antenna (LISA) will be sensitive in lower frequency ranges, which will make it possible to detect gravitational waves emitted long before these binaries merge. In this paper, we investigate the possibilities for parameter estimation using the Fisher-matrix formalism with combined information from present and future detectors in different frequency bands. The detectors we consider are the LIGO/Virgo detectors, the Einstein Telescope, LISA, and the first stage of the Deci-Hertz Interferometer Gravitational wave Observatory (B-DECIGO). The underlying models are constructed in time domain, which allows us to accurately model long-duration signal observations with multiband (or broadband) detector networks on parameter estimation. We assess the benefit of combining information from ground-based and space-borne detectors, and how choices of the orbit of B-DECIGO influence parameter estimates.}}, DOI = {{10.1103/PhysRevD.102.022007}}, Article-Number = {{022007}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Harms, Jan/J-4359-2012}}, ORCID-Numbers = {{Harms, Jan/0000-0002-7332-9806}}, Unique-ID = {{ISI:000550997900002}}, } @article{ ISI:000548741400008, Author = {Sachdev, Surabhi and Regimbau, Tania and Sathyaprakash, B. S.}, Title = {{Subtracting compact binary foreground sources to reveal primordial gravitational-wave backgrounds}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{2}}, Month = {{JUL 16}}, Abstract = {{Detection of primordial gravitational-wave backgrounds generated during the early Universe phase transitions is a key science goal for future ground-based detectors. The rate of compact binary mergers is so large that their cosmological population produces a confusion background that could masquerade the detection of potential primordial stochastic backgrounds. In this paper, we study the ability of current and future detectors to resolve the confusion background to reveal interesting primordial backgrounds. The current detector network of LIGO and Virgo and the upcoming KAGRA and LIGO-India will not be able to resolve the cosmological compact binary source population, and its sensitivity to stochastic background will be limited by the confusion background of these sources. We find that a network of three (and five) third generation (3G) detectors of Cosmic Explorer and Einstein Telescope will resolve the confusion background produced by binary black holes leaving only about 1.3\% (respectively, 0.075\%) unresolved; in contrast, as many as 25\% (respectively, 7.7\%) of binary neutron star sources remain unresolved. Consequently, the binary black hole population will likely not limit observation of primordial backgrounds, but the binary neutron star population will limit the sensitivity of 3G detectors to Omega(GW) similar to 10(-11) at 10 Hz (respectively, Omega(GW) similar to 3 x 10(-12)).}}, DOI = {{10.1103/PhysRevD.102.024051}}, Article-Number = {{024051}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014 }}, ORCID-Numbers = {{Sathyaprakash, Bangalore/0000-0003-3845-7586 Sachdev, Surabhi/0000-0002-0525-2317}}, Unique-ID = {{ISI:000548741400008}}, } @article{ ISI:000546758500001, Author = {Lin, Hai-Nan and Li, Xin}, Title = {{A new method to test the cosmic distance duality relation using the strongly lensed gravitational waves{*}}}, Journal = {{CHINESE PHYSICS C}}, Year = {{2020}}, Volume = {{44}}, Number = {{7}}, Month = {{JUL}}, Abstract = {{We propose a new method to test the cosmic distance duality relation using the strongly lensed gravitational waves. The simultaneous observation of the image positions, relative time delay between different images, redshift measurements of the lens and the source, together with the mass modelling of the lens galaxy, provide the angular diameter distance to the gravitational wave source. On the other hand, the luminosity distance to the source can be obtained from the observation of the gravitational wave signals. To our knowledge this is the first time a method is proposed to simultaneously measure the angular diameter distance and the luminosity distance from the same source. Hence, the strongly lensed gravitational waves provide a unique method to test the cosmic distance duality relation. With the construction of the third generation gravitational detectors such as the Einstein Telescope, it will be possible to test the cosmic distance duality relation with an accuracy of a few percent.}}, DOI = {{10.1088/1674-1137/44/7/075101}}, Article-Number = {{075101}}, ISSN = {{1674-1137}}, EISSN = {{2058-6132}}, ORCID-Numbers = {{Lin, Hai-Nan/0000-0003-1659-3368}}, Unique-ID = {{ISI:000546758500001}}, } @article{ ISI:000546679500019, Author = {Pang, Peter T. H. and Hannuksela, Otto A. and Dietrich, Tim and Pagano, Giulia and Harry, Ian W.}, Title = {{Lensed or not lensed: determining lensing magnifications for binary neutron star mergers from a single detection}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{495}}, Number = {{4}}, Pages = {{3740-3750}}, Month = {{JUL}}, Abstract = {{Advanced LIGO and Advanced Virgo could observe the first lensed gravitational wave sources in the coming years, while the future Einstein Telescope could observe hundreds of lensed events. It is, therefore, crucial to develop methodologies to distinguish between lensed from unlensed gravitational-wave observations. A lensed signal not identified as such will lead to biases during the interpretation of the source. In particular, sources will appear to have intrinsically higher masses. No robust method currently exists to distinguish between the magnification bias caused by lensing and intrinsically high-mass sources. In this work, we show how to recognize lensed and unlensed binary neutron star systems through the measurement of their tidal effects for highly magnified sources as a proof-of-principle. The proposed method could be used to identify lensed binary neutron stars that are the chief candidate for lensing cosmography studies. We apply our method on GW190425, finding no evidence in favour of lensing, mainly due to the poor measurement of the event's tidal effects. However, we expect that future detections with better tidal measurements can yield better constraints.}}, DOI = {{10.1093/mnras/staa1430}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Pang, Peter Tsun Ho/0000-0001-7041-3239 Hannuksela, Otto Akseli/0000-0002-3887-7137 Harry, Ian/0000-0002-5304-9372}}, Unique-ID = {{ISI:000546679500019}}, } @article{ ISI:000544521600007, Author = {Dror, Jeff A. and Laha, Ranjan and Opferkuch, Toby}, Title = {{Probing muonic forces with neutron star binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{102}}, Number = {{2}}, Month = {{JUL 1}}, Abstract = {{We show that gravitational wave emission from neutron star binaries can be used to discover any generic long-ranged muonic force due to the large inevitable abundance of muons inside neutron stars. As a minimal consistent example, we focus on a gauged U(1) L-mu-L-tau symmetry. In pulsar binaries, such U(1) L-mu-L-tau vectors induce an anomalously fast decay of the orbital period through the emission of dipole radiation. We study a range of different pulsar binaries, finding the most powerful constraints for vector masses below O(10(-18) eV). For merging binaries, the presence of muons in neutron stars can result in dipole radiation as well as a modification of the chirp mass during the inspiral phase. We make projections for a prospective search using both the GW170817 and S190814bv events and find that current data can discover light vectors with masses below O(10(-10) eV). In both cases, the limits attainable with neutron stars reach gauge coupling g' less than or similar to 10(-20), which are many orders of magnitude stronger than previous constraints. We also show projections for next generation experiments, such as Einstein Telescope and Cosmic Explorer.}}, DOI = {{10.1103/PhysRevD.102.023005}}, Article-Number = {{023005}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Laha, Ranjan/0000-0001-7104-5730}}, Unique-ID = {{ISI:000544521600007}}, } @article{ ISI:000542920500003, Author = {Zhang, Teng and Martynov, Denis and Freise, Andreas and Miao, Haixing}, Title = {{Quantum squeezing schemes for heterodyne readout}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{12}}, Month = {{JUN 25}}, Abstract = {{Advanced gravitational-wave detectors are limited by quantum noise in their most sensitive frequency band. Quantum noise suppression techniques, such as the application of the quantum squeezed state of light, have been actively studied in the context of homodyne readouts. In this paper, we consider quantum squeezing schemes for the heterodyne readouts. This is motivated by a successful suppression of the higher-order-mode content by stable recycling cavities in advanced detectors. The heterodyne readout scheme requires precise tuning of the interferometer parameters and a broadband squeezing source, but is conceptually simple and elegant. We further show that it is compatible with the frequency-dependent squeezing, which reduces both the shot noise and the radiation-pressure noise. We propose a test of the heterodyne readout with squeezing in Advanced LIGO. This can serve as a pathfinder not only for the implementation in future detectors, such as the Einstein Telescope and Cosmic Explorer, but also for general high-precision optical measurements.}}, DOI = {{10.1103/PhysRevD.101.124052}}, Article-Number = {{124052}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Zhang, Teng/Y-3281-2018 }}, ORCID-Numbers = {{Zhang, Teng/0000-0001-5278-4220 Freise, Andreas/0000-0001-6586-9901}}, Unique-ID = {{ISI:000542920500003}}, } @article{ ISI:000603596000010, Author = {Calore, Francesca and Cuoco, Alessandro and Regimbau, Tania and Sachdev, Surabhi and Serpico, Pasquale Dario}, Title = {{Cross-correlating galaxy catalogs and gravitational waves: A tomographic approach}}, Journal = {{PHYSICAL REVIEW RESEARCH}}, Year = {{2020}}, Volume = {{2}}, Number = {{2}}, Month = {{JUN 9}}, Abstract = {{Unveiling the origin of the coalescing binaries detected via gravitational waves (GWs) is challenging, notably if no multiwavelength counterpart is detected. One important diagnostic tool is the coalescing binary distribution with respect to the large-scale structures (LSSs) of the Universe, which we quantify via the cross-correlation of galaxy catalogs with GW ones. By using both existing and forthcoming galaxy catalogs and using realistic Monte Carlo simulations of GW events, we find that the cross-correlation signal should be marginally detectable in 10-year data taking of advanced LIGO-Virgo detectors at design sensitivity, at least for binary neutron star mergers. The expected addition of KAGRA and LIGO-India to the GW detector network would allow for a firmer detection of this signal, and, in combination with future cosmological surveys, would also permit the detection of cross-correlation for coalescing black holes. Such a measurement may unveil, for instance, a primordial origin of coalescing black holes. To attain this goal, we find that it is crucial to adopt a tomographic approach and to reach a sufficiently accurate localization of GW events. The depth of forthcoming surveys will be fully exploited by third-generation GW detectors such as the Einstein Telescope or the Cosmic Explorer, which will allow one to perform precision studies of the coalescing black hole LSS distribution and attain rather advanced model discrimination capabilities.}}, DOI = {{10.1103/PhysRevResearch.2.023314}}, Article-Number = {{023314}}, EISSN = {{2643-1564}}, ResearcherID-Numbers = {{Serpico, Pasquale Dario/AAF-7147-2021}}, ORCID-Numbers = {{Serpico, Pasquale Dario/0000-0002-8656-7942}}, Unique-ID = {{ISI:000603596000010}}, } @article{ ISI:000551875400046, Author = {Li, Hai-Li and He, Dong-Ze and Zhang, Jing-Fei and Zhang, Xin}, Title = {{Quantifying the impacts of future gravitational-wave data on constraining interacting dark energy}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{6}}, Month = {{JUN}}, Abstract = {{In this work, we investigate the impacts of the future gravitational-wave (GW) standard siren observation by the Einstein Telescope (ET) on constraining the interacting dark energy (IDE) models. We simulate 1000 GW events in the redshift range of 0 less than or similar to z less than or similar to 5 based on the 10-year observation of the ET. We combine the simulated GW data with the current mainstream cosmological electromagnetic observations including the cosmic microwave background anisotropies, the baryon acoustic oscillations, and the type Ia supernovae to constrain the IDE models. We consider typical IDE models in the context of a perturbed universe. To avoid the large-scale instability problem for IDE models, we apply the extended parameterized post-Friedmann approach to calculate the cosmological perturbations. We find that the addition of the GW standard siren data could significantly improve the constraint accuracies for most of the cosmological parameters (e.g., H-0, w, and Omega(m)). For the coupling parameter beta, the constraint errors could also be slightly improved when adding the GW data in the cosmological fit.}}, DOI = {{10.1088/1475-7516/2020/06/038}}, Article-Number = {{038}}, ISSN = {{1475-7516}}, ORCID-Numbers = {{Zhang, Xin/0000-0002-6029-1933 He, Dong-Ze/0000-0001-5344-9467}}, Unique-ID = {{ISI:000551875400046}}, } @article{ ISI:000543015800033, Author = {Liao, Kai and Tian, Shuxun and Ding, Xuheng}, Title = {{Probing compact dark matter with gravitational wave fringes detected by the Einstein Telescope}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{495}}, Number = {{2}}, Pages = {{2002-2006}}, Month = {{JUN}}, Abstract = {{Unlike the electromagnetic radiation from astrophysical objects, gravitational waves (GWs) from binary star mergers have much longer wavelengths and are coherent. For ground-based GW detectors, when the lens object between the source and the Earth has mass similar to 1-10(5) M-circle dot, the diffraction effect should be considered since the chirping wavelengths are comparable to the scale of the barrier (its Schwarzschild radius). The waveform will thus be distorted as the fringes. In this work, we show that signals from the third-generation GW detectors like the Einstein Telescope (ET) would be a smoking gun for probing the nature of compact dark matter (CDM) or primordial black holes. Detection of the lensing effects becomes harder when the lens mass is smaller. ET is more sensitive than LIGO, the constraint is available for CDM mass >5 M-circle dot while LIGO can only detect the mass >100 M-circle dot. For a null search of the fringes, one-year observation of ET can constrain the CDM density fraction to similar to 10(-2) to 10(-5) in the mass range M-CDM = 10-100 M-circle dot.}}, DOI = {{10.1093/mnras/staa1388}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Tian, Shuxun/0000-0001-8751-5020 Ding, Xuheng/0000-0001-8917-2148}}, Unique-ID = {{ISI:000543015800033}}, } @article{ ISI:000543015800068, Author = {Liu, Boyuan and Bromm, Volker}, Title = {{Gravitational waves from Population III binary black holes formed by dynamical capture}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{495}}, Number = {{2}}, Pages = {{2475-2495}}, Month = {{JUN}}, Abstract = {{We use cosmological hydrodynamic simulations to study the gravitational wave (GW) signals from high-redshift binary black holes (BBHs) formed by dynamical capture (ex situ formation channel). We in particular focus on black holes (BHs) originating from the first generation of massive, metal-poor, so-called Population III (Pop III) stars. An alternative (in situ) formation pathway arises in Pop III binary stars whose GWligi signature has been intensively studied. In our optimistic model, we predict a localGWevent rate density for ex situ BBHs (formed atz> 4) of similar to 0.04 yr(-1) Gpc(-3). This is comparable to or even higher than the conservative predictions of the rate density for in situ BBHs similar to 0.01-0.1 yr(-1) Gpc(-3), indicating that the ex situ formation channel may be as important as the in situ one for producing GW events. We also evaluate the detectability of our simulated GW events for selected planned GW instruments, such as the Einstein Telescope (ET). For instance, we find the all-sky detection rate with signal-to-noise ratios above 10 to be less than or similar to 100 yr(-1) for the xylophone configuration of ET. However, our results are highly sensitive to the subgrid models for BBH identification and evolution, such that the GW event efficiency (rate) is reduced by a factor of 4 (20) in the pessimistic case. The ex situ channel of Pop III BBHs deserves further investigation with better modelling of the environments around Pop III-seeded BHs.}}, DOI = {{10.1093/mnras/staa1362}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, Unique-ID = {{ISI:000543015800068}}, } @article{ ISI:000539097800007, Author = {Powell, Jade and Mueller, Bernhard}, Title = {{Three-dimensional core-collapse supernova simulations of massive and rotating progenitors}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{494}}, Number = {{4}}, Pages = {{4665-4675}}, Month = {{JUN}}, Abstract = {{We present 3D simulations of the core-collapse of massive rotating and non-rotating progenitors performed with the general relativistic neutrino hydrodynamics code COCONUT-FMT. The progenitor models include Wolf-Rayet stars with initial helium star masses of 39 M-circle dot and 20M(circle dot), and an 18M(circle dot) red supergiant. The 39M(circle dot) model is a rapid rotator, whereas the two other progenitors are non-rotating. Both Wolf-Rayet models produce healthy neutrino-driven explosions, whereas the red supergiant model fails to explode. By the end of the simulations, the explosion energies have already reached 1.1 x 10(51) and 0.6 x 10(51) erg for the 39M(circle dot) and 20M(circle dot) model, respectively. They produce neutron stars of relatively high mass, but with modest kicks. Due to the alignment of the bipolar explosion geometry with the rotation axis, there is a relatively small misalignment of 30 degrees between the spin and the kick in the rapidly rotating 39M(circle dot) model. For this model, we find that rotation significantly changes the dependence of the characteristic gravitational-wave frequency of the f-mode on the proto-neutron star parameters compared to the non-rotating case. Its gravitational-wave amplitudes would make it detectable out to almost 2Mpc by the Einstein Telescope. The other two progenitors have considerably smaller detection distances, despite significant low-frequency emission in the most sensitive frequency band of current gravitational-wave detectors.}}, DOI = {{10.1093/mnras/staa1048}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Mueller, Bernhard/0000-0002-4470-1277 Powell, Jade/0000-0002-1357-4164}}, Unique-ID = {{ISI:000539097800007}}, } @article{ ISI:000535454600006, Author = {Gupta, Anuradha and Gerosa, Davide and Arun, K. G. and Berti, Emanuele and Farr, Will M. and Sathyaprakash, B. S.}, Title = {{Black holes in the low-mass gap: Implications for gravitational-wave observations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{10}}, Month = {{MAY 26}}, Abstract = {{Binary neutron-star mergers will predominantly produce black-hole remnants of mass similar to 3-4 M-circle dot, thus populating the putative low-mass gap between neutron stars and stellar-mass black holes. If these low-mass black holes are in dense astrophysical environments, mass segregation could lead to ``second-generation{''} compact binaries merging within a Hubble time. In this paper, we investigate possible signatures of such low-mass compact binary mergers in gravitational-wave observations. We show that this unique population of objects, if present, will be uncovered by the third-generation gravitational-wave detectors, such as Cosmic Explorer and Einstein Telescope. Future joint measurements of chirp mass M and effective spin chi(eff) could clarify the formation scenario of compact objects in the low-mass gap. As a case study, we show that the recent detection of GW190425 (along with GW170817) favors a double Gaussian mass model for neutron stars, under the assumption that the primary in GW190425 is a black hole formed from a previous binary neutron-star merger.}}, DOI = {{10.1103/PhysRevD.101.103036}}, Article-Number = {{103036}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014 Berti, Emanuele/C-9331-2016}}, ORCID-Numbers = {{Gerosa, Davide/0000-0002-0933-3579 Arun, K G/0000-0002-6960-8538 Gupta, Anuradha/0000-0002-5441-9013 Farr, Will/0000-0003-1540-8562 Sathyaprakash, Bangalore/0000-0003-3845-7586 Berti, Emanuele/0000-0003-0751-5130}}, Unique-ID = {{ISI:000535454600006}}, } @article{ ISI:000533159800006, Author = {Poisson, Eric}, Title = {{Gravitomagnetic tidal resonance in neutron-star binary inspirals}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{10}}, Month = {{MAY 15}}, Abstract = {{A compact binary system implicating at least one rotating neutron star undergoes a sequence of four gravitomagnetic tidal resonances as it inspirals toward its final merger. These resonances have a dynamical impact on the binary's orbital motion, and thus on the phasing of the emitted gravitational waves. The resonances are produced by the inertial modes of vibration of the rotating star, and they occur when the orbital frequency becomes momentarily equal to a mode eigenfrequency. Four distinct modes are involved, and their eigenfrequencies are equal, up to a numerical factor of order unity, to the star's rotational angular velocity. The resonances occur within the frequency band of interferometric gravitational-wave detectors when the star spins at a frequency that lies within this band; the phenomenon is therefore of relevance to LIGO/Virgo for rotation rates comparable to 100 Hz. The resonances are driven by the gravitomagnetic tidal field created by the companion star; this is described by a post-Newtonian vector potential (the time-space components of the metric tensor), which is produced by the mass currents associated with the orbital motion. The gravitomagnetic tidal resonances were identified previously by Flanagan and Racine {[}Phys. Rev. D 75, 044001 (2007)], but these authors accounted only for the response of a single mode, the r-mode, a special case of inertial modes. All four relevant inertial modes (including the r-mode) are included in the analysis presented in this paper. The total accumulated gravitational-wave phase shift caused by the gravitomagnetic tidal resonances is shown to range from approximately 10(-2) radians when the spin and orbital angular momenta are aligned to approximately 10(-1) radians when the angular momenta are antialigned. Such phase shifts are small, but they will become measurable in the coming decades with the deployment of the next generation of gravitational-wave detectors (Cosmic Explorer, Einstein Telescope); they might even come to light within this decade, thanks to planned improvements in the current detectors (LIGO A+). With good constraints on the binary masses and spins gathered from the inspiral waveform, the phase shifts incurred during the gravitomagnetic tidal resonances deliver information regarding the internal structure of the rotating neutron star, and therefore on the equation of state of nuclear matter at high densities.}}, DOI = {{10.1103/PhysRevD.101.104028}}, Article-Number = {{104028}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000533159800006}}, } @article{ ISI:000603578300005, Author = {Puerrer, Michael and Haster, Carl-Johan}, Title = {{Gravitational waveform accuracy requirements for future ground-based detectors}}, Journal = {{PHYSICAL REVIEW RESEARCH}}, Year = {{2020}}, Volume = {{2}}, Number = {{2}}, Month = {{MAY 11}}, Abstract = {{Future third-generation (3G) ground-based gravitational wave (GW) detectors, such as the Einstein Telescope and Cosmic Explorer, will have unprecedented sensitivities enabling studies of the entire population of stellar mass binary black hole coalescences in the universe, while the A+ and Voyager upgrades to current detectors will significantly improve over advanced LIGO and Virgo design sensitivities. To infer binary parameters from a GW signal we require accurate models of the gravitational waveform as a function of black hole masses, spins, etc. Such waveform models are built from numerical relativity (NR) simulations and/or semianalytical expressions in the inspiral. We investigate the limits of the current waveform models and study at what detector sensitivity these models will yield unbiased parameter inference for loud ``golden{''} binary black hole systems, what biases we can expect beyond these limits, and what implications such biases will have for GW astrophysics. For 3G detectors we find that the mismatch error for semianalytical models needs to be reduced by at least three orders of magnitude and for NR waveforms by one order of magnitude. We show that typical biases in units of standard deviations for the mass-ratio and effective aligned-spin will be of order unity for 2G design sensitivity and will reach several tens for 3G networks. In addition, we show that for a population of one hundred high mass precessing binary black holes, measurement errors sum up to a sizable population bias, about 10-30 times larger than the sum of 90\% credible intervals for chirp mass, mass-ratio, effective aligned, and precessing spin parameters. Furthermore, we demonstrate that the residual signal between the GW data recorded by a detector and the best fit template waveform obtained by parameter inference analyses can have significant signal-to-noise ratio and can lead to Bayes factors as high as 10(11) between a coherent and an incoherent wavelet model for the population events. This coherent power left in the residual could lead to the observation of erroneous deviations from general relativity. To address these issues and be ready to reap the scientific benefits of 3G GW detectors in the 2030s, waveform models that are significantly more physically complete and accurate need to be developed in the next decade along with major advances in efficiency and accuracy of NR codes.}}, DOI = {{10.1103/PhysRevResearch.2.023151}}, Article-Number = {{023151}}, EISSN = {{2643-1564}}, Unique-ID = {{ISI:000603578300005}}, } @article{ ISI:000531186400003, Author = {Mukherjee, Suvodip and Wandelt, Benjamin D. and Silk, Joseph}, Title = {{Multimessenger tests of gravity with weakly lensed gravitational waves}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{10}}, Month = {{MAY 8}}, Abstract = {{General relativity (GR) predicts concordant trajectories for photons and gravitational waves (GWs). We propose a new multimessenger avenue (GW-CMB-CMB) to prove this aspect of fundamental physics by cross-correlating the GW signal of astrophysical origin with the lensing field derived from the cosmic microwave background (CMB). This new window will allow robust measurement of the prediction from GR with high signal-to-noise ratio and will be able to unveil the true nature of gravity using the GW sources detected by missions such as the Laser Interferometer Space Antenna, Einstein Telescope, and Cosmic Explorer.}}, DOI = {{10.1103/PhysRevD.101.103509}}, Article-Number = {{103509}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Mukherjee, Suvodip/AAX-8173-2020}}, ORCID-Numbers = {{Mukherjee, Suvodip/0000-0002-3373-5236}}, Unique-ID = {{ISI:000531186400003}}, } @article{ ISI:000530635800002, Author = {Chen, An and Johnson-McDaniel, Nathan K. and Dietrich, Tim and Dudi, Reetika}, Title = {{Distinguishing high-mass binary neutron stars from binary black holes with second- and third-generation gravitational wave observatories}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{10}}, Month = {{MAY 6}}, Abstract = {{While the gravitational-wave (GW) signal GW170817 was accompanied by a variety of electromagnetic (EM) counterparts, sufficiently high-mass binary neutron star (BNS) mergers are expected to be unable to power bright EM counterparts. The putative high-mass binary BNS merger GW190425, for which no confirmed EM counterpart has been identified, may be an example of such a system. Since current and future GW detectors are expected to detect many more BNS mergers, it is important to understand how well we will be able to distinguish high-mass BNSs and low-mass binary black holes (BBHs) solely from their GW signals. To do this, we consider the imprint of the tidal deformability of the neutron stars on the GW signal for systems undergoing prompt black hole formation after merger. We model the BNS signals using hybrid numerical relativity-tidal effectiveone-body waveforms. Specifically, we consider a set of five nonspinning equal-mass BNS signals with total masses of 2.7, 3.0, 3.2 M-circle dot and with three different equations of state, as well as the analogous BBH signals. We perforni Bayesian parameter estimation on these signals at luminosity distances of 40 and 98 Mpc in an Advanced LIGO-Advanced Virgo network and an Advanced LIGO-Advanced Virgo-KAGRA network with sensitivities similar to the third and fourth observing runs (O3 and O4), respectively, and at luminosity distances of 369 and 835 Mpc in a network of two Cosmic Explorers and one Einstein Telescope, with a Cosmic Explorer sensitivity similar to Stage 2. Our analysis suggests that we cannot distinguish the signals from high-mass BNSs and BBHs at a 90\% credible level with the O3-like network even at 40 Mpc. However, we can distinguish all but the most compact BNSs that we consider in our study from BBHs at 40 Mpc at a >= 95\% credible level using the O4-like network and can even distinguish them at a > 99.2\% (>= 97\%) credible level at 369 (835) Mpc using the 3G network. Additionally, we present a simple method to compute the leading effect of the Earth's rotation on the response of a gravitational wave detector in the frequency domain.}}, DOI = {{10.1103/PhysRevD.101.103008}}, Article-Number = {{103008}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Chen, An/0000-0001-9174-7780 Dudi, Reetika/0000-0002-7592-3112}}, Unique-ID = {{ISI:000530635800002}}, } @article{ ISI:000535877200031, Author = {Mukherjee, Suvodip and Wandelt, Benjamin D. and Silk, Joseph}, Title = {{Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2020}}, Volume = {{494}}, Number = {{2}}, Pages = {{1956-1970}}, Month = {{MAY}}, Abstract = {{The cross-correlation of gravitational wave strain with upcoming galaxy surveys probes theories of gravity in a new way. This method enables testing the theory of gravity by combining the effects from both gravitational lensing of gravitational waves and the propagation of gravitational waves in space-time. We find that within 10 yr the combination of the Advanced LIGO (Laser Interferometer Gravitational-Wave Observatory) and VIRGO (Virgo interferometer) detector networks with planned galaxy surveys should detect weak gravitational lensing of gravitational waves in the low-redshift Universe (z < 0.5). With the next-generation gravitational wave experiments such as Voyager, LISA (Laser Interferometer Space Antenna), Cosmic Explorer, and the Einstein Telescope, we can extend this test of the theory of gravity to larger redshifts by exploiting the synergies between electromagnetic wave and gravitational wave probes.}}, DOI = {{10.1093/mnras/staa827}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Mukherjee, Suvodip/AAX-8173-2020 }}, ORCID-Numbers = {{Mukherjee, Suvodip/0000-0002-3373-5236 silk, joe/0000-0002-1566-8148}}, Unique-ID = {{ISI:000535877200031}}, } @article{ ISI:000535391600022, Author = {Bachega, Riis R. A. and Costa, Andre A. and Abdalla, E. and Fornazier, K. S. F.}, Title = {{Forecasting the interaction in dark matter-dark energy models with standard sirens from the Einstein telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{5}}, Month = {{MAY}}, Abstract = {{Gravitational Waves (GW's) can determine the luminosity distance of the progenitor directly from the amplitude of the wave, without assuming any specific cosmological model. Thus, it can be considered as a standard siren. The coalescence of binary neutron stars (BNS) or neutron star-black hole pair (NSBH) can generate GW's as well as the electromagnetic counterpart, which can be detected in a form of Gamma-Ray Bursts (GRB) and can be used to determine the redshift of the source. Consequently, such a standard siren can be a very useful probe to constrain the cosmological parameters. In this work, we consider an interacting Dark Matter-Dark Energy (DM-DE) model. Assuming some fiducial values for the parameters of our model, we simulate the luminosity distance for a ``realistic{''} and ``optimistic{''} GW+GRB events , which can be detected by the third-generation GW detector Einstein Telescope (ET). Using these simulated events, we perform a Monte Carlo Markov Chain (MCMC) to constrain the DM-DE coupling constant and other model parameters in 1 sigma and 2 sigma confidence levels. We also investigate how GW's can improve the constraints obtained by current cosmological probes.}}, DOI = {{10.1088/1475-7516/2020/05/021}}, Article-Number = {{021}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{da Costa, Andre Alencar/ABF-8322-2020}}, ORCID-Numbers = {{da Costa, Andre Alencar/0000-0002-3670-9826}}, Unique-ID = {{ISI:000535391600022}}, } @article{ ISI:000535391600012, Author = {Badurina, L. and Bentine, E. and Blas, D. and Bongs, K. and Bortoletto, D. and Bowcock, T. and Bridges, K. and Bowden, W. and Buchmueller, O. and Burrage, C. and Coleman, J. and Elertas, G. and Ellis, J. and Foot, C. and Gibson, V and Haehnelt, M. G. and Harte, T. and Hedges, S. and Hobson, R. and Holynski, M. and Jones, T. and Langlois, M. and Lellouch, S. and Lewicki, M. and Maiolino, R. and Majewski, P. and Malik, S. and March-Russell, J. and McCabe, C. and Newbold, D. and Sauer, B. and Schneider, U. and Shipsey, I and Singh, Y. and Uchida, M. A. and Valenzuela, T. and van der Grinten, M. and Vaskonen, V. and Vossebeld, J. and Weatherill, D. and Wilmut, I}, Title = {{AION: an atom interferometer observatory and network}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{5}}, Month = {{MAY}}, Abstract = {{We outline the experimental concept and key scientific capabilities of AION (Atom Interferometer Observatory and Network), a proposed experimental programme using cold strontium atoms to search for ultra-light dark matter, to explore gravitational waves in the mid-frequency range between the peak sensitivities of the LISA and LIGO/Virgo/ KA-GRA/INDIGO/Einstein Telescope/Cosmic Explorer experiments, and to probe other frontiers in fundamental physics. AION would complement other planned searches for dark matter, as well as probe mergers involving intermediate-mass black holes and explore early-universe cosmology. AION would share many technical features with the MAGIS experimental programme, and synergies would flow from operating AION in a network with this experiment, as well as with other atom interferometer experiments such as MICA, ZAIGA and ELGAR. Operating AION in a network with other gravitational wave detectors such as LIGO, Virgo and LISA would also offer many synergies.}}, DOI = {{10.1088/1475-7516/2020/05/011}}, Article-Number = {{011}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Schneider, Ulrich/N-4820-2015 McCabe, Christopher/G-5705-2014 }}, ORCID-Numbers = {{Schneider, Ulrich/0000-0003-4345-9498 McCabe, Christopher/0000-0002-4767-821X Vaskonen, Ville/0000-0003-0003-2259}}, Unique-ID = {{ISI:000535391600012}}, } @article{ ISI:000535391600029, Author = {Domcke, Valerie and Garcia-Bellido, Juan and Peloso, Marco and Pieroni, Mauro and Ricciardone, Angelo and Sorbo, Lorenzo and Tasinato, Gianmassimo}, Title = {{Measuring the net circular polarization of the stochastic gravitational wave background with interferometers}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{5}}, Month = {{MAY}}, Abstract = {{Parity violating interactions in the early Universe can source a stochastic gravitational wave background (SGWB) with a net circular polarization. In this paper, we study possible ways to search for circular polarization of the SGWB with interferometers. Planar detectors are unable to measure the net circular polarization of an isotropic SGWB. We discuss the possibility of using the dipolar anisotropy kinematically induced by the motion of the solar system with respect to the cosmic reference frame to measure the net circular polarization of the SGWB with planar detectors. We apply this approach to LISA, re-assessing previous analyses by means of a more detailed computation and using the most recent instrument specifications, and to the Einstein Telescope (ET), estimating for the first time its sensitivity to circular polarization. We find that both LISA and ET, despite operating at different frequencies, could detect net circular polarization with a signal-to-noise ratio of order one in a SGWB with amplitude h(2)Omega(Gw) similar or equal to 10(-11). We also investigate the case of a network of ground based detectors. We present fully analytical, covariant formulas for the detector overlap functions in the presence of circular polarization. Our formulas do not rely on particular choices of reference frame, and can be applied to interferometers with arbitrary angles among their arms.}}, DOI = {{10.1088/1475-7516/2020/05/028}}, Article-Number = {{028}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Garcia-Bellido, Juan/C-2920-2017}}, ORCID-Numbers = {{Domcke, Valerie/0000-0002-7208-4464 Ricciardone, Angelo/0000-0002-5688-455X Garcia-Bellido, Juan/0000-0002-9370-8360}}, Unique-ID = {{ISI:000535391600029}}, } @article{ ISI:000531325800003, Author = {von Harling, Benedict and Pomarol, Alex and Pujolas, Oriol and Rompineve, Fabrizio}, Title = {{Peccei-Quinn phase transition at LIGO}}, Journal = {{JOURNAL OF HIGH ENERGY PHYSICS}}, Year = {{2020}}, Number = {{4}}, Month = {{APR 29}}, Abstract = {{The LIGO observatories can potentially detect stochastic gravitational waves arising from phase transitions which happened in the early universe at temperatures around T similar to 10(8) GeV. This provides an extraordinary opportunity for discovering the phase transition associated with the breaking of the Peccei-Quinn symmetry, required in QCD axion models. Here we consider the simplest Peccei-Quinn models and study under which conditions a strong first-order phase transition can occur, analyzing its associated gravitational wave signal. To be detectable at LIGO, we show that some supercooling is needed, which can arise either in Coleman-Weinberg-type symmetry breaking or in strongly-coupled models. We also investigate phase transitions that interestingly proceed by first breaking the electroweak symmetry at large scales before tunneling to the Peccei-Quinn breaking vacuum. In this case, the associated gravitational wave signal is more likely to be probed at the proposed Einstein Telescope.}}, DOI = {{10.1007/JHEP04(2020)195}}, Article-Number = {{195}}, ISSN = {{1029-8479}}, ResearcherID-Numbers = {{von Harling, Benedict/AAM-3937-2020 }}, ORCID-Numbers = {{von Harling, Benedict/0000-0001-5405-714X Rompineve, Fabrizio/0000-0001-8046-1111}}, Unique-ID = {{ISI:000531325800003}}, } @article{ ISI:000530369100003, Author = {Wang, Sai}, Title = {{Exploring the CPT violation and birefringence of gravitational waves with ground- and space-based gravitational-wave interferometers}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2020}}, Volume = {{80}}, Number = {{4}}, Month = {{APR 27}}, Abstract = {{In the gravitational sector, we study the CPT violation and birefringence in gravitational waves. In presence of the CPT violation, a relative dephasing is generated between two circular polarization states of gravitational waves. This effect induces the birefringence of gravitational waves. Given the gravitational waveform modified by the CPT violation, we estimate the expected constraints on the CPT violation from Advanced Laser Interferometer Gravitational-Wave Observatory, Einstein Telescope and Laser Interferometer Space Antenna.}}, DOI = {{10.1140/epjc/s10052-020-7812-2}}, Article-Number = {{342}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ORCID-Numbers = {{Wang, Sai/0000-0001-6692-6859}}, Unique-ID = {{ISI:000530369100003}}, } @article{ ISI:000525328000001, Author = {Jones, Philip and Zhang, Teng and Miao, Haixing and Freise, Andreas}, Title = {{Implications of the quantum noise target for the Einstein Telescope infrastructure design}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{8}}, Month = {{APR 13}}, Abstract = {{The design of a complex instrument such as Einstein Telescope (ET) is based on a target sensitivity derived from an elaborate case for scientific exploration. At the same time it incorporates many trade-off decisions to maximize the scientific value by balancing the performance of the various subsystems against the cost of the installation and operation. In this paper we discuss the impact of a long signal recycling cavity (SRC) on the quantum noise performance. We show the reduction in sensitivity due to a long SRC for an ET high-frequency interferometer, provide details on possible compensations schemes and suggest a reduction of the SRC length. We also recall details of the trade-off between the length and optical losses for filter cavities, and show the strict requirements for an ET low-frequency interferometer. Finally, we present an alternative filter cavity design for an ET low-frequency interferometer making use of a coupled cavity, and discuss the advantages of the design in this context.}}, DOI = {{10.1103/PhysRevD.101.082002}}, Article-Number = {{082002}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Zhang, Teng/Y-3281-2018 }}, ORCID-Numbers = {{Zhang, Teng/0000-0001-5278-4220 Jones, Philip/0000-0001-7923-1415 Freise, Andreas/0000-0001-6586-9901}}, Unique-ID = {{ISI:000525328000001}}, } @article{ ISI:000531476300011, Author = {Belgacem, Enis and Dirian, Yves and Finke, Andreas and Foffa, Stefano and Maggiore, Michele}, Title = {{Gravity in the infrared and effective nonlocal models}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{4}}, Month = {{APR}}, Abstract = {{We provide a systematic and updated discussion of a research line carried out by our group over the last few years, in which gravity is modified at cosmological distances by the introduction of nonlocal terms, assumed to emerge at an effective level from the infrared behavior of the quantum theory. The requirement of producing a viable cosmology turns out to be very stringent and basically selects a unique model, in which the nonlocal term describes an effective mass for the conformal mode. We discuss how such a specific structure could emerge from a fundamental local theory of gravity, and we perform a detailed comparison of this model with the most recent cosmological datasets, confirming that it fits current data at the same level as Lambda CDM. Most notably, the model has striking predictions in the sector of tensor perturbations, leading to a very large effect in the propagation of gravitational wave (GWs) over cosmological distances. At the redshifts relevant for the next generation of GW detectors such as Einstein Telescope, Cosmic Explorer and LISA, this leads to deviations from GR that could be as large as 80\%, and could be verified with the detection of just a single coalescing binary with electromagnetic counterpart. This would also have potentially important consequences for the search of the counterpart since, for a given luminosity distance to the source, as inferred through the GW signal, the actual source redshift could be significantly different from that predicted by Lambda CDM. At the redshifts relevant for advanced LIGO/Virgo/Kagra the effect is smaller, but still potentially observable over a few years of runs at target sensitivity.}}, DOI = {{10.1088/1475-7516/2020/04/010}}, Article-Number = {{010}}, ISSN = {{1475-7516}}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X}}, Unique-ID = {{ISI:000531476300011}}, } @article{ ISI:000531476300053, Author = {De Luca, V and Franciolini, G. and Pani, P. and Riotto, A.}, Title = {{The evolution of primordial black holes and their final observable spins}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{4}}, Month = {{APR}}, Abstract = {{Primordial black holes in the mass range of ground-based gravitational-wave detectors can comprise a significant fraction of the dark matter. Mass and spin measurements from coalescences can be used to distinguish between an astrophysical or a primordial origin of the binary black holes. In standard scenarios the spin of primordial black holes is very small at formation. However, the mass and spin can evolve through the cosmic history due to accretion. We show that the mass and spin of primordial black holes are correlated in a redshift-dependent fashion, in particular primordial black holes with masses below O(30)M-circle dot are likely non-spinning at any redshift, whereas heavier black holes can be nearly extremal up to redshift z similar to 10. The dependence of the mass and spin distributions on the redshift can be probed with future detectors such as the Einstein Telescope. The mass and spin evolution affect the gravitational waveform parameters, in particular the distribution of the final mass and spin of the merger remnant, and that of the effective spin of the binary. We argue that, compared to the astrophysical-formation scenario, a primordial origin of black hole binaries might better explain the spin distribution of merger events detected by LIGO-Virgo, in which the effective spin parameter of the binary is compatible to zero except possibly for few high-mass events. Upcoming results from LIGO-Virgo third observation run might reinforce or weaken these predictions.}}, DOI = {{10.1088/1475-7516/2020/04/052}}, Article-Number = {{052}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Pani, Paolo/G-7412-2012 }}, ORCID-Numbers = {{Pani, Paolo/0000-0003-4443-1761 Franciolini, Gabriele/0000-0002-6892-9145}}, Unique-ID = {{ISI:000531476300053}}, } @article{ ISI:000519253000006, Author = {Zhang, Jing-Fei and Dong, Hong-Yan and Qi, Jing-Zhao and Zhang, Xin}, Title = {{Prospect for constraining holographic dark energy with gravitational wave standard sirens from the Einstein Telescope}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2020}}, Volume = {{80}}, Number = {{3}}, Month = {{MAR 6}}, Abstract = {{We study the holographic dark energy (HDE) model by using the future gravitational wave (GW) standard siren data observed from the Einstein Telescope (ET) in this work. We simulate 1000 GW standard siren data based on a 10-year observation of the ET to make this analysis. We find that all the cosmological parameters in theHDEmodel can be tremendously improved by including the GW standard siren data in the cosmological fit. TheGWdata combined with the current cosmic microwave background anisotropies, baryon acoustic oscillations, and type Ia supernovae data will measure the cosmological parameters m, H0, and c in the HDE model to be at the accuracies of 1.28\%, 0.59\%, and 3.69\%, respectively. A comparison with the cosmological constant model and the constant-w dark energy model shows that, compared to the standard model, the parameter degeneracies will be broken more thoroughly in a dynamical dark energy model. We find that the GWdata alone can provide a fairly good measurement for H0, but for other cosmological parameters the GW data alone can only provide rather weak measurements. However, due to the fact that the parameter degeneracies can be broken by the GW data, the standard sirens can play an essential role in improving the parameter estimation.}}, DOI = {{10.1140/epjc/s10052-020-7767-3}}, Article-Number = {{217}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ORCID-Numbers = {{Zhang, Xin/0000-0002-6029-1933}}, Unique-ID = {{ISI:000519253000006}}, } @article{ ISI:000517964500005, Author = {Belgacem, Enis and Foffa, Stefano and Maggiore, Michele and Yang, Tao}, Title = {{Gaussian processes reconstruction of modified gravitational wave propagation}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{6}}, Month = {{MAR 3}}, Abstract = {{Recent work has shown that modified gravitational wave (GW) propagation can be a powerful probe of dark energy and modified gravity, specific to GW observations. We use the technique of Gaussian processes, which allows the reconstruction of a function from the data without assuming any parametrization, to measurements of the GW luminosity distance from simulated joint GW-gamma-ray-burst detections, combined with measurements of the electromagnetic luminosity distance by simulated data from the dark energy survey (DES). For the GW events, we consider both a second-generation LIGO/Virgo/ Kagra (HVLKI) network, and a third-generation detector such as the Einstein Telescope. We find that the HVLKI network at target sensitivity, with O(15) neutron star binaries with an electromagnetic counterpart, could already detect deviations from general relativity at a level predicted by some modified gravity models, and a third-generation detector such as the Einstein Telescope would have a remarkable discovery potential. We discuss the complementarity of the Gaussian processes technique to the (Xi(0), n) parametrization of modified GW propagation.}}, DOI = {{10.1103/PhysRevD.101.063505}}, Article-Number = {{063505}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X Yang, Tao/0000-0002-2161-0495 Foffa, Stefano/0000-0002-4530-3051}}, Unique-ID = {{ISI:000517964500005}}, } @article{ ISI:000528029100016, Author = {Bonilla, Alexander and D'Agostino, Rocco and Nunes, Rafael C. and de Araujo, Jose C. N.}, Title = {{Forecasts on the speed of gravitational waves at high z}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{3}}, Month = {{MAR}}, Abstract = {{The observation of GW170817 binary neutron star (BNS) merger event has imposed strong bounds on the speed of gravitational waves (GWs) locally, inferring that the speed of GWs propagation is equal to the speed of light. Current GW detectors in operation will not be able to observe BNS merger to long cosmological distance, where possible cosmological corrections on the cosmic expansion history are expected to play an important role, specially for investigating possible deviations from general relativity. Future GW detectors designer projects will be able to detect many coalescences of BNS at high z, such as the third generation of the ground GW detector called Einstein Telescope (ET) and the space-based detector deci-hertz interferometer gravitational wave observatory (DECIGO). In this paper, we relax the condition c(T)/c = 1 to investigate modified GW propagation where the speed of GWs propagation is not necessarily equal to the speed of light. Also, we consider the possibility for the running of the Planck mass corrections on modified GW propagation. We parametrize both corrections in terms of an effective GW luminosity distance and we perform a forecast analysis using standard siren events from BNS mergers, within the sensitivity predicted for the ET and DECIGO. We find at high z very strong forecast bounds on the running of the Planck mass, namely O (10(-1)) and O(10(-2)) from ET and DECIGO, respectively. Possible anomalies on GW propagation are bound to vertical bar c(T)/c - 1 vertical bar <= 10(-2) (10(-2)) from ET (DECIGO), respectively. We finally discuss the consequences of our results on modified gravity phenomenology.}}, DOI = {{10.1088/1475-7516/2020/03/015}}, Article-Number = {{015}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{de Araujo, Jose C N/C-5181-2013 }}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289 Bonilla Rivera, Alexander/0000-0002-7001-0728 D'Agostino, Rocco/0000-0003-2342-1134 nunes, rafael/0000-0002-8432-5616}}, Unique-ID = {{ISI:000528029100016}}, } @article{ ISI:000528029100052, Author = {Jin, Shang-Jie and He, Dong-Ze and Xu, Yidong and Zhang, Jing-Fei and Zhang, Xin}, Title = {{Forecast for cosmological parameter estimation with gravitational-wave standard siren observation from the Cosmic Explorer}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{3}}, Month = {{MAR}}, Abstract = {{The third-generation ground-based gravitational-wave (GW) detector, Cosmic Explorer (CE), is scheduled to start its observation in the 2030s. In this paper, we make a forecast for cosmological parameter estimation with gravitational-wave standard siren observation from the CE. We use the simulated GW standard siren data of CE to constrain the Lambda CDM, wCDM and CPL models. We combine the simulated GW data with the current cosmological electromagnetic observations including the latest cosmic microwave background anisotropies data from Planck, the optical baryon acoustic oscillation measurements, and the type Ia supernovae observation (Pantheon compilation) to do the analysis. We find that the future standard siren observation from CE will improve the cosmological parameter estimation to a great extent, since the future GW standard siren data can well break the degeneracies generated by the optical observations between various cosmological parameters. We also find that the CE's constraining capability on the cosmological parameters is slightly better than that of the same-type GW detector, the Einstein Telescope. In addition, the synergy between the GW standard siren observation from CE and the 21 cm emission observation from SKA is also discussed.}}, DOI = {{10.1088/1475-7516/2020/03/051}}, Article-Number = {{051}}, ISSN = {{1475-7516}}, ORCID-Numbers = {{He, Dong-Ze/0000-0001-5344-9467 Zhang, Xin/0000-0002-6029-1933}}, Unique-ID = {{ISI:000528029100052}}, } @article{ ISI:000528029100051, Author = {Maggiore, Michele and Van den Broeck, Chris and Bartolo, Nicola and Belgacem, Enis and Bertacca, Daniele and Bizouard, Marie Anne and Branchesi, Marica and Clesse, Sebastien and Foffa, Stefano and Garcia-Bellido, Juan and Grimm, Stefan and Harms, Jan and Hinderer, Tanja and Matarrese, Sabino and Palomba, Cristiano and Peloso, Marco and Ricciardone, Angelo and Sakellariadou, Mairi}, Title = {{Science case for the Einstein telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{3}}, Month = {{MAR}}, Abstract = {{The Einstein Telescope (ET), a proposed European ground-based gravitational-wave detector of third-generation, is an evolution of second-generation detectors such as Advanced LIGO, Advanced Virgo, and KAGRA which could be operating in the mid 2030s. ET will explore the universe with gravitational waves up to cosmological distances. We discuss its main scientific objectives and its potential for discoveries in astrophysics, cosmology and fundamental physics.}}, DOI = {{10.1088/1475-7516/2020/03/050}}, Article-Number = {{050}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Garcia-Bellido, Juan/C-2920-2017 }}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X Palomba, Cristiano/0000-0002-4450-9883 PELOSO, MARCO/0000-0002-9348-9970 Sakellariadou, Mairi/0000-0002-2715-1517 Garcia-Bellido, Juan/0000-0002-9370-8360 Ricciardone, Angelo/0000-0002-5688-455X}}, Unique-ID = {{ISI:000528029100051}}, } @article{ ISI:000528029100020, Author = {Shafieloo, Arman and Keeley, Ryan E. and Linder, V, Eric}, Title = {{Will cosmic gravitational wave sirens determine the Hubble constant?}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2020}}, Number = {{3}}, Month = {{MAR}}, Abstract = {{Incorrect assumptions about the background expansion history of the Universe can induce significant biases when estimating the Hubble constant H-0 and other key cosmological parameters from cosmic (z greater than or similar to 0.1) gravitational wave standard sirens, even with electromagnetic counterpart redshifts. Future gravitational wave experiments such as the Einstein Telescope can provide us with a compilation of gravitational wave sirens that can be used to determine these cosmological parameters with very high precision. In such a future, the statistical precision can reach to the level of 1\% uncertainty on H-0. However, such datasets would include a large number of cosmic gravitational wave sirens, and not only sources at very low redshifts of z less than or similar to 0.1. We show that wrong assumptions about the background expansion history of the Universe (e.g. form of dark energy) can introduce substantial bias in estimation of the Hubble constant and the other key parameters. Such biases would occur in non-Lambda CDM cosmologies that can be degenerate with the standard Lambda CDM model. To avoid model-dependent biases, statistical techniques that are appropriately agnostic about model assumptions need to be employed.}}, DOI = {{10.1088/1475-7516/2020/03/019}}, Article-Number = {{019}}, ISSN = {{1475-7516}}, Unique-ID = {{ISI:000528029100020}}, } @article{ ISI:000519285500001, Author = {Boco, L. and Lapi, A. and Danese, L.}, Title = {{Growth of Supermassive Black Hole Seeds in ETG Star-forming Progenitors: Multiple Merging of Stellar Compact Remnants via Gaseous Dynamical Friction and Gravitational-wave Emission}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{891}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{We propose a new mechanism for the growth of supermassive black hole (BH) seeds in the star-forming progenitors of local early-type galaxies (ETGs) at z greater than or similar to 1. This envisages the migration and merging of stellar compact remnants (neutron stars and stellar-mass BHs) via gaseous dynamical friction toward the central high-density regions of such galaxies. We show that, under reasonable assumptions and initial conditions, the process can build up central BH masses of the order of 10(4)-10(6) M within some 10(7) yr, so effectively providing heavy seeds before standard disk (Eddington-like) accretion takes over to become the dominant process for further BH growth. Remarkably, such a mechanism may provide an explanation, alternative to super-Eddington accretion rates, for the buildup of billion-solar-massed BHs in quasar hosts at z greater than or similar to 7, when the age of the universe less than or similar to 0.8 Gyr constitutes a demanding constraint; moreover, in more common ETG progenitors at redshift z similar to 2-6, it can concur with disk accretion to build such large BH masses even at moderate Eddington ratios less than or similar to 0.3 within the short star formation duration less than or similar to Gyr of these systems. Finally, we investigate the perspectives to detect the merger events between the migrating stellar remnants and the accumulating central supermassive BH via gravitational-wave emission with future ground- and space-based detectors such as the Einstein Telescope and the Laser Interferometer Space Antenna.}}, DOI = {{10.3847/1538-4357/ab7446}}, Article-Number = {{94}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, Unique-ID = {{ISI:000519285500001}}, } @article{ ISI:000519097500001, Author = {Ding, Xuheng and Liao, Kai and Biesiada, Marek and Zhu, Zong-Hong}, Title = {{Black Hole Mass Function and Its Evolution-The First Prediction for the Einstein Telescope}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{891}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{Knowledge of the black hole mass function (BHMF) and its evolution would help us understand the origin of BHs and how BH binaries formed at different stages in the history of the universe. We demonstrate the ability of a future third-generation gravitational-wave (GW) detector-the Einstein Telescope (ET)-to infer the slope of the BHMF and its evolution with redshift. We perform a Monte Carlo simulation of the measurements of chirp signals from binary BH systems (BBH) that could be detected by ET, including the BH masses and their luminosity distances (d(L)). We use the mass of a primary black hole in each binary system to infer the BHMF as a power-law function with slope parameter alpha. Taking into account the bias that could be introduced by the uncertainty of measurements and by the selection effect, we carried out the numerical tests and found that only 1000 GW events registered by ET (similar to 1\% of its yearly detection rate) could accurately infer the alpha with a precision of alpha similar to 0.1. Furthermore, we investigate the validity of our method to recover a scenario where alpha evolves with redshift as d(L) as the redshift estimator, our tests show that one could infer the value of evolving parameter alpha(1) accurately at the uncertainty level of similar to 0.5. Our numerical tests verify the reliability of our method. The uncertainty levels of the inferred parameters can be trusted directly for several sets of the parameters we assumed, yet they should not be treated as general.}}, DOI = {{10.3847/1538-4357/ab7228}}, Article-Number = {{76}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Ding, Xuheng/0000-0001-8917-2148}}, Unique-ID = {{ISI:000519097500001}}, } @article{ ISI:000519056000001, Author = {Sedda, Manuel Arca}, Title = {{Birth, Life, and Death of Black Hole Binaries around Supermassive Black Holes: Dynamical Evolution of Gravitational Wave Sources}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{891}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{This paper explores the mechanisms that regulate the formation and evolution of stellar black hole binaries (BHBs) around supermassive black holes (SMBHs). We show that dynamical interactions can efficiently drive ``in situ{''} BHB formation if the SMBH is surrounded by a massive nuclear cluster, while orbitally segregated star clusters can replenish the BHB reservoir in SMBH-dominated nuclei. We discuss how the combined action of stellar hardening and mass segregation sculpts the BHB orbital properties. We use direct N-body simulations including post-Newtonian corrections up to 2.5 order to study the BHB-SMBH interplay, showing that the Kozai-Lidov mechanism plays a crucial role in shortening the lifetime of binaries. We find that the merging probability weakly depends on the SMBH mass in the 10(6)-10(9) M-circle dot range, leading to a merger rate Gamma similar or equal to 3-8 yr(-1) Gpc(-3) at redshift zero. Nearly 40\% of the mergers have masses in the ``BH mass gap,{''} 50-140 M-circle dot, thus indicating that galactic nuclei are ideal places to form BHs in this mass range. We argue that gravitational wave (GW) sources with component masses m(1) > 40 M-circle dot and m(2) < 30 M-circle dot would represent a strong indicator of a galactic nucleus origin. The majority of these mergers could be multiband GW sources in the local universe: nearly 40\% might be seen by LISA as eccentric sources and, a few years later, as circular sources by LIGO and the Einstein Telescope, making decihertz observatories like DECIGO unique instruments to bridge the observations during the binary inspiral.}}, DOI = {{10.3847/1538-4357/ab723b}}, Article-Number = {{47}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{arca-sedda, manuel/AAJ-7595-2020}}, ORCID-Numbers = {{arca-sedda, manuel/0000-0002-3987-0519}}, Unique-ID = {{ISI:000519056000001}}, } @article{ ISI:000515692300007, Author = {Liu, Xiaolin and Cao, Zhoujian and Shao, Lijing}, Title = {{Validating the effective-one-body numerical-relativity waveform models for spin-aligned binary black holes along eccentric orbits}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{4}}, Month = {{FEB 24}}, Abstract = {{Effective-one-body (EOB) numerical-relativity (NR) waveform models for spin-aligned binary black holes (BBHs), known as the SEOBNR waveform models, are based on the EOB theoretical framework and NR simulations. SEOBNR models have played an important role in the LIGO Scientific Collaboration (LSC) gravitational wave (GW) data analysis for both signal search and parameter estimation. SEOBNR models for quasicircular orbits have evolved through version 1 to version 4 by extending their validity domain and including more NR results. Along another direction, we recently extended the SEOBNRv1 model to the SEOBNRE model which is valid for spin-aligned BBH coalescence along eccentric orbits. In this paper we validate this theoretical waveform model by comparing them against the NR simulation bank, simulating extreme spacetimes (SXS) catalog. In total, 278 NR waveforms are investigated which include binaries with large eccentricity; large spin and large mass ratio. Our SEOBNRE can model the NR waveforms quite well. The fitting factor for most of the 278 waveforms is larger than 99\%. It indicates that the SEOBNRE model could be used as template waveforms for eccentric spin-aligned BBH coalescence. Moreover, we investigate the limitation in using circular BBH waveform templates in the Advanced LIGO and Einstein Telescope era.}}, DOI = {{10.1103/PhysRevD.101.044049}}, Article-Number = {{044049}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{cao, zhou jian/0000-0002-1932-7295 Shao, Lijing/0000-0002-1334-8853}}, Unique-ID = {{ISI:000515692300007}}, } @article{ ISI:000522100700072, Author = {Niu, Rui and Zhang, Xing and Liu, Tan and Yu, Jiming and Wang, Bo and Zhao, Wen}, Title = {{Constraining Screened Modified Gravity with Spaceborne Gravitational-wave Detectors}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{890}}, Number = {{2}}, Month = {{FEB 20}}, Abstract = {{Screened modified gravity (SMG) is a unified theoretical framework that describes scalar-tensor gravity with a screening mechanism. Based on the gravitational-wave (GW) waveform derived in our previous work, in this article we investigate the potential constraints on SMG theory through GW observation by future spaceborne GW detectors, including the Laser Interferometer Space Antenna (LISA), TianQin, and Taiji. We find that, for the extreme-mass-ratio inspirals (EMRIs) consisting of a massive black hole and a neutron star, if the EMRIs are at the Virgo cluster, the GW signals can be detected by the detectors at quite high significance level, and the screened parameter epsilon(NS) can be constrained at about O(10(-5)), which is more than one order of magnitude tighter than the potential constraint given by a ground-based Einstein telescope. However, for the EMRIs consisting of a massive black hole and a white dwarf, it is more difficult to detect them than in the previous case. For the specific SMG models, including chameleon, symmetron, and dilaton, we find these constraints are complementary to that from the Cassini experiment, but weaker than those from lunar laser ranging observations and binary pulsars, due to the strong gravitational potentials on the surface of neutron stars. By analyzing the deviation of the GW waveform in SMG from that in general relativity, as anticipated, we find the dominant contribution of the SMG constraint comes from the correction terms in the GW phases, rather than the extra polarization modes or the correction terms in the GW amplitudes.}}, DOI = {{10.3847/1538-4357/ab6d03}}, Article-Number = {{163}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Zhang, Xing/0000-0001-5435-6502}}, Unique-ID = {{ISI:000522100700072}}, } @article{ ISI:000513575900015, Author = {Bhagwat, Swetha and Forteza, Xisco Jimenez and Pani, Paolo and Ferrari, Valeria}, Title = {{Ringdown overtones, black hole spectroscopy, and no-hair theorem tests}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{4}}, Month = {{FEB 14}}, Abstract = {{Validating the black hole no-hair theorem with gravitational-wave observations of compact binary coalescences provides a compelling argument that the remnant object is indeed a black hole as described by the general theory of relativity. This requires performing a spectroscopic analysis of the postmerger signal and resolving the frequencies of either different angular modes or overtones (of the same angular mode). For a nearly-equal-mass binary black hole system, only the dominant angular mode (l = m = 2) is sufficiently excited, and the overtones are instrumental to performing this test. Here we investigate the robustness of modeling the postmerger signal of a binary black hole coalescence as a superposition of overtones. Further, we study the bias expected in the recovered frequencies as a function of the start time of a spectroscopic analysis and provide a computationally cheap procedure to choose it based on the interplay between the expected statistical error due to the detector noise and the systematic errors due to waveform modeling. Moreover, since the overtone frequencies are closely spaced, we find that resolving the overtones is particularly challenging and requires a loud ringdown signal. Rayleigh's resolvability criterion suggests that-in an optimistic scenario-a ringdown signal-to-noise ratio larger than similar to 30 (achievable possibly with LIGO at design sensitivity and routinely with future interferometers such as the Einstein Telescope, Cosmic Explorer, and LISA) is necessary to resolve the overtone frequencies. We then conclude by discussing some conceptual issues associated with black hole spectroscopy with overtones.}}, DOI = {{10.1103/PhysRevD.101.044033}}, Article-Number = {{044033}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Pani, Paolo/G-7412-2012 }}, ORCID-Numbers = {{Pani, Paolo/0000-0003-4443-1761 Ferrari, Valeria/0000-0002-0600-6070 Bhagwat, Swetha/0000-0003-4700-5274}}, Unique-ID = {{ISI:000513575900015}}, } @article{ ISI:000523306600005, Author = {Tringali, Maria C. and Bulik, Tomasz and Harms, Jan and Fiori, Irene and Paoletti, Federico and Singh, Neha and Idzkowski, Bartosz and Kutynia, Adam and Nikliborc, Krzysztof and Suchinski, Maciej and Bertolini, Alessandro and Koley, Soumen}, Title = {{Seismic array measurements at Virgo's west end building for the configuration of a Newtonian-noise cancellation system}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2020}}, Volume = {{37}}, Number = {{2}}, Month = {{JAN 23}}, Abstract = {{Terrestrial gravity fluctuations produce so-called Newtonian noise (NN) which is expected to limit the low frequency sensitivity of existing gravitational-waves (GW) detectors LIGO and Virgo, when they will reach their full potential, and of next-generation detectors like the Einstein Telescope. In this paper, we present a detailed characterization of the seismic field at Virgo's west end building as part of the development of a Newtonian noise cancellation system. The cancellation system will use optimally filtered data from a seismometer array to produce an estimate of the Newtonian-noise generated by the seismic field, and to subtract this estimate from the gravitational-wave channel of the detector. By using an array of 38 seismic sensors, we show that, despite the influence of the complexity of Virgo's infrastructure on the correlation across the array, Wiener filtering can still be very efficient in reconstructing the seismic field around the test-mass location. Taking into account the division of the building's foundations into separate concrete slabs, and the different properties of the seismic field across them, we conclude that the arrays to be used for the Newtonian-noise cancellation at Virgo will require a relatively large number of seismometers per test mass, i.e. significantly more than 10. Moreover, observed variations of the absolute noise residuals over time, related to the daily evolution of anthropogenic noise, suggest that the Wiener filter will need to be updated regularly, probably more often than every hour, to achieve stationarity of the background level after subtraction.}}, DOI = {{10.1088/1361-6382/ab5c43}}, Article-Number = {{025005}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Harms, Jan/J-4359-2012 }}, ORCID-Numbers = {{Tringali, Maria Concetta/0000-0001-5087-189X Bulik, Tomasz/0000-0003-2045-4803 Idzkowski, Bartosz/0000-0001-5869-2714 Harms, Jan/0000-0002-7332-9806 Paoletti, Federico/0000-0001-8898-1963}}, Unique-ID = {{ISI:000523306600005}}, } @article{ ISI:000509498400011, Author = {Maselli, Andrea and Pani, Paolo and Gualtieri, Leonardo and Berti, Emanuele}, Title = {{Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{2}}, Month = {{JAN 22}}, Abstract = {{Black-hole spectroscopy is arguably the most promising tool to test gravity in extreme regimes and to probe the ultimate nature of black holes with unparalleled precision. These tests are currently limited by the lack of a ringdown parametrization that is both robust and accurate. We develop an observable-based parametrization of the ringdown of spinning black holes beyond general relativity, which we dub ParSpec (parametrized ringdown spin expansion coefficients). This approach is perturbative in the spin, but it can be made arbitrarily precise (at least in principle) through a high-order expansion. It requires O(10) ringdown detections, which should be routinely available with the planned space mission LISA and with third-generation ground-based detectors. We provide a preliminary analysis of the projected bounds on parametrized ringdown parameters with LISA and with the Einstein Telescope, and discuss extensions of our model that can be straightforwardly included in the future.}}, DOI = {{10.1103/PhysRevD.101.024043}}, Article-Number = {{024043}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Gualtieri, Leonardo/F-2612-2012 Berti, Emanuele/C-9331-2016 Pani, Paolo/G-7412-2012}}, ORCID-Numbers = {{Gualtieri, Leonardo/0000-0002-1097-3266 Berti, Emanuele/0000-0003-0751-5130 Maselli, Andrea/0000-0001-8515-8525 Pani, Paolo/0000-0003-4443-1761}}, Unique-ID = {{ISI:000509498400011}}, } @article{ ISI:000520565600001, Author = {Wu, Yan and Cao, Shuo and Zhang, Jia and Liu, Tonghua and Liu, Yuting and Geng, Shuaibo and Lian, Yujie}, Title = {{Exploring the ``L-sigma{''} Relation of H ii Galaxies and Giant Extragalactic H ii Regions Acting as Standard Candles}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2020}}, Volume = {{888}}, Number = {{2}}, Month = {{JAN 10}}, Abstract = {{Cosmological applications of H ii galaxies and giant extragalactic H ii regions (GEHRs) to construct the Hubble diagram at high redshifts require knowledge of the ``L-sigma{''} relation of the standard candles used. In this paper, we study the properties of a large sample of 156 sources (25 high-z H ii galaxies, 107 local H ii galaxies, and 24 GEHRs) compiled by Terlevich et al. Using the cosmological distances reconstructed through two new cosmology-independent methods, we investigate the correlation between the H beta emission-line luminosity L and the ionized gas velocity dispersion sigma. The method is based on non-parametric reconstruction using the measurements of Hubble parameters from cosmic clocks, as well as the simulated data of gravitational waves from the third-generation gravitational wave detector (the Einstein Telescope, ET), which can be considered as standard sirens. Assuming the relation between emission-line luminosity and ionized gas velocity dispersion, we find that the full sample provides a tight constraint on the correlation parameters. However, similar analysis done on three different subsamples seems to support the scheme of treating H ii galaxies and GEHRs with distinct strategies. Using the corrected ``L-sigma{''} relation for the H ii observational sample beyond the current reach of Type Ia supernovae, we obtain values of the matter density parameter, omega(m) = 0.314 0.054 (calibrated with standard clocks) and omega(m) = 0.311 0.049 (calibrated with standard sirens), in the spatially flat ?CDM cosmology.}}, DOI = {{10.3847/1538-4357/ab5b94}}, Article-Number = {{113}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Cao, Shuo/0000-0002-8870-981X}}, Unique-ID = {{ISI:000520565600001}}, } @article{ ISI:000506593500001, Author = {Bernard, Laura}, Title = {{Dipolar tidal effects in scalar-tensor theories}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{2}}, Month = {{JAN 10}}, Abstract = {{The inclusion of finite-size effects in the gravitational waveform templates allows one not only to constrain the internal structure of compact objects, but to test deviations from general relativity. Here, we address the problem of tidal effects in massless scalar-tensor theories. We introduce the scalar-type tidal Love numbers that relate the time-varying scalar dipole moment to the induced scalar tidal field. We compute the leading-order scalar tidal contribution in the conservative dynamics and for the first time in the wave generation for quasicircular orbits. Importantly, we show that, in a system dominated by dipolar emission, such tidal effects may be detectable by third generation detectors such as the Einstein Telescope.}}, DOI = {{10.1103/PhysRevD.101.021501}}, Article-Number = {{021501}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000506593500001}}, } @article{ ISI:000506592700001, Author = {Tsuchida, Satoshi and Kanda, Nobuyuki and Itoh, Yousuke and Mori, Masaki}, Title = {{Dark matter signals on a laser interferometer}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2020}}, Volume = {{101}}, Number = {{2}}, Month = {{JAN 8}}, Abstract = {{WIMPs are promising dark matter candidates. A WIMP occasionally collides with a mirror equipped with interferometric gravitational wave detectors such as LIGO, Virgo, KAGRA and the Einstein Telescope (ET). When WIMPs collide with a mirror of an interferometer, we expect that characteristic motions of the pendulum and mirror are excited, and those signals could be extracted by highly sophisticated sensors developed for gravitational wave detection. We analyze the motions of the pendulum and mirror, and estimate the detectability of these motions. For the ``Thin-ET{''} detector, the signal-to-noise ratio may be 1.7(m(DM)/100 GeV), where m(DM) is the mass of a WIMP. We may set a more strict upper limit on the cross section between a WIMP and a nucleon than the limits obtained by other experiments so far when m(DM) is approximately lower than 0.2 GeV. We find an order-of-magnitude improvement in the upper limit around m(DM) = 0.2 GeV.}}, DOI = {{10.1103/PhysRevD.101.023005}}, Article-Number = {{023005}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Mori, Masaki/0000-0003-2921-1592}}, Unique-ID = {{ISI:000506592700001}}, } @inproceedings{ ISI:000539995300220, Author = {Miyo, Koseki and KAGRA Collaboration}, Book-Group-Author = {{IOP}}, Title = {{Global control using a laser strainmeter for KAGRA}}, Booktitle = {{16TH INTERNATIONAL CONFERENCE ON TOPICS IN ASTROPARTICLE AND UNDERGROUND PHYSICS (TAUP 2019)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2020}}, Volume = {{1468}}, Note = {{16th International Conference on Topics in Astroparticle and Underground Physics (TAUP), Univ Tokyo, Inst Cosm Ray Res, Toyama, JAPAN, SEP 09-13, 2019}}, Abstract = {{The KAGRA is a large-scale laser interferometric gravitational wave (GW) telescope that is has been constructed in Japan's underground. Underground telescopes such as KAGRA and the proposed Einstein Telescope have the advantage of substantially reduced seismic noise above 1 Hz relative to GW telescopes on the surface. However, even in underground, seismic motion at low frequencies such as microseisms (< 1 Hz) and earthquakes (< 10 mHz), could severely degrade GW telescopes' stability. In the current design of the KAGRA, these disturbances are suppressed by feedback controls using inertial sensors such as seismometers and geophones. Nevertheless, suppression with this control method is limited by the insufficient sensitivity and tilt-horizontal coupling of the sensors at low frequencies. In this paper, we have developed a new control method based on a laser strainmeter named the Geophysics Interferometer (GIF) to resolve this problem. This was installed in the KAGRA tunnel and has a superior sensitivity of less than 100 mHz and no problems with tilt coupling. This new method will achieve improved stability for the operation of an interferometer. Also presented in the paper is the design of the control system and an experimental result.}}, DOI = {{10.1088/1742-6596/1468/1/012221}}, Article-Number = {{012221}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, Unique-ID = {{ISI:000539995300220}}, } @inproceedings{ ISI:000539995300240, Author = {Naticchioni, L. and Boschi, V. and Calloni, E. and Capello, M. and Cardini, A. and Carpinelli, M. and Cuccuru, S. and D'Ambrosio, M. and de Rosa, R. and Di Giovanni, M. and d'Urso, D. and Fiori, I. and Gaviano, S. and Giunchi, C. and Majorana, E. and Migoni, C. and Oggiano, G. and Olivieri, M. and Paoletti, F. and Paratore, M. and Perciballi, M. and Piccinini, D. and Punturo, M. and Puppo, P. and Rapagnani, P. and Ricci, F. and Saccorotti, G. and Sipala, V. and Tringali, M. C.}, Book-Group-Author = {{IOP}}, Title = {{Characterization of the Sos Enattos site for the Einstein Telescope}}, Booktitle = {{16TH INTERNATIONAL CONFERENCE ON TOPICS IN ASTROPARTICLE AND UNDERGROUND PHYSICS (TAUP 2019)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2020}}, Volume = {{1468}}, Note = {{16th International Conference on Topics in Astroparticle and Underground Physics (TAUP), Univ Tokyo, Inst Cosm Ray Res, Toyama, JAPAN, SEP 09-13, 2019}}, Abstract = {{In this work we report the ongoing characterization of the Sos Enattos former mine (Sardinia, Italy), one of the two candidate sites for the Einstein Telescope (ET), the European third-generation underground interferometric detector of Gravitational Waves. The Sos Enattos site lies on a crystalline basement, made of rocks with good geomechanical properties, characterized by negligible groundwater. In addition, the site has a very low seismic background noise due to the absence of active tectonics involving Sardinia. Finally, the area has a low population density, resulting in a reduced anthropic noise even at the ground level. This location was already studied in 2012-2014 as a promising site for an underground detector. More recently, in March 2019, we deployed a new network of surface and underground seismometers at the site, that is currently monitoring the local seismic noise. Most of the energy carried by the seismic waves is due to the microseisms below 1 Hz, showing a significant correlation with the waves of the west Mediterranean sea. Above 1 Hz the seismic noise in the underground levels of the mine approaches the Peterson's low noise model. Exploiting mine blasting works into the former mine, we were also able to perform active seismic measurements to evaluate the seismic waves propagation across the area. In conclusion we also give a first assessment about the acoustic and magnetic noise in this underground site.}}, DOI = {{10.1088/1742-6596/1468/1/012242}}, Article-Number = {{012242}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, ResearcherID-Numbers = {{Naticchioni, Luca/AAB-7775-2019 Punturo, Michele/I-3995-2012 Giunchi, Carlo/H-8508-2012}}, ORCID-Numbers = {{Naticchioni, Luca/0000-0003-2918-0730 Punturo, Michele/0000-0001-8722-4485 Tringali, Maria Concetta/0000-0001-5087-189X Giunchi, Carlo/0000-0002-0174-324X}}, Unique-ID = {{ISI:000539995300240}}, } @article{ ISI:000513509200018, Author = {Fenyvesi, Edit and Molnar, Jozsef and Czellar, Sandor}, Title = {{Investigation of Infrasound Background Noise at Matra Gravitational and Geophysical Laboratory (MGGL)}}, Journal = {{UNIVERSE}}, Year = {{2020}}, Volume = {{6}}, Number = {{1}}, Month = {{JAN}}, Abstract = {{Infrasound and seismic waves are supposed to be the main contributors to the gravity-gradient noise (Newtonian noise) of the third-generation subterranean gravitational wave detectors. This noise will limit the sensitivity of the instrument at frequencies below 20 Hz. Investigation of its origin and the possible methods of mitigation have top priority during the designing period of the detectors. Therefore, long-term site characterizing measurements are needed at several subterranean sites. However, at some sites, mining activities can occur. These activities can cause sudden changes (transients) in the measured signal, and increase the continuous background noise, too. We have developed an algorithm based on discrete Haar transform to find these transients in the infrasound signal. We found that eliminating the transients decreases the variation of the noise spectra, and therefore results a more accurate characterization of the continuous background noise. We carried out experiments for controlling the continuous noise. Machines operating at the mine were turned on and off systematically in order to see their effect on the noise spectra. These experiments showed that the main contributor of the continuous noise is the ventilation system of the mine. We also estimated the contribution of infrasound Newtonian noise at MGGL to the strain noise of a subterranean GW detector similar to Einstein Telescope.}}, DOI = {{10.3390/universe6010010}}, Article-Number = {{10}}, EISSN = {{2218-1997}}, ResearcherID-Numbers = {{Fenyvesi, Edit/B-9076-2018}}, ORCID-Numbers = {{Fenyvesi, Edit/0000-0003-2777-3719}}, Unique-ID = {{ISI:000513509200018}}, } @article{ ISI:000504638100001, Author = {Zhou, Lu and Fu, Xiangyun and Peng, Zhaohui and Chen, Jun}, Title = {{Probing the cosmic opacity from future gravitational wave standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{12}}, Month = {{DEC 24}}, Abstract = {{In this work, using the Gaussian process, we explore the potentiality of future gravitational wave (GW) measurement to probe cosmic opacity through comparing its opacity-free luminosity distance (LD) with the opacity-dependent one from type Ia supernovae (SNIa). GW data points are simulated from the third-generation Einstein Telescope, and SNIa data are taken from the Joint Light Analysis (JLA) or Pantheon compilation. The advantages of using the Gaussian process are that one may match SNIa data with GW data at the same redshift and use all available data to probe cosmic opacity. We obtain that the error bar of the constraint on cosmic opacity can be reduced to sigma(epsilon) similar to 0.011 and 0.006 at la confidence level (CL) for JLA and Pantheon, respectively, in a cosmological-independent way. Thus, the future GW measurements can give competitive results on the cosmic opacity test. Furthermore, we propose a method to probe the spatial homogeneity of the cosmic transparency through comparing the reconstructed LD from the mock GW with the reconstructed one from SNIa data in a flat ACDM with the Gaussian process. The result shows that a transparent universe is favored at 1 sigma CL, although the best-fit value of cosmic opacity is redshift dependent.}}, DOI = {{10.1103/PhysRevD.100.123539}}, Article-Number = {{123539}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000504638100001}}, } @article{ ISI:000503048900004, Author = {Bertone, Gianfranco and Coogan, Adam M. and Gaggero, Daniele and Kavanagh, Bradley J. and Weniger, Christoph}, Title = {{Primordial black holes as silver bullets for new physics at the weak scale}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{12}}, Month = {{DEC 17}}, Abstract = {{Observational constraints on gamma rays produced by the annihilation of weakly interacting massive particles around primordial black holes (PBHs) imply that these two classes of dark matter candidates cannot coexist. We show here that the successful detection of one or more PBHs by radio searches (with the Square Kilometer Array) and gravitational wave searches (with LIGO/Virgo and the upcoming Einstein Telescope) would set extraordinarily stringent constraints on virtually all weak-scale extensions of the standard model with stable relics, including those predicting a WIMP abundance much smaller than that of dark matter. Upcoming PBH searches have in particular the potential to rule out almost the entire parameter space of popular theories such as the minimal supersymmetric standard model and scalar singlet dark matter.}}, DOI = {{10.1103/PhysRevD.100.123013}}, Article-Number = {{123013}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Kavanagh, Bradley/AAB-1239-2021 Gaggero, Daniele/ABB-8175-2020 }}, ORCID-Numbers = {{Kavanagh, Bradley/0000-0002-3634-4679 Gaggero, Daniele/0000-0003-3534-1406}}, Unique-ID = {{ISI:000503048900004}}, } @article{ ISI:000499696200007, Author = {Qi, Jing-Zhao and Cao, Shuo and Pan, Yu and Li, Jin}, Title = {{Cosmic opacity: Cosmological-model-independent tests from gravitational waves and Type Ia Supernova}}, Journal = {{PHYSICS OF THE DARK UNIVERSE}}, Year = {{2019}}, Volume = {{26}}, Month = {{DEC}}, Abstract = {{In this paper, we present a scheme to investigate the opacity of the Universe in a cosmological-model-independent way, with the combination of current and future available data in gravitational wave (GW) and electromagnetic (EM) domain. In the FLRW metric, GWs propagate freely through a perfect fluid without any absorption and dissipation, which provides a distance measurement unaffected by the cosmic opacity. Focusing on the simulated data of gravitational waves from the third-generation gravitational wave detector (the Einstein Telescope, ET), as well as the newly-compiled SNe Ia data (JLA and Pantheon sample), we find an almost transparent universe is strongly favored at much higher redshifts (z similar to 2.26). Our results suggest that, although the tests of cosmic opacity are not significantly sensitive to its parametrization, a strong degeneracy between the cosmic opacity parameter and the absolute B-band magnitude of SNe Ia is revealed in this analysis. More importantly, we obtain that future measurements of the luminosity distances of gravitational waves sources will be much more competitive than the current analyses, which makes it expectable more vigorous and convincing constraints on the cosmic opacity (and consequently on background physical mechanisms) and a deeper understanding of the intrinsic properties of type Ia supernovae in a cosmological-model-independent way. (C) 2019 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.dark.2019.100338}}, Article-Number = {{100338}}, ISSN = {{2212-6864}}, ResearcherID-Numbers = {{Qi, JingZhao/AAC-9594-2020}}, Unique-ID = {{ISI:000499696200007}}, } @article{ ISI:000496926900091, Author = {Kalita, Surajit and Mukhopadhyay, Banibrata}, Title = {{Continuous gravitational wave from magnetized white dwarfs and neutron stars: possible missions for LISA, DECIGO, BBO, ET detectors}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2019}}, Volume = {{490}}, Number = {{2}}, Pages = {{2692-2705}}, Month = {{DEC}}, Abstract = {{Recent detection of gravitational wave from nine black hole merger events and one neutron star merger event by LIGO and VIRGO shed a new light in the field of astrophysics. On the other hand, in the past decade, a few super-Chandrasekhar white dwarf candidates have been inferred through the peak luminosity of the light curves of a few peculiar Type Ia supernovae, though there is no direct detection of these objects so far. Similarly, a number of neutron stars with mass > 2 M-circle dot have also been observed. Continuous gravitational wave can be one of the alternate ways to detect these compact objects directly. It was already argued that magnetic field is one of the prominent physics to form super-Chandrasekhar white dwarfs and massive neutron stars. If such compact objects are rotating with certain angular frequency, then they can efficiently emit gravitational radiation, provided their magnetic field and rotation axes are not aligned, and these gravitational waves can be detected by some of the upcoming detectors, e.g. LISA, BBO, DECIGO, Einstein Telescope, etc. This will certainly be a direct detection of rotating magnetized white dwarfs as well as massive neutron stars.}}, DOI = {{10.1093/mnras/stz2734}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Kalita, Surajit/0000-0002-3818-6037 Mukhopadhyay, Banibrata/0000-0002-3020-9513}}, Unique-ID = {{ISI:000496926900091}}, } @article{ ISI:000507259700019, Author = {Belgacem, Enis and Dirian, Yves and Finke, Andreas and Foffa, Stefano and Maggiore, Michele}, Title = {{Nonlocal gravity and gravitational-wave observations}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2019}}, Number = {{11}}, Month = {{NOV}}, Abstract = {{We discuss a modified gravity model which fits cosmological observations at a level statistically indistinguishable from Lambda CDM and at the same time predicts very large deviations from General Relativity (GR) in the propagation of gravitational waves (GWs) across cosmological distances. The model is a variant of the RT nonlocal model proposed and developed by our group, with initial conditions set during inflation, and predicts a GW luminosity distance that, at the redshifts accessible to LISA or to a third-generation GW detector such as the Einstein Telescope (ET), can differ from that in GR by as much as 60\%. An effect of this size could be detected with just a single standard siren with counterpart by LISA or ET. At the redshifts accessible to a LIGO/Virgo/Kagra network at target sensitivity the effect is smaller but still potentially detectable. Indeed, for the recently announced LIGO/Virgo NS-BH candidate S190814bv, the RT model predicts that, given the measured GW luminosity distance, the actual luminosity distance, and the redshift of an electromagnetic counterpart, would be smaller by as much as 7\% with respect to the value inferred from Lambda CDM.}}, DOI = {{10.1088/1475-7516/2019/11/022}}, Article-Number = {{022}}, ISSN = {{1475-7516}}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X}}, Unique-ID = {{ISI:000507259700019}}, } @article{ ISI:000499628800004, Author = {Zhang, Tong-Jie and Liu, Yang and Liu, Zhi-E and Wan, Hao-Yi and Zhang, Ting-Ting and Wang, Bao-Quan}, Title = {{The constraint ability of Hubble parameter by gravitational wave standard sirens on cosmological parameters}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2019}}, Volume = {{79}}, Number = {{11}}, Month = {{NOV}}, Abstract = {{In this paper, we present the application of a new method measuring Hubble parameter H(z) by using the anisotropy of luminosity distance (d(L)) of the gravitational wave (GW) standard sirens of neutron star (NS) binary system. The method has never been put into practice so far due to the lack of the ability of detecting GW. However, LIGO's success in detecting GW of black hole (BH) binary system merger announced the potential possibility of this new method. We apply this method to several GW detecting projects, including Advanced LIGO (aLIGO), Einstein Telescope (ET) and DECIGO, and evaluate its constraint ability on cosmological parameters of H(z). It turns out that the H(z) by aLIGO and ET is of bad accuracy, while the H(z) by DECIGO shows a good one. We simulate H(z) data at every 0.1 redshift span using the error information of H(z) by DECIGO, and put the mock data into the forecasting of cosmological parameters. Compared with the previous data and method, we get an obviously tighter constraint on cosmological parameters by mock data, and a concomitantly higher value of Figure of Merit (FoM, the reciprocal of the area enclosed by the 2 sigma confidence region). For a 3-year-observation by standard sirens of DECIGO, the FoM value is as high as 170.82. If a 10-year-observation is launched, the FoM could reach 569.42. For comparison, the FoM of 38 actual observed H(z) data (OHD) is 9.3. We also investigate the undulant universe, which shows a comparable improvement on the constraint of cosmological parameters. These improvement indicates that the new method has great potential in further cosmological constraints.}}, DOI = {{10.1140/epjc/s10052-019-7434-8}}, Article-Number = {{900}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, Unique-ID = {{ISI:000499628800004}}, } @article{ ISI:000501029200001, Author = {Hall, Evan D. and Evans, Matthew}, Title = {{Metrics for next-generation gravitational-wave detectors}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2019}}, Volume = {{36}}, Number = {{22}}, Month = {{OCT 15}}, Abstract = {{Gravitational-wave astrophysics has the potential to be transformed by a global network of longer, colder, and thus more sensitive detectors. This network must be constructed to address a wide range of science goals, involving binary coalescence signals as well as signals from other, potentially unknown, sources. It is crucial to understand which network configurations-the number, type, and location of the detectors in the network-can best achieve these goals. In this work we examine a large number of possible three-detector networks, variously composed of Voyager, Einstein Telescope, and Cosmic Explorer detectors, and evaluate their performance against a number of figures of merit meant to capture a variety of future science goals. From this we infer that network performance, including sky localization, is determined most strongly by the type of detectors contained in the network, rather than the location and orientation of the facilities.}}, DOI = {{10.1088/1361-6382/ab41d6}}, Article-Number = {{225002}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ORCID-Numbers = {{Hall, Evan/0000-0001-9018-666X}}, Unique-ID = {{ISI:000501029200001}}, } @article{ ISI:000489827700003, Author = {Beckey, Jacob L. and Ma, Yiqiu and Boyer, Vincent and Miao, Haixing}, Title = {{Broadband quantum noise reduction in future long baseline gravitational-wave detectors via EPR entanglement}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{8}}, Month = {{OCT 14}}, Abstract = {{Broadband quantum noise reduction can be achieved in gravitational-wave detectors by injecting frequency-dependent squeezed light into the dark port of the interferometer. This frequency-dependent squeezing can be generated by combining squeezed light with external filter cavities. However, in future long baseline interferometers (LBIs), the filter cavity required to achieve the broadband squeezing has a low bandwidth-necessitating a very long cavity to mitigate the issue from optical loss. It has been shown recently that by taking advantage of Einstein-Podolsky-Rosen (EPR) entanglement in the squeezed light source, the interferometer can simultaneously act as a detector and a filter cavity. This is an attractive broadband squeezing scheme for LBIs because the length requirement for the filter cavity is naturally satisfied by the length of the interferometer arms. In this paper we present a systematic way of finding the working points for this broadband squeezing scheme in LBIs. We also show that in LBIs, the EPR scheme achieves nearly perfect ellipse rotation as compared to 4-km interferometers which have appreciable error around the intermediate frequency. Finally, we show that an approximation for the optomechanical coupling constant in the 4-km case can break down for longer baselines. These results are applicable to future detectors such as the 10-km Einstein Telescope and the 40-km Cosmic Explorer.}}, DOI = {{10.1103/PhysRevD.100.083011}}, Article-Number = {{083011}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Miao, Haixing/0000-0003-2879-5821 Beckey, Jacob/0000-0002-2009-8661 Boyer, Vincent/0000-0002-6900-8786}}, Unique-ID = {{ISI:000489827700003}}, } @article{ ISI:000488261900008, Author = {Maggio, Elisa and Testa, Adriano and Bhagwat, Swetha and Pani, Paolo}, Title = {{Analytical model for gravitational-wave echoes from spinning remnants}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{6}}, Month = {{SEP 26}}, Abstract = {{Gravitational-wave echoes in the postmerger signal of a binary coalescence are predicted in various scenarios, including near-horizon quantum structures, exotic states of matter in ultracompact stars, and certain deviations from general relativity. The amplitude and frequency of each echo is modulated by the photon-sphere barrier of the remnant, which acts as a spin- and frequency-dependent high-pass filter, decreasing the frequency content of each subsequent echo. Furthermore, a major fraction of the energy of the echo signal is contained in low-frequency resonances corresponding to the quasinormal modes of the remnant. Motivated by these features, in this work we provide an analytical gravitational-wave template in the low-frequency approximation describing the postmerger ringdown and the echo signal of a spinning ultracompact object. Besides the standard ringdown parameters, the template is parametrized in terms of only two physical quantities: the reflectivity coefficient and the compactness of the remnant. We discuss novel effects related to the spin and to the complex reflectivity, such as a more involved modulation of subsequent echoes, the mixing of two polarizations, and the ergoregion instability in the case of perfectly reflecting spinning remnants. Finally, we compute the errors in the estimation of the template parameters with current and future gravitational-wave detectors using a Fisher matrix framework. Our analysis suggests that models with almost perfect reflectivity can be excluded/detected with current instruments, whereas probing values of the reflectivity smaller than 80\% at the 3 sigma confidence level requires future detectors (Einstein Telescope, Cosmic Explorer, LISA). The template developed in this work can easily be implemented to perform a matched-filter based search for echoes and to constrain models of exotic compact objects.}}, DOI = {{10.1103/PhysRevD.100.064056}}, Article-Number = {{064056}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Maggio, Elisa/AAO-6422-2020 Pani, Paolo/G-7412-2012 }}, ORCID-Numbers = {{Maggio, Elisa/0000-0002-1960-8185 Pani, Paolo/0000-0003-4443-1761 Bhagwat, Swetha/0000-0003-4700-5274 Testa, Adriano/0000-0003-4423-9243}}, Unique-ID = {{ISI:000488261900008}}, } @article{ ISI:000485197900007, Author = {Nunes, Rafael C. and Alves, Marcio E. S. and de Araujo, Jose C. N.}, Title = {{Forecast constraints on f(T) gravity with gravitational waves from compact binary coalescences}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{6}}, Month = {{SEP 9}}, Abstract = {{The direct detection of gravitational waves (GWs) opened a new chapter in the modern cosmology to probe possible deviations from the general relativity (GR) theory. In the present work, we investigate for the first time the modified GW form propagation from the inspiraling of compact binary systems within the context of f (T) gravity in order to obtain new forecasts/constraints on the free parameter of the theory. First, we show that the modified waveform differs from the GR waveform essentially due to induced corrections on the GWs amplitude. Then, we discuss the forecasts on the f (T) gravity assuming simulated sources of GWs as black hole binaries, neutron star binaries and black hole-neutron star binary systems, which emit GWs in the frequency band of the Advanced LIGO (aLIGO) interferometer and of the third generation Einstein Telescope (ET). We show that GW sources detected within the aLIGO sensitivity can return estimates of the same order of magnitude of the current cosmological observations. On the other hand, detection within the ET sensitivity can improve by up to 2 orders of magnitude the current bound on the f(T) gravity. Therefore, the statistical accuracy that can be achieved by future ground based GW observations, mainly with the ET detector (and planed detectors with a similar sensitivity), can allow strong bounds on the free parameter of the theory, and can be decisive to test the theory of gravitation.}}, DOI = {{10.1103/PhysRevD.100.064012}}, Article-Number = {{064012}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Alves, Marcio E.S./AAB-5094-2019 de Araujo, Jose C N/C-5181-2013}}, ORCID-Numbers = {{Alves, Marcio E.S./0000-0002-7063-694X de Araujo, Jose C N/0000-0003-4418-4289}}, Unique-ID = {{ISI:000485197900007}}, } @article{ ISI:000516537200003, Author = {Zhang, Jing-Fei and Zhang, Ming and Jin, Shang-Jie and Qi, Jing-Zhao and Zhang, Xin}, Title = {{Cosmological parameter estimation with future gravitational wave standard siren observation from the Einstein Telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2019}}, Number = {{9}}, Month = {{SEP}}, Abstract = {{In this work, we use the simulated gravitational wave (GW) standard siren data from the future observation of the Einstein Telescope (ET) to constrain various dark energy cosmological models, including the wCDM, wCDM, CPL, alpha DE, GCG, and NGCG models. We also use the current mainstream cosmological electromagnetic observations, i.e., the cosmic microwave background anisotropies data, the baryon acoustic oscillations data, and the type Ia supernovae data, to constrain these models. We find that the GW standard siren data could tremendously improve the constraints on the cosmological parameters for all these dark energy models. For all the cases, the GW standard siren data can be used to break the parameter degeneracies generated by the current cosmological electromagnetic observational data. Therefore, it is expected that the future GW standard siren observation from the ET would play a crucial role in the cosmological parameter estimation in the future. The conclusion of this work is quite solid because it is based on the analysis for various dark energy models.}}, DOI = {{10.1088/1475-7516/2019/09/068}}, Article-Number = {{068}}, ISSN = {{1475-7516}}, ORCID-Numbers = {{Zhang, Xin/0000-0002-6029-1933}}, Unique-ID = {{ISI:000516537200003}}, } @article{ ISI:000489062100001, Author = {Van, P. and Barnafoldi, G. G. and Bulik, T. and Biro, T. and Czellar, S. and Cieslar, M. and Czanik, Cs and David, E. and Debreceni, E. and Denys, M. and Dobroka, M. and Fenyvesi, E. and Gondek-Rosinska, D. and Graczer, Z. and Hamar, G. and Huba, G. and Kacskovics, B. and Kis, A. and Kovacs, I and Kovacs, R. and Lemperger, I and Levai, P. and Lokos, S. and Mlynarczyk, J. and Molnar, J. and Singh, N. and Novak, A. and Olah, L. and Starecki, T. and Suchenek, M. and Suranyi, G. and Szalai, S. and Tringali, M. C. and Varga, D. and Vasuth, M. and Vasarhelyi, B. and Wesztergom, V and Weber, Z. and Zimboras, Z. and Somlai, L.}, Title = {{Long term measurements from the Matra Gravitational and Geophysical Laboratory}}, Journal = {{EUROPEAN PHYSICAL JOURNAL-SPECIAL TOPICS}}, Year = {{2019}}, Volume = {{228}}, Number = {{8}}, Pages = {{1693-1743}}, Month = {{SEP}}, Abstract = {{The Summary of the long term data taking, related to one of the proposed next generation ground-based gravitational detector's location is presented here. Results of seismic and infrasound noise, electromagnetic attenuation and cosmic muon radiation measurements are reported in the underground Matra Gravitational and Geophysical Laboratory near Gyongyosoroszi, Hungary. The collected seismic data of more than two years is evaluated from the point of view of the Einstein Telescope, a proposed third generation underground gravitational wave observatory. Applying our results for the site selection will significantly improve the signal to noise ratio of the multi-messenger astrophysics era, especially at the low frequency regime.}}, DOI = {{10.1140/epjst/e2019-900153-1}}, ISSN = {{1951-6355}}, EISSN = {{1951-6401}}, ResearcherID-Numbers = {{Weber, Zoltan/A-7375-2009 Kovacs, Robert/P-8911-2015 Kovacs, Istvan/A-1267-2008 Denys, Mateusz/I-6417-2018 Kovacs, Istvan/AAB-6187-2020 Van, Peter/F-8579-2010 Barnafoldi, Gergely Gabor/AAB-5738-2021 Bulik, Tomasz/AAJ-6742-2020 Vasarhelyi, Balazs/G-9270-2011 Fenyvesi, Edit/B-9076-2018 Lokos, Sandor/A-4798-2019 }}, ORCID-Numbers = {{Weber, Zoltan/0000-0002-0017-3505 Kovacs, Robert/0000-0001-5822-6035 Kovacs, Istvan/0000-0002-3488-3716 Denys, Mateusz/0000-0003-4837-9649 Van, Peter/0000-0002-9396-4073 Barnafoldi, Gergely Gabor/0000-0001-9223-6480 Fenyvesi, Edit/0000-0003-2777-3719 Lokos, Sandor/0000-0002-4447-4836 Rosinska, Dorota/0000-0002-3681-9304 Bulik, Tomasz/0000-0003-2045-4803 Tringali, Maria Concetta/0000-0001-5087-189X Starecki, Tomasz/0000-0002-4730-6803}}, Unique-ID = {{ISI:000489062100001}}, } @article{ ISI:000483694100002, Author = {Wang, Yu-Tong and Zhang, Jun and Zhou, Shuang-Yong and Piao, Yun-Song}, Title = {{On echo intervals in gravitational wave echo analysis}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2019}}, Volume = {{79}}, Number = {{9}}, Month = {{SEP}}, Abstract = {{Gravitational wave echoes, if they exist, could encode important information of new physics from the strong gravity regime. Current echo searches usually assume constant interval echoes (CIEs) a priori, although unequal interval echoes (UIEs) are also possible. Despite of its simplicity, the using of CIE templates need to be properly justified, especially given the high sensitivity of future gravitational wave detectors. In this paper, we assess the necessity of UIE templates in echo searches. By reconstructing injected UIE signals with both CIE and UIE templates, we show that the CIE template may significantly misinterpret the echo signals if the variation of the interval is greater than the statistical errors of the interval, which is further confirmed by a Bayesian analysis on model stelection. We also forecast the constraints on the echo intervals given by future GW detectors such as Advanced LIGO and Einstein Telescope.}}, DOI = {{10.1140/epjc/s10052-019-7234-1}}, Article-Number = {{726}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, Unique-ID = {{ISI:000483694100002}}, } @article{ ISI:000482450500004, Author = {Du, Minghui and Yang, WebJiang and Xu, Lixin and Pan, Supriya and Mota, David F.}, Title = {{Future constraints on dynamical dark-energy using gravitational-wave standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{4}}, Month = {{AUG 23}}, Abstract = {{The detection of gravitational waves (GW) by the LIGO and Virgo collaborations offers a whole new range of possible tests and opens up a new window that may shed light on the nature of dark energy and dark matter. In the present work we investigate how future gravitational-wave data could help to constrain different dynamical dark energy models. In particular, we perform cosmological forecastings of a class of well-known and most used dynamical dark energy models using the third-generation gravitational wave detector, the Einstein Telescope. We have considered 1000 simulated GW events in order to constrain the parameter space of the dynamical dark energy models. Our analyses show that the inclusion of the GW data from the Einstein Telescope significantly improves the parameter space of the dynamical dark energy models compared to their constraints extracted from the standard cosmological probes, namely, the cosmic microwave observations, baryon acoustic oscillations distance measurements, supernove type Ia, and the Hubble parameter measurements.}}, DOI = {{10.1103/PhysRevD.100.043535}}, Article-Number = {{043535}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000482450500004}}, } @article{ ISI:000482214500006, Author = {D'Agostino, Rocco and Nunes, Rafael C.}, Title = {{Probing observational bounds on scalar-tensor theories from standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{4}}, Month = {{AUG 22}}, Abstract = {{Standard sirens are the gravitational wave (GW) analog of the astronomical standard candles and can provide powerful information about the dynamics of the Universe. In this work, we simulate a catalog with 1000 standard siren events from binary neutron star mergers, within the sensitivity predicted for the third generation of the ground GW detector called the Einstein Telescope (ET). After correctly modifying the propagation of GWs as input to generate the catalog, we apply our mock dataset on scalar-tensor theories where the speed of GW propagation is equal to the speed of light. As a first application, we find new observational bounds on the running of the Planck mass, when considering appropriate values within the stability condition of the theory, and we discuss some consequences on the amplitude of the running of the Planck mass. In the second part, we combine our simulated standard sirens catalog with other geometric cosmological tests (supernovae la and cosmic chronometer measurements) to constrain the Hu-Sawicki f (R) gravity model. We thus find new and non-null deviations from the standard ACDM model, showing that in the future f (R) gravity can be tested up to 95\% confidence level. The results obtained here show that the statistical accuracy achievable by future ground-based GW observations, mainly with the ET detector (and planned detectors with a similar sensitivity), can provide strong observational bounds on modified gravity theories.}}, DOI = {{10.1103/PhysRevD.100.044041}}, Article-Number = {{044041}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{D'Agostino, Rocco/0000-0003-2342-1134 nunes, rafael/0000-0002-8432-5616}}, Unique-ID = {{ISI:000482214500006}}, } @article{ ISI:000482600400001, Author = {Boco, L. and Lapi, A. and Goswami, S. and Perrotta, F. and Baccigalupi, C. and Danese, L.}, Title = {{Merging Rates of Compact Binaries in Galaxies: Perspectives for Gravitational Wave Detections}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2019}}, Volume = {{881}}, Number = {{2}}, Month = {{AUG 20}}, Abstract = {{We investigate the merging rates of compact binaries in galaxies and the related detection rate of gravitational wave (GW) events with AdvLIGO/Virgo and with the Einstein Telescope. To this purpose, we rely on three basic ingredients: (i) the redshift-dependent galaxy statistics provided by the latest determination of the star formation rate functions from UV-Pfar-IRAsub)millimeter/radio data; (ii) star formation and chemical enrichment histories for individual galaxies, modeled on the basis of observations; and (iii) compact remnant mass distribution and prescriptions for merging of compact binaries from stellar evolution simulations. We present results for the intrinsic birth rate of compact remnants, the merging rates of compact binaries, GW detection rates, and GW counts, attempting to differentiate the outcomes among black hole-black hole, neutron star-neutron star, and black hole-neutron star mergers and to estimate their occurrence in disk and spheroidal host galaxies. We compare our approach with the one based on cosmic star formation rate density and cosmic metallicity, exploited by many literature studies; the merging rates from the two approaches are in agreement within the overall astrophysical uncertainties. We also investigate the effects of galaxy-scale strong gravitational lensing of GW in enhancing the rate of detectable events toward high redshift. Finally, we discuss the contribution of undetected GW emission from compact binary mergers to the stochastic background.}}, DOI = {{10.3847/1538-4357/ab328e}}, Article-Number = {{157}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, Unique-ID = {{ISI:000482600400001}}, } @article{ ISI:000482550700001, Author = {Song, Hao-Ran and Ai, Shun-Ke and Wang, Min-Hao and Xing, Nan and Gao, He and Zhang, Bing}, Title = {{Viewing Angle Constraints on S190425z and S190426c and the Joint Gravitational-wave/Gamma-Ray Detection Fractions for Binary Neutron Star Mergers}}, Journal = {{ASTROPHYSICAL JOURNAL LETTERS}}, Year = {{2019}}, Volume = {{881}}, Number = {{2}}, Month = {{AUG 20}}, Abstract = {{The Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo scientific collaboration (LVC) detected two binary neutron star (BNS) merger candidates, S190425z and S190426c. The Fermi-Gamma-ray Burst Monitor (GBM) observed 55.6\% (for S190425z) and 100\% (for S190426c) of the probability regions of both events at the respective merger times, but no gamma-ray burst (GRB) was detected in either case. The derived luminosity upper limits suggest that a short GRB similar to GRB 170817A would not be detectable for both cases due to their distances, which are larger than that of GW170817. Assuming that the jet profile obtained from GW170817/GRB 170817A is quasi-universal for all BNS-GRB associations, we derive that the viewing angles of S190425z and S190426c should be >(0.11-0.41) and >(0.09-0.39), respectively. Through Monte Carlo simulations, we show that with the GRB 170817A-like jet structure, all sky gamma-ray detectors, such as GBM and the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor, are expected to detect similar to 4.6\%, 3.9\%, 1.7\%, and 6.6\%, 5.7\%, 2.8\% of BNS mergers triggered by advanced LIGO, A+, and the Einstein Telescope, respectively. The joint detection fraction would be largely reduced for Swift-BAT, SVOM-ECLAIRS, and the Einstein Probe, whose sensitivities are better but whose FOVs are smaller.}}, DOI = {{10.3847/2041-8213/ab3921}}, Article-Number = {{L40}}, ISSN = {{2041-8205}}, EISSN = {{2041-8213}}, ResearcherID-Numbers = {{Zhang, Bing/AAG-2824-2019}}, Unique-ID = {{ISI:000482550700001}}, } @article{ ISI:000481821000001, Author = {Takeda, Hiroki and Nishizawa, Atsushi and Nagano, Koji and Michimura, Yuta and Komori, Kentaro and Ando, Masaki and Hayama, Kazuhiro}, Title = {{Prospects for gravitational-wave polarization tests from compact binary mergers with future ground-based detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{100}}, Number = {{4}}, Month = {{AUG 20}}, Abstract = {{There exist six possible polarization modes of gravitational waves in a general metric theory of gravity, while two tensor polarization modes are allowed in general relativity. The properties and number of polarization modes depend on gravity theories. For transient signals, the number of the detectors needs to be basically equal to the number of the gravitational-wave polarization modes for separation of polarizations. However, a single detector having great sensitivity at lower frequency could be effectively regarded as a virtual detector network including a set of detectors along its trajectory due to a long gravitational-wave signal from a compact binary and the Earth's rotation. Thus, time-varying antenna pattern functions can help test the polarizations of gravitational waves. We study the effects of the Earth's rotation on the polarization test and show a possibility to test the nontensorial polarization modes from future observations of compact binary mergers with ground-based gravitational detectors such as Einstein telescope and Cosmic Explorer.}}, DOI = {{10.1103/PhysRevD.100.042001}}, Article-Number = {{042001}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{ANDO, MASAKI/G-4989-2014}}, ORCID-Numbers = {{ANDO, MASAKI/0000-0002-8865-9998}}, Unique-ID = {{ISI:000481821000001}}, } @article{ ISI:000480385200001, Author = {Cao, Shuo and Qi, Jingzhao and Cao, Zhoujian and Biesiada, Marek and Li, Jin and Pan, Yu and Zhu, Zong-Hong}, Title = {{Direct test of the FLRW metric from strongly lensed gravitational wave observations}}, Journal = {{SCIENTIFIC REPORTS}}, Year = {{2019}}, Volume = {{9}}, Month = {{AUG 12}}, Abstract = {{The assumptions of large-scale homogeneity and isotropy underly the familiar Friedmann-Lemaitre-Robertson-Walker (FLRW) metric that appears to be an accurate description of our Universe. In this paper, we propose a new strategy of testing the validity of the FLRW metric, based on the galactic-scale lensing systems where strongly lensed gravitational waves and their electromagnetic counterparts can be simultaneously detected. Each strong lensing system creates opportunity to infer the curvature parameter of the Universe. Consequently, combined analysis of many such systems will provide a model-independent tool to test the validity of the FLRW metric. Our study demonstrates that the third-generation ground based GW detectors, like the Einstein Telescope (ET) and space-based detectors, like the Big Bang Observer (BBO), are promising concerning determination of the curvature parameter or possible detection of deviation from the FLRW metric. Such accurate measurements of the FLRW metric can become a milestone in precision GW cosmology.}}, DOI = {{10.1038/s41598-019-47616-4}}, Article-Number = {{11608}}, ISSN = {{2045-2322}}, ResearcherID-Numbers = {{Cao, Zhoujian/AAH-2470-2020 Qi, JingZhao/AAC-9594-2020 Biesiada, Marek/ABC-3364-2020}}, ORCID-Numbers = {{Cao, Zhoujian/0000-0002-1932-7295 Biesiada, Marek/0000-0003-1308-7304}}, Unique-ID = {{ISI:000480385200001}}, } @article{ ISI:000600560300001, Author = {Steinlechner, Jessica and Martin, Iain W.}, Title = {{Thermal noise from icy mirrors in gravitational wave detectors}}, Journal = {{PHYSICAL REVIEW RESEARCH}}, Year = {{2019}}, Volume = {{1}}, Number = {{1}}, Month = {{AUG 12}}, Abstract = {{The detection of gravitational waves has established a new and very exciting field of astronomy in the past few years. To increase the number of detections and allow observation of a wider range of sources, several future gravitational wave detectors will operate at cryogenic temperatures. Recent investigations of a mirror in one of the cryostats of the Japanese KAGRA detector showed a decrease in reflectivity due to ice growth, induced by residual water molecules moving from the warm to the cold sections of the detector's vacuum system. Based on the optical measurements made in KAGRA, in this paper we calculate the implications of an ice layer on coating thermal noise for the planned European Einstein Telescope. We find coating thermal noise to oscillate, due to periodic reflectivity changes as the ice layer grows. The average coating thermal noise increases significantly over a time of one year with a larger increase at higher temperatures.}}, DOI = {{10.1103/PhysRevResearch.1.013008}}, Article-Number = {{013008}}, EISSN = {{2643-1564}}, ORCID-Numbers = {{Steinlechner, Jessica/0000-0002-6697-9026}}, Unique-ID = {{ISI:000600560300001}}, } @article{ ISI:000481698100001, Author = {Belgacem, Enis and Dirian, Yves and Foffa, Stefano and Howell, Eric J. and Maggiore, Michele and Regimbau, Tania}, Title = {{Cosmology and dark energy from joint gravitational wave-GRB observations}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2019}}, Number = {{8}}, Month = {{AUG}}, Abstract = {{Gravitational-wave (GW) detectors can contribute to the measurement of cosmological parameters and to testing the dark-energy sector of alternatives to ACDM, by using standard sirens. In this paper we focus on binary neutron stars with a counterpart detected through a gamma-ray burst (GRB), both at a second-generation network made by advanced LIGO+advanced Virgo+LIGO India+Kagra, and at third-generation (3G) detectors, discussing in particular the cases of a single Einstein Telescope (ET), and of a network of ET plus two Cosmic Explorer (CE). We construct mock catalogs of standard sirens, using different scenarios for the local merger rate and for the detection of the electromagnetic counterpart. For 3G detectors we estimate the coincidences with a GRB detector with the characteristics of the proposed THESEUS mission. We discuss how these standard sirens with a GRB counterpart can improve the determination of cosmological parameters (and particularly of H-0) in ACDM, and we then study how to extract information on dark energy, considering both a non-trivial dark energy equation of state and modified GW propagation. We find that a 2G detector network can already reach, over several years of data taking, an interesting sensitivity to modified GW propagation, while a single ET detector would have a remarkable potential for discovery. We also find that, to fully exploit the potential of a Gravitational-wave (GW) detectors can contribute to the measurement of cosmological parameters and to testing the dark-energy sector of alternatives to ACDM, by using standard sirens. In this paper we focus on binary neutron stars with a counterpart detected through a gamma-ray burst (GRB), both at a second-generation network made by advanced LIGO+advanced Virgo+LIGO India+Kagra, and at third-generation (3G) detectors, discussing in particular the cases of a single Einstein Telescope (ET), and of a network of ET plus two Cosmic Explorer (CE). We construct mock catalogs of standard sirens, using different scenarios for the local merger rate and for the detection of the electromagnetic counterpart. For 3G detectors we estimate the coincidences with a GRB detector with the characteristics of the proposed THESEUS mission. We discuss how these standard sirens with a GRB counterpart can improve the determination of cosmological parameters (and particularly of Ho) in ACDM, and we then study how to extract information on dark energy, considering both a non-trivial dark energy equation of state and modified GW propagation. We find that a 2G detector network can already reach, over several years of data taking, an interesting sensitivity to modified GW propagation, while a single ET detector would have a remarkable potential for discovery. We also find that, to fully exploit the potential of a ET+CE+CE network, it is necessary a much stronger program of search for electromagnetic counterparts (or else to resort to statistical methods for standard sirens), and furthermore gravitational lensing can become a limiting factor.}}, DOI = {{10.1088/1475-7516/2019/08/015}}, Article-Number = {{015}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Howell, Eric/H-5072-2014 }}, ORCID-Numbers = {{Howell, Eric/0000-0001-7891-2817 Maggiore, Michele/0000-0001-7348-047X}}, Unique-ID = {{ISI:000481698100001}}, } @article{ ISI:000474919700036, Author = {Liu, Bin and Li, Zhengxiang and Zhu, Zong-Hong}, Title = {{Complementary constraints on dark energy equation of state from strongly lensed gravitational wave}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2019}}, Volume = {{487}}, Number = {{2}}, Pages = {{1980-1985}}, Month = {{AUG}}, Abstract = {{It has been shown that time delay of strong gravitational lensing is not only an effective cosmological probe to constrain the Hubble constant, the matter density, and the curvature of the universe but also useful for breaking the degeneracy of the dark energy equation of state and thus provide complementarity with other popular probes, such as Type Ia supernovae, baryon acoustic oscillations, and cosmic microwave background radiation. Interestingly, compared to traditional strong lensing systems where quasars act as sources, strongly lensed gravitational waves (GWs) from compact binary coalescence and their electromagnetic (EM) counterpart systems have been recently proposed to be more powerful for studying cosmology since GWs and their EM counterparts are transients. Short durations of GWs and their EM counterparts are very advantageous to time delay measurement and lens profile modelling. Here, in the framework of Chevalier-Polarski-Linder parametrization, we investigate improvement of constraining power on the dark energy equation of state due to including time delay measurements of strong lensed GW systems. It is suggested that, on the basis of the third generation ground-based detector, e.g. the Einstein Telescope, adding time delay of only 30 strong lensed GW systems to Type Ia supernovae and cosmic microwave background radiation can improve the dark energy figure of merit by a factor of 2. For the traditional standard siren method where the uncertainties of luminosity distances of GWs are similar to 10 per cent, a few x 10(4) events are expected to present similar constraints. In the precision cosmology era, this progress is of great significance for studying the nature of dark energy.}}, DOI = {{10.1093/mnras/stz1179}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, Unique-ID = {{ISI:000474919700036}}, } @article{ ISI:000472944000002, Author = {Badaracco, F. and Harms, J.}, Title = {{Optimization of seismometer arrays for the cancellation of Newtonian noise from seismic body waves}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2019}}, Volume = {{36}}, Number = {{14}}, Month = {{JUL 25}}, Abstract = {{Newtonian noise (NN) from seismic fields is predicted to become a sensitivity limiting noise contribution of the gravitational-wave detectors Advanced LIGO and Virgo in the next few years. It also plays a major role in the planning of next-generation detectors, which might be constructed underground as planned for the Einstein telescope (ET) mostly to suppress NN. Coherent noise cancellation using Wiener filters provides a way to mitigate NN. So far, only the cancellation of NN produced by seismic surface waves has been studied in detail due to its relevance for Advanced LIGO and Virgo. However, seismic body waves can still contribute significantly to NN in surface detectors, and they might be the dominant source of gravity fluctuations in underground detectors. In this paper, we present the first detailed analysis of coherent cancellation of NN from body waves. While the required number of seismometers to achieve a certain level of noise suppression is higher than for seismic surface waves, we show that optimal seismometer arrays can greatly reduce body-wave NN. The optimal array configurations and achieved residuals depend strongly on the composition of the seismic field in terms of average compressional-wave and shear-wave content. We propose Newtonian-noise cancellation to achieve the ambitious low-frequency target of the ET.}}, DOI = {{10.1088/1361-6382/ab28c1}}, Article-Number = {{145006}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Harms, Jan/J-4359-2012}}, ORCID-Numbers = {{Badaracco, Francesca/0000-0001-8553-7904 Harms, Jan/0000-0002-7332-9806}}, Unique-ID = {{ISI:000472944000002}}, } @article{ ISI:000476907600001, Author = {Yang, Weiqiang and Vagnozzi, Sunny and Di Valentino, Eleonora and Nunes, Rafael C. and Pang, Supriya and Mota, David F.}, Title = {{Listening to the sound of dark sector interactions with gravitational wave standard sirens}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2019}}, Number = {{7}}, Month = {{JUL}}, Abstract = {{We consider two stable Interacting Dark Matter-Dark Energy models and confront them against current Cosmic Microwave Background data from the Planck satellite. We then generate luminosity distance measurements from O(10(3)) mock Gravitational Wave events matching the expected sensitivity of the proposed Einstein Telescope. We use these to forecast how the addition of Gravitational Wave standard sirens data can improve current limits on the Dark Matter-Dark Energy coupling strength (xi). We find that the addition of Gravitational Waves data can reduce the current uncertainty by a factor of 5. Moreover, if the underlying cosmological model truly features Dark Matter-Dark Energy interactions with a value of xi within the currently allowed 1 sigma upper limit, the addition of Gravitational Wave data would help disentangle such an interaction from the standard case of no interaction at a significance of more than 3 sigma.}}, DOI = {{10.1088/1475-7516/2019/07/037}}, Article-Number = {{037}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Vagnozzi, Sunny/W-7331-2019 Di Valentino, Eleonora/AAX-6486-2020 }}, ORCID-Numbers = {{Vagnozzi, Sunny/0000-0002-7614-6677 Di Valentino, Eleonora/0000-0001-8408-6961 nunes, rafael/0000-0002-8432-5616}}, Unique-ID = {{ISI:000476907600001}}, } @article{ ISI:000474907100090, Author = {Powell, Jade and Muller, Bernhard}, Title = {{Gravitational wave emission from 3D explosion models of core-collapse supernovae with low and normal explosion energies}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2019}}, Volume = {{487}}, Number = {{1}}, Pages = {{1178-1190}}, Month = {{JUL}}, Abstract = {{Understanding gravitational wave emission from core-collapse supernovae will be essential for their detection with current and future gravitational wave detectors. This requires a sample of waveforms from modern 3D supernova simulations reaching well into the explosion phase, where gravitational wave emission is expected to peak. However, recent waveforms from 3D simulations with multigroup neutrino transport do not reach far into the explosion phase, and some are still obtained from non-exploding models. We therefore calculate waveforms up to 0.9 s after bounce using the neutrino hydrodynamics code COCONUT-FMT. We consider two models with low and normal explosion energy, namely explosions of an ultra-stripped progenitor with an initial helium star mass of 3.5 M-circle dot, and of an 18 M-circle dot single star. Both models show gravitational wave emission from the excitation of surface g modes in the proto-neutron star with frequencies between similar to 800 and 1000 Hz at peak emission. The peak amplitudes are about 6 and 10 cm, respectively, which is somewhat higher than in most recent 3D models of the pre-explosion or early explosion phase. Using a Bayesian analysis, we determine the maximum detection distances for our models in simulated Advanced LIGO, Advanced Virgo, and Einstein Telescope (ET) design sensitivity noise. The more energetic 18 M-circle dot explosion will be detectable to about 17.5 kpc by the LIGO/Virgo network and to about 180 kpc with the ET.}}, DOI = {{10.1093/mnras/stz1304}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Mueller, Bernhard/0000-0002-4470-1277 Powell, Jade/0000-0002-1357-4164}}, Unique-ID = {{ISI:000474907100090}}, } @article{ ISI:000472129800014, Author = {Zhao, Zhi-Chao and Lin, Hai-Nan and Chang, Zhe}, Title = {{The prospects of using gravitational waves for constraining the anisotropy of the Universe}}, Journal = {{CHINESE PHYSICS C}}, Year = {{2019}}, Volume = {{43}}, Number = {{7}}, Month = {{JUL}}, Abstract = {{The observation of GW150914 gave a new independent measurement of the luminosity distance of a gravitational wave event. In this paper, we constrain the anisotropy of the Universe by using gravitational wave events. We simulate hundreds of events of binary neutron star merger that may be observed by the Einstein Telescope. Full simulation of the production process of gravitational wave data is employed. We find that 200 binary neutron star merging events with the redshift in (0,1) observed by the Einstein Telescope may constrain the anisotropy with an accuracy comparable to that from the Union2.1 supernovae. This result shows that gravitational waves can be a powerful tool for investigating cosmological anisotropy.}}, DOI = {{10.1088/1674-1137/43/7/075102}}, Article-Number = {{075102}}, ISSN = {{1674-1137}}, EISSN = {{2058-6132}}, ORCID-Numbers = {{Chang, Zhe/0000-0002-9720-803X}}, Unique-ID = {{ISI:000472129800014}}, } @article{ ISI:000471988600002, Author = {Craig, Kieran and Steinlechner, Jessica and Murray, Peter G. and Bell, Angus S. and Birney, Ross and Haughian, Karen and Hough, Jim and MacLaren, Ian and Penn, Steve and Reid, Stuart and Robie, Raymond and Rowan, Sheila and Martin, Iain W.}, Title = {{Mirror Coating Solution for the Cryogenic Einstein Telescope}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2019}}, Volume = {{122}}, Number = {{23}}, Month = {{JUN 13}}, Abstract = {{Planned cryogenic gravitational-wave detectors will require improved coatings with a strain thermal noise reduced by a factor of 25 compared to Advanced LIGO. We present investigations of HfO2 doped with SiO(2 )as a new coating material for future detectors. Our measurements show an extinction coefficient of k = 6 x 10(-6) and a mechanical loss of phi = 3.8 x 10(-4) at 10 K, which is a factor of 2 below that of SiO2, the currently used low refractive-index coating material. These properties make HfO2 doped with SiO2 ideally suited as a low-index partner material for use with a-Si in the lower part of a multimaterial coating. Based on these results, we present a multimaterial coating design which, for the first time, can simultaneously meet the strict requirements on optical absorption and thermal noise of the cryogenic Einstein Telescope.}}, DOI = {{10.1103/PhysRevLett.122.231102}}, Article-Number = {{231102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{MacLaren, Ian/C-1773-2010 }}, ORCID-Numbers = {{MacLaren, Ian/0000-0002-5334-3010 Steinlechner, Jessica/0000-0002-6697-9026 Birney, Ross/0000-0002-4766-0757}}, Unique-ID = {{ISI:000471988600002}}, } @article{ ISI:000470889300002, Author = {Safarzadeh, Mohammadtaher and Berger, Edo and Ng, Ken K. Y. and Chen, Hsin-Yu and Vitale, Salvatore and Whittle, Chris and Scannapieco, Evan}, Title = {{Measuring the Delay Time Distribution of Binary Neutron Stars. II. Using the Redshift Distribution from Third-generation Gravitational-wave Detectors Network}}, Journal = {{ASTROPHYSICAL JOURNAL LETTERS}}, Year = {{2019}}, Volume = {{878}}, Number = {{1}}, Month = {{JUN 10}}, Abstract = {{We investigate the ability of current and third-generation gravitational wave (GW) detectors to determine the delay time distribution (DTD) of binary neutron stars (BNSs) through a direct measurement of the BNS merger rate as a function of redshift. We assume that the DTD follows a power-law distribution with a slope Gamma and a minimum merger time t(min), and also allow the overall BNS formation efficiency per unit stellar mass to vary. By convolving the DTD and mass efficiency with the cosmic star formation history, and then with the GW detector capabilities, we explore two relevant regimes. First, for the current generation of GW detectors, which are only sensitive to the local universe but can lead to precise redshift determinations via the identification of electromagnetic counterparts and host galaxies, we show that the DTD parameters are strongly degenerate with the unknown mass efficiency and therefore cannot be determined uniquely. Second, for third-generation detectors such as Einstein Telescope and Cosmic Explorer, which will detect BNS mergers at cosmological distances but with a redshift uncertainty inherent to GW-only detections (delta(z) /z approximate to 0.1z), we show that the DTD and mass efficiency can be well constrained to better than 10\% with a year of observations. This long-term approach to determining the DTD through a direct mapping of the BNS merger redshift distribution will be supplemented by more near-term studies of the DTD through the properties of BNS merger host galaxies at z approximate to 0.}}, DOI = {{10.3847/2041-8213/ab22be}}, Article-Number = {{L13}}, ISSN = {{2041-8205}}, EISSN = {{2041-8213}}, ORCID-Numbers = {{Safarzadeh, Mohammadtaher/0000-0002-1827-7011 Chen, Hsin-Yu/0000-0001-5403-3762 Vitale, Salvatore/0000-0003-2700-0767 Ng, Ken K. Y./0000-0003-3896-2259}}, Unique-ID = {{ISI:000470889300002}}, } @article{ ISI:000470262600009, Author = {Somlai, L. Abel and Graczer, Zoltan and Levai, P. and Vasuth, M. and Weber, Z. and Van, P.}, Title = {{Seismic noise measures for underground gravitational wave detectors}}, Journal = {{ACTA GEODAETICA ET GEOPHYSICA}}, Year = {{2019}}, Volume = {{54}}, Number = {{2}}, Pages = {{301-313}}, Month = {{JUN}}, Abstract = {{The site characterisation of future underground gravitational wave detectors is based on spectral properties of the low frequency seismic noise. The evaluation of the collected long term seismological data in the Matra Gravitational and Geophysical Laboratory revealed some aspects that are not apparent in short term spectral noise characterisation. In this paper we survey the methodology. In particular, we argue that the spectral properties are best represented by percentiles of the data instead of the mode, because it is noisy, sensitive to the discretization and intrinsic averaging, therefore it is less suitable for a robust characterisation. The suitable cumulative measures are also scrutinized.}}, DOI = {{10.1007/s40328-019-00257-5}}, ISSN = {{2213-5812}}, EISSN = {{2213-5820}}, ResearcherID-Numbers = {{Van, Peter/F-8579-2010 Weber, Zoltan/A-7375-2009}}, ORCID-Numbers = {{Van, Peter/0000-0002-9396-4073 Weber, Zoltan/0000-0002-0017-3505}}, Unique-ID = {{ISI:000470262600009}}, } @article{ ISI:000470860900002, Author = {Martynov, Denis and Miao, Haixing and Yang, Huan and Vivanco, Francisco Hernandez and Thrane, Eric and Smith, Rory and Lasky, Paul and East, William E. and Adhikari, Rana and Bauswein, Andreas and Brooks, Aidan and Chen, Yanbei and Corbitt, Thomas and Freise, Andreas and Grote, Hartmut and Levin, Yuri and Zhao, Chunnong and Vecchio, Alberto}, Title = {{Exploring the sensitivity of gravitational wave detectors to neutron star physics}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{10}}, Month = {{MAY 31}}, Abstract = {{The physics of neutron stars can be studied with gravitational waves emitted from coalescing binary systems. Tidal effects become significant during the last few orbits and can be visible in the gravitational wave spectrum above 500 Hz. After the merger, the neutron star remnant oscillates at frequencies above 1 kHz and can collapse into a black hole. Gravitational wave detectors with a sensitivity of similar or equal to 10(-24) strain/root Hz at 2-4 kHz can observe these oscillations from a source which is approximately 100 Mpc away. The current observatories, such as LIGO and Virgo, are limited by shot noise at high frequencies and have a sensitivity of greater than or equal to 2 x 10(-23) strain/root Hz at 3 kHz. In this paper, we propose an optical configuration of gravitational wave detectors, which can be set up in present facilities using the current interferometer topology. This scheme has the potential to reach 7 x 10(-25) strain/root Hz at 2.5 kHz without compromising the detector sensitivity to black hole binaries. We argue that the proposed instruments have the potential to detect similar amount of postmerger neutron star oscillations as the next generation detectors, such as Cosmic Explorer and Einstein Telescope. We also optimize the arm length of the future detectors for neutron star physics and find that the optimal arm length is approximate to 20 km. These instruments have the potential to observe neutron star postmerger oscillations at a rate of approximately 30 events per year with a signal-to-noise ratio of 5 or more.}}, DOI = {{10.1103/PhysRevD.99.102004}}, Article-Number = {{102004}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Brooks, Aidan/U-5988-2017 Zhao, Chunnong/C-2403-2013 vecchio, alberto/F-8310-2015 }}, ORCID-Numbers = {{Brooks, Aidan/0000-0003-4295-792X Denis, Martynov/0000-0003-0679-1344 Hernandez Vivanco, Francisco/0000-0002-1942-7608 Thrane, Eric/0000-0002-4418-3895 vecchio, alberto/0000-0002-6254-1617 Miao, Haixing/0000-0003-2879-5821 Smith, Rory/0000-0001-8516-3324}}, Unique-ID = {{ISI:000470860900002}}, } @article{ ISI:000469460900001, Author = {Baldes, Iason and Garcia-Cely, Camilo}, Title = {{Strong gravitational radiation from a simple dark matter model}}, Journal = {{JOURNAL OF HIGH ENERGY PHYSICS}}, Year = {{2019}}, Number = {{5}}, Month = {{MAY 28}}, Abstract = {{A rather minimal possibility is that dark matter consists of the gauge bosons of a spontaneously broken symmetry. Here we explore the possibility of detecting the gravitational waves produced by the phase transition associated with such breaking. Concretely, we focus on the scenario based on an SU(2)(D) group and argue that it is a case study for the sensitivity of future gravitational wave observatories to phase transitions associated with dark matter. This is because there are few parameters and those fixing the relic density also determine the effective potential establishing the strength of the phase transition. Particularly promising for LISA and even the Einstein Telescope is the super-cool dark matter regime, with DM masses above O(100) TeV, for which we find that the gravitational wave signal is notably strong. In our analysis, we include the effect of astrophysical foregrounds, which are often ignored in the context of phase transitions.}}, DOI = {{10.1007/JHEP05(2019)190}}, Article-Number = {{190}}, ISSN = {{1029-8479}}, ResearcherID-Numbers = {{Garcia-Cely, Camilo/AAB-7855-2021 }}, ORCID-Numbers = {{Baldes, Iason/0000-0002-8875-6739 Garcia Cely, Camilo Alfredo/0000-0003-3093-7825}}, Unique-ID = {{ISI:000469460900001}}, } @article{ ISI:000468511900003, Author = {de Freitas Pacheco, J. A. and Carneiro, S. and Fabris, J. C.}, Title = {{Gravitational waves from binary axionic black holes}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2019}}, Volume = {{79}}, Number = {{5}}, Month = {{MAY 20}}, Abstract = {{In a recent paper we have shown that a minimally coupled, self-interacting scalar field of mass m can form black holes of mass M=/(4m) (in Planck units). If dark matter is composed by axions, they can form miniclusters that for QCD axions have masses below this value. In this work it is shown that for a scenario in which the axion mass depends on the temperature as mT-6, minicluster masses above 0.32M, corresponding to an axion mass of 3x10-10 eV, exceed M and can collapse into black holes. If a fraction of these black holes is in binary systems, gravitational waves emitted during the inspiral phase could be detected by advanced interferometers like LIGO or VIRGO and by the planned Einstein Telescope. For a detection rate of one event per year, the lower limits on the binary fraction are 10-4 and 10-6 for LIGO and Einstein Telescope respectively.}}, DOI = {{10.1140/epjc/s10052-019-6940-z}}, Article-Number = {{426}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ResearcherID-Numbers = {{Carneiro, Saulo/N-1397-2014}}, ORCID-Numbers = {{Carneiro, Saulo/0000-0001-7098-383X}}, Unique-ID = {{ISI:000468511900003}}, } @article{ ISI:000468222800007, Author = {Nishizawa, Atsushi and Arai, Shun}, Title = {{Generalized framework for testing gravity with gravitational-wave propagation. III. Future prospect}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{10}}, Month = {{MAY 15}}, Abstract = {{The properties of gravitational-wave (GW) propagation are modified in alternative theories of gravity and are crucial observables to test gravity at cosmological distance. The propagation speed has already been measured from GW170817 so precisely and pinned down to the speed of light, while other properties of GW propagation have not constrained tightly yet. In this paper, we investigate the measurement precisions of the amplitude damping rate (equivalently, the time variation of the gravitational coupling for GWs) and graviton mass in the generalized framework of GW propagation with the future detectors such as Voyager, Cosmic Explorer, and Einstein Telescope. As a result, we show that the future GW observation can reach 1\% error for the amplitude damping. We also study the time variation of the gravitational couplings in Horndeski theory by performing Monte Carlo-based numerical simulations. From the simulation results, we find that the current accelerating Universe prefers the models with less damping of GWs and that the equivalence principle can be tested at the level of 1\% by the future GW observation.}}, DOI = {{10.1103/PhysRevD.99.104038}}, Article-Number = {{104038}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000468222800007}}, } @article{ ISI:000466428600006, Author = {Congedo, Giuseppe and Taylor, Andy}, Title = {{Joint cosmological inference of standard sirens and gravitational wave weak lensing}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{8}}, Month = {{APR 30}}, Abstract = {{We present the first joint inference of standard sirens and gravitational wave weak lensing by filtering of the same dataset. We imagine a post-LISA scenario emerging around the late 2030s when LISA will have accumulated a number of detections at high redshift, LIGO-VIRGO will have finished observing at low redshift, and Einstein Telescope will have started making new observations out to redshifts possibly overlapping with LISA. Euclid and other cosmological probes will have provided constraints at the percent level by then, but will have mostly exhausted their ability to improve any further. We derive forecasts assuming similar to 1 deg(-2) detected sources, in conjunction with a spectroscopic follow-up (e.g., by Euclid, DESI, or ATHENA). Thanks to the statistical power of standard sirens as a geometry probe-lifting key degeneracies in the gravitational wave weak lensing-and no external priors assumed, the constraints on dark matter and its clustering, namely Omega(m) and sigma(8), could be achieved to 2\% and 3\%. The Hubble constant could be constrained to better than 1\% in all cases; the dark energy density, Omega(Lambda), to 2\%; the curvature, Omega(K), to 0.02; and the amplitude and spectral tilt of the scalar fluctuations, ln(10(10)A(s)) and n(s), to 2\% and 7\%. As a completely independent cosmological probe, with fewer calibration requirements, the joint inference of standard sirens and gravitational wave weak lensing might help solve the tensions currently observed between other cosmological probes, such as the CMB, galaxy lensing, and type-Ia supernovae, and distinguish between residual systematics and new physics.}}, DOI = {{10.1103/PhysRevD.99.083526}}, Article-Number = {{083526}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Congedo, Giuseppe/H-8587-2015}}, ORCID-Numbers = {{Congedo, Giuseppe/0000-0003-2508-0046}}, Unique-ID = {{ISI:000466428600006}}, } @article{ ISI:000466426300003, Author = {Fu, Xiangyun and Zhou, Lu and Chen, Jun}, Title = {{Testing the cosmic distance-duality relation from future gravitational wave standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{8}}, Month = {{APR 26}}, Abstract = {{A validation of the cosmic distance-duality relation (CDDR) is crucial because any observational departure from it could be a signal of new physics. In this work, we explore the potentialities of luminosity distance data from the gravitational wave (GW) standard sirens of the future Einstein Telescope (ET) to test the CDDR. The angular diameter distance data are used from the galaxy cluster samples and the baryon acoustic oscillation (BAO) measurements. The basic advantage of GW measurement substituting for the observation from the type Ia supernovae (SNIa) is that the luminosity distance from GW is insensitive to the nonconservation of the number of photons. By simulating 550 and 1000 data points of future GW measurements in the low redshift range 0 < z < 1, we show that the measurements of future GW events will be a powerful tool to test the CDDR.}}, DOI = {{10.1103/PhysRevD.99.083523}}, Article-Number = {{083523}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000466426300003}}, } @article{ ISI:000466426300004, Author = {Isi, Maximiliano and Sun, Ling and Brito, Richard and Melatos, Andrew}, Title = {{Directed searches for gravitational waves from ultralight bosons}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{8}}, Month = {{APR 26}}, Abstract = {{Gravitational-wave detectors can be used to search for yet-undiscovered ultralight bosons, including those conjectured to solve problems in particle physics, high-energy theory, and cosmology. In particular, ground-based instruments could probe boson masses between 10(-15) eV and 10(-11) eV, which are largely inaccessible to other experiments. In this paper, we explore the prospect of searching for the continuous gravitational waves generated by boson clouds around known black holes. We carefully study the predicted waveforms and use the latest-available numerical results to model signals for different black-hole and boson parameters. We then demonstrate the suitability of a specific method (hidden Markov model tracking) to efficiently search for such signals, even when the source parameters are not perfectly known as well as allowing for some uncertainty in theoretical predictions. We empirically study this method's sensitivity and computational cost in the context of boson signals, finding that it will be possible to target remnants from compact-binary mergers localized with at least three instruments. For signals from scalar clouds, we also compute detection horizons for future detectors (Advanced LIGO, LIGO Voyager, Cosmic Explorer, and the Einstein Telescope). Among other results, we find that, after one year of observation, an Advanced LIGO detector at design sensitivity could detect these sources up to over 100 Mpc, while Cosmic Explorer could reach over 10(4) Mpc. These projections offer a more complete picture than previous estimates based on analytic approximations to the signal power or idealized search strategies. Finally, we discuss specific implications for the follow-up of compact-binary coalescences and black holes in x-ray binaries. Along the way, we review the basic physics of bosons around black holes, in the hope of providing a bridge between the theory and data-analysis literatures.}}, DOI = {{10.1103/PhysRevD.99.084042}}, Article-Number = {{084042}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Brito, Richard/K-8803-2015}}, ORCID-Numbers = {{Sun, Ling/0000-0001-7959-892X Isi Banales, Maximiliano/0000-0001-8830-8672 Melatos, Andrew/0000-0003-4642-141X Brito, Richard/0000-0002-7807-3053}}, Unique-ID = {{ISI:000466426300004}}, } @article{ ISI:000464746300004, Author = {Liao, Kai}, Title = {{Constraints on cosmic curvature with lensing time delays and gravitational waves}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{8}}, Month = {{APR 16}}, Abstract = {{Assuming the ACDM model, the CMB and BAO observations indicate a very flat Universe. Model-independent measurements are therefore worth studying. Time delays measured in lensed quasars provide the time delay distances. When compared with the luminosity distances from the supernova Ia (SNe Ia) observation, the measurements can provide the curvature information under the Distance Sum Rule of the Friedmann-Lemaitre-Robertson-Walker (FLRW) metric. This method is limited by the low redshifts of SNe Ia. In this work, we propose that gravitational waves from the Einstein Telescope, as standard sirens which reach higher redshifts covering the redshift range of lensed quasars from the Large Synoptic Survey Telescope, could provide much more stringent constraints on the curvature. We first consider a conservative case where only 100 gravitational waves with electromagnetic counterparts are available; the la uncertainty for the curvature parameter Omega(k) is 0.057. In an optimistic case with 1000 signals available, then Omega(k) uncertainty is 0.027. Combining with SNe Ia from the Dark Energy Survey, Omega(k) can be further constrained to 0.027 and 0.018, respectively.}}, DOI = {{10.1103/PhysRevD.99.083514}}, Article-Number = {{083514}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000464746300004}}, } @article{ ISI:000464745200006, Author = {Nunes, Rafael C. and Alves, Marcio E. S. and de Araujo, Jose C. N.}, Title = {{Primordial gravitational waves in Horndeski gravity}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{8}}, Month = {{APR 12}}, Abstract = {{We investigate the propagation of primordial gravitational waves within the context of the Homdeski theories; for this, we present a generalized transfer function quantifying the subhorizon evolution of gravitational wave modes after they enter the horizon. We compare the theoretical prediction of the modified primordial gravitational wave spectral density with the aLIGO, Einstein telescope, LISA, gLISA and DECIGO sensitivity curves. Assuming reasonable and different values for the free parameters of the theory (in agreement with the event GW170817 and stability conditions of the theory), we note that the gravitational wave amplitude can vary significantly in comparison with general relativity. We find that in some cases the gravitational primordial spectrum can cross the sensitivity curves for the DECIGO detector with the maximum frequency sensitivity to the theoretical predictions around 0.05-0.30 Hz. From our results, it is clear that the future generations of space based interferometers can bring new perspectives to probing modifications in general relativity.}}, DOI = {{10.1103/PhysRevD.99.084022}}, Article-Number = {{084022}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Alves, Marcio E.S./AAB-5094-2019 de Araujo, Jose C N/C-5181-2013}}, ORCID-Numbers = {{Alves, Marcio E.S./0000-0002-7063-694X de Araujo, Jose C N/0000-0003-4418-4289}}, Unique-ID = {{ISI:000464745200006}}, } @article{ ISI:000463102400011, Author = {Yang, Lilan and Ding, Xuheng and Biesiada, Marek and Liao, Kai and Zhu, Zong-Hong}, Title = {{How Does the Earth's Rotation Affect Predictions of Gravitational Wave Strong Lensing Rates?}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2019}}, Volume = {{874}}, Number = {{2}}, Month = {{APR 1}}, Abstract = {{The next generation of ground-based gravitational wave (GW) detectors, e.g., the Einstein Telescope, is expected to observe a significant number of strongly lensed GW events as predicted in many previous papers. However, all these works ignored the impact of the Earth's rotation on this prediction. Multiple lensed images arrive at the Earth at different time, thus the ground-based detector has different responses to the lensed images due to different orientations of the detector relative to the GW source direction. Therefore the amplitudes of the GW signal from different images are modulated appropriately, in addition to the lensing magnification. In order to assess this effect, we performed Monte Carlo simulations to calculate the event rate of lensed GW signals. Our conclusion is that the Earth's rotation has a non-negligible impact on the event rate of lensed GW images. The updated event rates decrease by factors of similar to 40\%, similar to 20\%, and similar to 10\%, for NS-NS, BH-NS, and BH-BH systems, respectively.}}, DOI = {{10.3847/1538-4357/ab095c}}, Article-Number = {{139}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Ding, Xuheng/0000-0001-8917-2148 Yang, Lilan/0000-0002-8434-880X}}, Unique-ID = {{ISI:000463102400011}}, } @article{ ISI:000462917900002, Author = {Roma, Vincent and Powell, Jade and Heng, Ik Siong and Frey, Raymond}, Title = {{Astrophysics with core-collapse supernova gravitational wave signals in the next generation of gravitational wave detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{6}}, Month = {{MAR 26}}, Abstract = {{The next generation of gravitational wave detectors will improve the detection prospects for gravitational waves from core-collapse supernovae. The complex astrophysics involved in core-collapse supernovae pose a significant challenge to modeling such phenomena. The Supernova Model Evidence Extractor (SMEE) attempts to capture the main features of gravitational wave signals from core-collapse supernovae by using numerical relativity waveforms to create approximate models. These models can then be used to perform Bayesian model selection to determine if the targeted astrophysical feature is present in the gravitational wave signal. In this paper, we extend SMEE's model selection capabilities to include features in the gravitational wave signal that are associated with g-modes and the standing accretion shock instability. For the first time, we test SMEE's performance using simulated data for planned future detectors, such as the Einstein Telescope, Cosmic Explorer, and LIGO Voyager. Further to this, we show how the performance of SMEE is improved by creating models from the spectrograms of supernova waveforms instead of their time-series waveforms that contain stochastic features. In third generation detector configurations, we find that about 50\% of neutrino-driven simulations were detectable at 100 kpc, and 10\% at 275 kpc. The explosion mechanism was correctly determined for all detected signals.}}, DOI = {{10.1103/PhysRevD.99.063018}}, Article-Number = {{063018}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Powell, Jade/0000-0002-1357-4164}}, Unique-ID = {{ISI:000462917900002}}, } @article{ ISI:000461059700004, Author = {Qi, Jing-Zhao and Cao, Shuo and Zheng, Chenfa and Pan, Yu and Li, Zejun and Li, Jin and Liu, Tonghua}, Title = {{Testing the Etherington distance duality relation at higher redshifts: Combined radio quasar and gravitational wave data}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{6}}, Month = {{MAR 12}}, Abstract = {{In this paper, we analyze the implications of the latest cosmological data sets to test the Etherington distance duality relation (DDR), which connects the luminosity distance D(L )and angular diameter distance D-A at the same redshift. For D-L, we consider the simulated data of gravitational waves from the third-generation gravitational wave detector {[}the Einstein Telescope (ET)], which can be considered as standard candles (or standard siren), while the angular diameter distances D-A are derived from the newly compiled sample of compact radio quasars observed by very-long-baseline interferometry (VLBI), which represents a new type of cosmological standard ruler. Alleviating the absorbtion and scattering effects of dust in the Universe, this will create a valuable opportunity to directly test DDR at much higher precision with the combination of gravitational wave (GW) and electromagnetic (EM) signals. Our results show that, with the combination of the current radio quasar observations, the duality-distance relation can be verified at the precision of 10(-2). Moreover, the Einstein Telescope would produce more robust constraints on the validity of such distance duality relation (at the precision of 10(-3 )), with a larger sample of compact milliarcsecond radio quasars detected in future VLBI surveys.}}, DOI = {{10.1103/PhysRevD.99.063507}}, Article-Number = {{063507}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Qi, JingZhao/AAC-9594-2020}}, Unique-ID = {{ISI:000461059700004}}, } @article{ ISI:000461059700007, Author = {Zhang, Xuan-Neng and Wang, Ling-Feng and Zhang, Jing-Fei and Zhang, Xin}, Title = {{Improving cosmological parameter estimation with the future gravitational-wave standard siren observation from the Einstein Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{6}}, Month = {{MAR 12}}, Abstract = {{Detection of gravitational waves produced by the merger of binary compact objects could provide an independent way for measuring the luminosity distance to the gravitational-wave burst source, indicating that gravitational-wave observation, combined with observation of electromagnetic counterparts, can provide ``standard sirens{''} for investigating the expansion history of the Universe in cosmology. In this work, we wish to investigate how the future gravitational-wave standard siren observations would break the parameter degeneracies existing in the conventional optical observations and how they help improve the parameter estimation in cosmology. We take the third-generation ground-based gravitational-wave detector, the Einstein Telescope, as an example to make an analysis. By simulating 1000 events data in the redshift range between 0 and 5 based on the ten-year observation of the Einstein Telescope, we find that the gravitational-wave data could largely break the degeneracy between the matter density and the Hubble constant, thus significantly improving the cosmological constraints. We further show that the constraint on the equation-of-state parameter of dark energy could also be significantly improved by including the gravitational-wave data in the cosmological fit.}}, DOI = {{10.1103/PhysRevD.99.063510}}, Article-Number = {{063510}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Zhang, Xin/0000-0002-6029-1933}}, Unique-ID = {{ISI:000461059700007}}, } @article{ ISI:000460660600003, Author = {Krishnendu, N. V. and Mishra, Chandra Kant and Arun, K. G.}, Title = {{Spin-induced deformations and tests of binary black hole nature using third-generation detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2019}}, Volume = {{99}}, Number = {{6}}, Month = {{MAR 8}}, Abstract = {{In a recent letter {[}N.V. Krishnendu et al., Phys. Rev. Lett. 119, 091101 (2017)] we explored the possibility of probing the binary black hole nature of coalescing compact binaries, by measuring their spin-induced multipole moments, observed in advanced LIGO detectors. Coefficients characterizing the spin-induced multipole moments of Kerr black holes are predicted by the ``no-hair{''} conjecture and appear in the gravitational waveforms through quadratic and higher order spin interactions and hence can be directly measured from gravitational wave observations. By employing a nonprecessing post-Newtonian (PN) waveform model, we assess the capabilities of the third-generation gravitational wave interferometers such as Cosmic Explorer and Einstein Telescope in carrying out such measurements and use them to test the binary black hole nature of observed binaries. In this paper, we extend the investigations of {[}N.V. Krishnendu et al., Phys. Rev. Lett. 119, 091101 (2017)], limited to measuring the binary's spin-induced quadrupole moment using their observation in second generation detectors, by proposing to measure (a) spin-induced quadrupole effects using third generation detectors, (b) simultaneous measurements of spin-induced quadrupole and octupole effects, again in the context of the third-generation detectors. We study the accuracy of these measurements as a function of total mass, mass ratio, spin magnitudes, and spin alignments. Further, we consider two different binary black hole populations, as proxies of the population that will be observed by the third generation detectors, and obtain the resulting distribution of the spin-induced quadrupole coefficient. This helps us assess how common are those cases where this test would provide very stringent constraints on the black hole nature. These error bars provide us upper limits on the values of the coefficients that characterize the spin-induced multipoles. We find that, using third-generation detectors the symmetric combination of coefficients associated with the spin-induced quadrupole moment of each binary component may be constrained to a value <= 1.1 while a similar combination of coefficients for spin-induced octupole moment may be constrained to <= 2, where both combinations take the value of 1 for a binary black hole system. These estimates suggest that third-generation detectors can accurately constrain the first four multipole moments of the compact objects (mass, spin, quadrupole, and octupole) facilitating a thorough probe of their black hole nature.}}, DOI = {{10.1103/PhysRevD.99.064008}}, Article-Number = {{064008}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000460660600003}}, } @article{ ISI:000460136100005, Author = {Li, Yufeng and Fan, Xilong and Gou, Lijun}, Title = {{Constraining Cosmological Parameters in the FLRW Metric with Lensed GW plus EM Signals}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2019}}, Volume = {{873}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{We proposed a model-independent method to constrain cosmological parameters using the Distance Sum Rule of the Friedmann-Lemaitre-Robertson-Walker metric by combining the time delay distances and the comoving distances through a multi-messenger approach. The time delay distances are measured from lensed gravitational wave. (GW) signals together with their corresponding electromagnetic wave. (EM) counterparts, while the comoving distances are obtained from a parameterized fitting approach with independent supernova observations. With a series of simulations based on the Einstein Telescope, Large Synoptic Survey Telescope, and The Dark Energy Survey, we find that only 10 lensed GW+EM systems can achieve the constraining power comparable to and even stronger than 300 lensed quasar systems due to the more precise time delay from lensed GW signals. Specifically, the cosmological parameters can be constrained to k = 0.01(-0.05)(+0.05) and H-0 = 69.7(-0.35)(+0.35) (1 sigma).(5) Our results show that more precise time delay measurements could provide more stringent cosmological parameter values, and lensed GW+EM systems therefore can be applied as a powerful tool in the future precision cosmology.}}, DOI = {{10.3847/1538-4357/ab037e}}, Article-Number = {{37}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Fan, Xilong/0000-0002-8174-0128 li, yufeng/0000-0002-4135-074X}}, Unique-ID = {{ISI:000460136100005}}, } @article{ ISI:000460136100007, Author = {Wang, Y. Y. and Wang, F. Y.}, Title = {{Calibration of Gamma-Ray Burst Luminosity Correlations Using Gravitational Waves as Standard Sirens}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2019}}, Volume = {{873}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{Gamma-ray bursts (GRBs) are a potential tool to probe the high-redshift universe. However, the circularity problem has encouraged people to find model-independent methods to study the luminosity correlations of GRBs. Here, we present a new method that uses gravitational waves (GWs) as standard sirens to calibrate GRB luminosity correlations. For the third-generation ground-based GW detectors (i.e., Einstein Telescope-ET), the redshifts of GW events accompanying electromagnetic counterparts can reach out to similar to 4, which is more distant than type Ia supernovae (z less than or similar to 2). The Amati relation and Ghirlanda relation are calibrated using the mock GW catalog from ET. We find that the 1 sigma. uncertainty of intercepts and slopes of these correlations can be constrained to less than 0.2\% and 8\% respectively. Using calibrated correlations, the evolution of the dark energy equation of state can be tightly measured, which is important for discriminating dark energy models.}}, DOI = {{10.3847/1538-4357/ab037b}}, Article-Number = {{39}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Wang, Fayin/B-1479-2009 }}, ORCID-Numbers = {{Wang, Fayin/0000-0003-4157-7714 Wang, Yuyang/0000-0002-3822-0389}}, Unique-ID = {{ISI:000460136100007}}, } @article{ ISI:000459520800005, Author = {Yang, Tao and Holand, R. F. L. and Hu, Bin}, Title = {{Constraints on the cosmic distance duality relation with simulated data of gravitational waves from the Einstein Telescope}}, Journal = {{ASTROPARTICLE PHYSICS}}, Year = {{2019}}, Volume = {{108}}, Pages = {{57-62}}, Month = {{MAR}}, Abstract = {{The cosmic distance duality relation (CDDR) has been test through several astronomical observations in the last years. This relation establishes a simple equation relating the angular diameter (D-A) and luminosity (D-L) distances at a redshift z, DLDA-1(1 + z)(-2) = eta = 1. However, only very recently this relation has been observationally tested at high redshifts (z approximate to 53.6) by using luminosity distances from type la super-novae (SNe Ia) and gamma ray bursts (GRBs) plus angular diameter distances from strong gravitational lensing (SGL) observations. The results show that no significant deviation from the CDDR validity has been verified. In this work, we test the potentialities of future luminosity distances from gravitational waves (GWs) sources to impose limit on possible departures of CDDR jointly with current SGL observations. The basic advantage of D-L from GWs is being insensitive to non-conservation of the number of photons. By simulating 600, 900 and 1200 data of GWs using the Einstein Telescope (ET) as reference, we derive limits on eta(z) function and obtain that the results will be at least competitive with current limits from the SNe Ia + GRBs + SGLs analyses. (C) 2019 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.astropartphys.2019.01.005}}, ISSN = {{0927-6505}}, EISSN = {{1873-2852}}, ORCID-Numbers = {{Hu, Bin/0000-0001-5093-8118 Yang, Tao/0000-0002-2161-0495}}, Unique-ID = {{ISI:000459520800005}}, } @article{ ISI:000459832200004, Author = {Chang, Zhe and Huang, Qing-Guo and Wang, Sai and Zhao, Zhi-Chao}, Title = {{Low-redshift constraints on the Hubble constant from the baryon acoustic oscillation ``standard rulers{''} and the gravitational wave ``standard sirens{''}}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2019}}, Volume = {{79}}, Number = {{2}}, Month = {{FEB 26}}, Abstract = {{The multi-messenger observations of GW170817 indicated a new independent measurement of the Hubble constant (H0). We obtain the low-redshift cosmological constraints on H0 by combining this gravitational wave measurement with the observations of distance scales in baryon acoustic oscillations. Using Fisher information matrix, we estimate the projected constraints on H0 from Einstein Telescope. Simulating 103 gravitational-wave standard sirens from binary neutron star coalescences, we find that Einstein Telescope alone can constrain H0 almost as tightly as Planck final data release in the cosmological constant plus cold dark matter model. This constraint can be further improved by combining Einstein Telescope with Dark Energy Spectroscopic Instrument. The Hubble constant tension can thus be checked by observing the standard sirens with Einstein Telescope in the future.}}, DOI = {{10.1140/epjc/s10052-019-6664-0}}, Article-Number = {{177}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ORCID-Numbers = {{Wang, Sai/0000-0001-6692-6859 Chang, Zhe/0000-0002-9720-803X}}, Unique-ID = {{ISI:000459832200004}}, } @article{ ISI:000459172000001, Author = {Croon, Djuna and Gonzalo, Tomas E. and White, Graham}, Title = {{Gravitational waves from a Pati-Salam phase transition}}, Journal = {{JOURNAL OF HIGH ENERGY PHYSICS}}, Year = {{2019}}, Number = {{2}}, Month = {{FEB 13}}, Abstract = {{We analyse the gravitational wave and low energy signatures of a Pati-Salam phase transition. For a Pati-Salam scale of M (PS) similar to 10(5) GeV, we find a stochastic power spectrum within reach of the next generation of ground-based interferometer experiments such as the Einstein Telescope, in parts of the parameter space. We study the lifetime of the proton in this model, as well as complementarity with low energy constraints including electroweak precision data, neutrino mass measurements, lepton flavour violation, and collider constraints.}}, DOI = {{10.1007/JHEP02(2019)083}}, Article-Number = {{083}}, ISSN = {{1029-8479}}, ResearcherID-Numbers = {{Gonzalo, Tomas/AAH-3302-2019 }}, ORCID-Numbers = {{Gonzalo, Tomas/0000-0003-2207-1005 White, Graham/0000-0003-2541-6785 Croon, Djuna/0000-0003-3359-3706}}, Unique-ID = {{ISI:000459172000001}}, } @inproceedings{ ISI:000507575500027, Author = {Kuerban, Abudushataer and Geng, Jin-Jun and Huang, Yong-Feng}, Editor = {{Li, A and Li, BA and Xu, F}}, Title = {{GW Emission from Merging Strange Quark Star-Strange Quark Planet Systems}}, Booktitle = {{XIAMEN-CUSTIPEN WORKSHOP ON THE EQUATION OF STATE OF DENSE NEUTRON-RICH MATTER IN THE ERA OF GRAVITATIONAL WAVE ASTRONOMY}}, Series = {{AIP Conference Proceedings}}, Year = {{2019}}, Volume = {{2127}}, Note = {{Xiamen-Custipen Workshop on the the Equation of State (EOS) of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Xiamen, PEOPLES R CHINA, JAN 03-07, 2019}}, Organization = {{Xiamen Univ, China U S Theory Inst Phys Exot Nuclei; Peking Univ, China Ctr Adv Sci \& Technol; Shanghai Jiao Tong Univ}}, Abstract = {{Strange quark matter (SQM) may be the true ground state of hadromc matter. The observed pulsars may actually be strange quark stars, rather than neutron stars. With such an SQM hypothesis, researchers have predicted the existence of hydrostatically stable sequence of strange quark stars, like strange quark dwarfs and even strange quark planets. However, the SQM hypothesis is difficult to test due to the similarity between strange stars and neutron stars. Recently, we proposed a hopeful new method to probe the existence of SQM, which focuses on the study of strange quark planet systems. Strange quark planets will not be tidally disrupted even when they get very close to their host stars due to their extreme compactness. It is pointed out that one could identify strange quark planets by searching for very close-in planets among extra-solar planetary systems. Particularly, we should pay attention to possible pulsar planets with an orbital radius less than about 5.6 x 10(10) cm and/or an orbital period less than about 6100 s. The pulsar planet of PSR J1719 - 1438 b, with an orbital radius of similar to 6 x 10(10) cm and orbital period of 7837 s, is encouragingly found to be a good candidate. Additionally, recent progresses in the field of gravitational wave astronomy encourages us to study gravitational waves emission from SQM planet systems. Strange quark planets can spiral very close to their host strange stars, and produce strong gravitational waves at the final merging stage. This kind of events can he detected by our current and upcoming gravitational wave detectors, such as the advanced LIGO and the Einstein Telescope.}}, DOI = {{10.1063/1.5117817}}, Article-Number = {{020027}}, ISSN = {{0094-243X}}, ISBN = {{978-0-7354-1869-1}}, ResearcherID-Numbers = {{Geng, Jin-Jun/K-4623-2019 }}, ORCID-Numbers = {{Geng, Jin-Jun/0000-0001-9648-7295 Kuerban, Abudushataer/0000-0002-2162-0378 Huang, Yongfeng/0000-0001-7199-2906}}, Unique-ID = {{ISI:000507575500027}}, } @article{ ISI:000455239200007, Author = {Akcay, Sarp}, Title = {{Forecasting Gamma-Ray Bursts Using Gravitational Waves}}, Journal = {{ANNALEN DER PHYSIK}}, Year = {{2019}}, Volume = {{531}}, Number = {{1}}, Month = {{JAN}}, Abstract = {{The intriguing possibility of employing future ground-based gravitational-wave interferometers to forecast short gamma-ray bursts (GRBs) is explored. The forecasting prospect is quantified in terms of an advance-warning time: the binary-neutron star (BNS) inspiral time (to merger) from when the interferometer network accumulates a signal-to-noise ratio of 15. As sources for the Advanced LIGO-Virgo (ALV) network of 2020, BNS systems at luminosity distances of D <= 200 Mpc are considered, and similarly, BNS systems at D <= 1000 Mpc for Einstein Telescope. It is shown that the ALV network will provide a few minutes of warning time, thus will not forecast GRBs in the 2020s. On the other hand, Einstein Telescope will provide advance-warning times of more than 5 hours for D <= 100 Mpc. Taking 1 hour as a benchmark advance-warning time, a corresponding BNS range of roughly 600 Mpc is obtained for Einstein Telescope. Using current BNS event rates, it is shown that Einstein Telescope will forecast O(102) GRBs in the 2030s. This warning-time computation is reapplied to black hole-neutron star inspirals and it is found that one to three tidal disruption events are expected to be forecast by the same detector.}}, DOI = {{10.1002/andp.201800365}}, Article-Number = {{1800365}}, ISSN = {{0003-3804}}, EISSN = {{1521-3889}}, Unique-ID = {{ISI:000455239200007}}, } @article{ ISI:000455194000016, Author = {Akutsu, T. and Ando, M. and Arai, K. and Arai, Y. and Araki, S. and Araya, A. and Aritomi, N. and Asada, H. and Aso, Y. and Atsuta, S. and Awai, K. and Bae, S. and Baiotti, L. and Barton, M. A. and Cannon, K. and Capocasa, E. and Chen, C-S. and Chiu, T-W. and Cho, K. and Chu, Y-K. and Craig, K. and Creus, W. and Doi, K. and Eda, K. and Enomoto, Y. and Flaminio, R. and Fujii, Y. and Fujimoto, M. -K. and Fukunaga, M. and Fukushima, M. and Furuhata, T. and Haino, S. and Hasegawa, K. and Hashino, K. and Hayama, K. and Hirobayashi, S. and Hirose, E. and Hsieh, B. H. and Huang, C-Z. and Ikenoue, B. and Inoue, Y. and Ioka, K. and Itoh, Y. and Izumi, K. and Kaji, T. and Kajita, T. and Kakizaki, M. and Kamiizumi, M. and Kanbara, S. and Kanda, N. and Kanemura, S. and Kaneyama, M. and Kang, G. and Kasuya, J. and Kataoka, Y. and Kawai, N. and Kawamura, S. and Kawasaki, T. and Kim, C. and Kim, J. and Kim, J. C. and Kim, W. S. and Kim, Y. -M. and Kimura, N. and Kinugawa, T. and Kirii, S. and Kitaoka, Y. and Kitazawa, H. and Kojima, Y. and Kokeyama, K. and Komori, K. and Kong, A. K. H. and Kotake, K. and Kozu, R. and Kumar, R. and Kuo, H-S. and Kuroyanagi, S. and Lee, H. K. and Lee, H. M. and Lee, H. W. and Leonardi, M. and Lin, C-Y. and Lin, F-L. and Liu, G. C. and Liu, Y. and Majorana, E. and Mano, S. and Marchio, M. and Matsui, T. and Matsushima, F. and Michimura, Y. and Mio, N. and Miyakawa, O. and Miyamoto, A. and Miyamoto, T. and Miyo, K. and Miyoki, S. and Morii, W. and Morisaki, S. and Moriwaki, Y. and Morozumi, T. and Musha, M. and Nagano, K. and Nagano, S. and Nakamura, K. and Nakamura, T. and Nakano, H. and Nakano, M. and Nakao, K. and Narikawa, T. and Naticchioni, L. and Quynh, L. Nguyen and Ni, W. -T. and Nishizawa, A. and Obuchi, Y. and Ochi, T. and Oh, J. J. and Oh, S. H. and Ohashi, M. and Ohishi, N. and Ohkawa, M. and Okutomi, K. and Ono, K. and Oohara, K. and Ooi, C. P. and Pan, S-S. and Park, J. and Arellano, F. E. Pena and Pinto, I. and Sago, N. and Saijo, M. and Saitou, S. and Saito, Y. and Sakai, K. and Sakai, Y. and Sakai, Y. and Sasai, M. and Sasaki, M. and Sasaki, Y. and Sato, S. and Sato, N. and Sato, T. and Sekiguchi, Y. and Seto, N. and Shibata, M. and Shimoda, T. and Shinkai, H. and Shishido, T. and Shoda, A. and Somiya, K. and Son, E. J. and Suemasa, A. and Suzuki, T. and Suzuki, T. and Tagoshi, H. and Tahara, H. and Takahashi, H. and Takahashi, R. and Takamori, A. and Takeda, H. and Tanaka, H. and Tanaka, K. and Tanaka, T. and Tanioka, S. and San Martin, E. N. Tapia and Tatsumi, D. and Tomaru, T. and Tomura, T. and Travasso, F. and Tsubono, K. and Tsuchida, S. and Uchikata, N. and Uchiyama, T. and Uehara, T. and Ueki, S. and Ueno, K. and Uraguchi, F. and Ushiba, T. and van Putten, M. H. P. M. and Vocca, H. and Wada, S. and Wakamatsu, T. and Watanabe, Y. and Xu, W-R. and Yamada, T. and Yamamoto, A. and Yamamoto, K. and Yamamoto, K. and Yamamoto, S. and Yamamoto, T. and Yokogawa, K. and Yokoyama, J. and Yokozawa, T. and Yoon, T. H. and Yoshioka, T. and Yuzurihara, H. and Zeidler, S. and Zhu, Z. -H. and KAGRA}, Title = {{KAGRA: 2.5 generation interferometric gravitational wave detector}}, Journal = {{NATURE ASTRONOMY}}, Year = {{2019}}, Volume = {{3}}, Number = {{1}}, Pages = {{35-40}}, Month = {{JAN}}, Abstract = {{The recent detections of gravitational waves (GWs) reported by the LIGO and Virgo collaborations have made a significant impact on physics and astronomy. A global network of GW detectors will play a key role in uncovering the unknown nature of the sources in coordinated observations with astronomical telescopes and detectors. Here we introduce KAGRA, a new GW detector with two 3 km baseline arms arranged in an `L' shape. KAGRA's design is similar to the second generations of Advanced LIGO and Advanced Virgo, but it will be operating at cryogenic temperatures with sapphire mirrors. This low-temperature feature is advantageous for improving the sensitivity around 100 Hz and is considered to be an important feature for the third-generation GW detector concept (for example, the Einstein Telescope of Europe or the Cosmic Explorer of the United States). Hence, KAGRA is often called a 2.5-generation GW detector based on laser interferometry. KAGRA's first observation run is scheduled in late 2019, aiming to join the third observation run of the advanced LIGO-Virgo network. When operating along with the existing GW detectors, KAGRA will be helpful in locating GW sources more accurately and determining the source parameters with higher precision, providing information for follow-up observations of GW trigger candidates.}}, DOI = {{10.1038/s41550-018-0658-y}}, ISSN = {{2397-3366}}, ResearcherID-Numbers = {{Kakizaki, Mitsuru/AAB-3015-2020 Naticchioni, Luca/AAB-7775-2019 Leonardi, Matteo/G-9694-2015 Tahara, Hidetoshi/G-7697-2019 Chiu, Ting-Wai/D-7400-2019 Shinkai, Hisa-aki/S-6590-2016 Leonardi, Matteo/AAT-5237-2020 Nakamura, Kouji/H-6364-2013 Aso, Yoichi/R-9361-2019 van Putten, Maurice/R-3171-2019 Takahashi, Ryutaro/C-2903-2013 Travasso, Flavio/J-9595-2016 Vocca, Helios/J-9579-2016 Kinugawa, Tomoya/AAU-3650-2020 ANDO, MASAKI/G-4989-2014 Somiya, Kentaro/ABE-2215-2020 Kuroyanagi, Sachiko/B-3843-2017 }}, ORCID-Numbers = {{Naticchioni, Luca/0000-0003-2918-0730 Leonardi, Matteo/0000-0002-7641-0060 Chiu, Ting-Wai/0000-0002-7371-1132 Shinkai, Hisa-aki/0000-0003-1082-2844 Nakamura, Kouji/0000-0001-6148-4289 Aso, Yoichi/0000-0002-1902-6695 Travasso, Flavio/0000-0002-4653-6156 Vocca, Helios/0000-0002-1200-3917 ANDO, MASAKI/0000-0002-8865-9998 Somiya, Kentaro/0000-0003-2601-2264 Kuroyanagi, Sachiko/0000-0001-6538-1447 UCHIKATA, NAMI/0000-0003-0030-3653 Aritomi, Naoki/0000-0003-4424-7657 Saijo, Motoyuki/0000-0003-3572-3746 Enomoto, Yutaro/0000-0001-6426-7079 Nguyen, Lan Quynh/0000-0002-1828-3702 Kim, Young-Min/0000-0001-8720-6113 Lin, Chun-Yu/0000-0002-7489-7418 Capocasa, Eleonora/0000-0003-3762-6958 Majorana, Ettore/0000-0002-2383-3692 Akutsu, Tomotada/0000-0003-0733-7530 Kong, Albert/0000-0002-5105-344X Tanioka, Satoshi/0000-0003-3321-1018 Oh, Sang Hoon/0000-0003-1184-7453 Zeidler, Simon/0000-0001-7949-1292 Pinto, Innocenzo M./0000-0002-2679-4457 Park, June Gyu/0000-0002-7510-0079 Shoda, Ayaka/0000-0002-0236-4735 Kuroyanagi, Sachiko/0000-0002-0950-2918 Lee, Hyung Mok/0000-0003-4412-7161 Yamamoto, Kohei/0000-0002-5064-4619 Yamamoto, Kazuhiro/0000-0001-5647-6735 Nakano, Hiroyuki/0000-0001-7665-0796 /0000-0003-2900-4817}}, Unique-ID = {{ISI:000455194000016}}, } @article{ ISI:000454428100002, Author = {Kastha, Shilpa and Gupta, Anuradha and Arun, K. G. and Sathyaprakash, B. S. and Van den Broeck, Chris}, Title = {{Testing the multipole structure of compact binaries using gravitational wave observations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{12}}, Month = {{DEC 26}}, Abstract = {{We propose a novel method to test the consistency of the multipole moments of compact binary systems with the predictions of general relativity (GR). The multipole moments of a compact binary system, known in terms of symmetric and trace-free tensors, are used to calculate the gravitational waveforms from compact binaries within the post-Newtonian (PN) formalism. For nonspinning compact binaries, we derive the gravitational wave phasing formula, in the frequency domain, parametrizing each PN order term in terms of the multipole moments which contribute to that order. Using GW observations, this parametrized multipolar phasing would allow us to derive the bounds on possible departures from the multipole structure of GR and hence constrain the parameter space of alternative theories of gravity. We compute the projected accuracies with which the second-generation ground-based detectors, such as the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO), the third-generation detectors such as the Einstein Telescope and Cosmic Explorer, as well as the space-based detector Laser Interferometer Space Antenna (LISA) will be able to measure these multipole parameters. We find that while Advanced LIGO can measure the first two or three multipole coefficients with good accuracy, Cosmic Explorer and the Einstein Telescope may be able to measure the first four multipole coefficients which enter the phasing formula. Intermediate-mass-ratio inspirals, with mass ratios of several tens, in the frequency band of the planned space-based LISA mission should be able to measure all seven multipole coefficients which appear in the 3.5PN phasing formula. Our finding highlights the importance of this class of sources for probing the strong-field gravity regime. The proposed test will facilitate the first probe of the multipolar structure of Einstein's general relativity.}}, DOI = {{10.1103/PhysRevD.98.124033}}, Article-Number = {{124033}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Gupta, Anuradha/0000-0002-5441-9013 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000454428100002}}, } @article{ ISI:000453951200001, Author = {Maria Ezquiaga, Jose and Zumalacarregui, Miguel}, Title = {{Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy}}, Journal = {{FRONTIERS IN ASTRONOMY AND SPACE SCIENCES}}, Year = {{2018}}, Volume = {{5}}, Month = {{DEC 21}}, Abstract = {{Gravitational waves (GWs) provide a new tool to probe the nature of dark energy (DE) and the fundamental properties of gravity. We review the different ways in which GWs can be used to test gravity and models for late-time cosmic acceleration. Lagrangian-based gravitational theories beyond general relativity (GR) are classified into those breaking fundamental assumptions, containing additional fields and massive graviton(s). In addition to Lagrangian based theories we present the effective theory of DE and the mu-Sigma parametrization as general descriptions of cosmological gravity. Multi-messenger GW detections can be used to measure the cosmological expansion (standard sirens), providing an independent test of the DE equation of state and measuring the Hubble parameter. Several key tests of gravity involve the cosmological propagation of GWs, including anomalous GW speed, massive graviton excitations, Lorentz violating dispersion relation, modified GW luminosity distance and additional polarizations, which may also induce GW oscillations. We summarize present constraints and their impact on DE models, including those arising from the binary neutron star merger GW170817. Upgrades of LIGO-Virgo detectors to design sensitivity and the next generation facilities such as LISA or Einstein Telescope will significantly improve these constraints in the next two decades.}}, DOI = {{10.3389/fspas.2018.00044}}, Article-Number = {{44}}, ISSN = {{2296-987X}}, ResearcherID-Numbers = {{Perez, Miguel Zumalacarregui/K-1426-2014 }}, ORCID-Numbers = {{Perez, Miguel Zumalacarregui/0000-0002-9943-6490 Ezquiaga, Jose Maria/0000-0002-7213-3211}}, Unique-ID = {{ISI:000453951200001}}, } @article{ ISI:000452982000007, Author = {Forteza, Xisco Jimenez and Abdelsalhin, Tiziano and Pani, Paolo and Gualtieri, Leonardo}, Title = {{Impact of high-order tidal terms on binary neutron-star waveforms}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{12}}, Month = {{DEC 13}}, Abstract = {{GW170817, the milestone gravitational-wave event originated from a binary neutron star merger, has allowed scientific community to place a constraint on the equation of state of neutron stars by extracting the leading-order, tidal-deformability term from the gravitational waveform. Here we incorporate tidal corrections to the gravitational-wave phase at next-to-leading and next-to-next-to-leading order, including the magnetic tidal Love numbers, tail effects, and the spin-tidal couplings recently computed in Tiziano Abdelsalhin et al. {[}Phys. Rev. D 98,104046 (2018)]. These effects have not yet been included in the waveform approximants for the analysis of GW170817. We provide a qualitative and quantitative analysis of the impact of these new terms by studying the parameter bias induced on events compatible with GW170817 assuming second-generation (advanced LIGO) and third-generation (Einstein Telescope) ground-based gravitational-wave interferometers. We fmd that including the tidal-tail term deteriorates the convergence properties of the post-Newtonian expansion in the relevant frequency range. We also find that the effect of magnetic tidal Love numbers could be measurable for an optimal GW170817 event with signal-to-noise ratio approximate to 1750 detected with the Einstein Telescope. On the same line, spin-tidal couplings may be relevant if mildly high-spin chi greater than or similar to 0.1 neutron star binaries exist in nature.}}, DOI = {{10.1103/PhysRevD.98.124014}}, Article-Number = {{124014}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Gualtieri, Leonardo/F-2612-2012 Pani, Paolo/G-7412-2012}}, ORCID-Numbers = {{Gualtieri, Leonardo/0000-0002-1097-3266 Pani, Paolo/0000-0003-4443-1761}}, Unique-ID = {{ISI:000452982000007}}, } @article{ ISI:000452689300002, Author = {Phelps, Margot and Reid, Mariela Masso and Douglas, Rebecca and van Veggel, Anna-Maria and Mangano, Valentina and Haughian, Karen and Jongschaap, Arjen and Kelly, Meghan and Hough, James and Rowan, Sheila}, Title = {{Strength of hydroxide catalysis bonds between sapphire, silicon, and fused silica as a function of time}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{12}}, Month = {{DEC 10}}, Abstract = {{Hydroxide catalysis bonds have formed an integral part of ground-based gravitational wave (GW) observatories since the 1990s. By allowing the creation of quasimonolithic fused silica mirror suspensions in detectors such as GEO600 and Advanced LIGO, their use was crucial to the first ever direct detection of gravitational waves. Following these successes, this bonding technique has been included in advanced next generation cryogenic detector designs. Currently, they are used to create quasimonolithic crystalline sapphire suspensions in the KAGRA detector. They are also planned for use in silicon suspensions of future detectors such as the Einstein Telescope. In this paper we report how the strength of hydroxide catalysis bonds evolves over time, and compare the curing rates of bonds as they form between fused silica substrates to those between sapphire to sapphire and silicon to silicon substrates. For bonds between all three types of substrate material we show that newly formed bonds exhibit slightly higher breaking stresses than bonds cured for longer periods of time. We find that the strength stabilizes at >= 15 MPa for bonds cured for up to 30 weeks (7 months). This finding is important to future cryogenic GW detector design as it is crucial to ensure the long term integrity of the suspension interfaces. Monitoring the strength of bonds that have been allowed to cure for shorter lengths of time can also shed light on the chemistry of bond formation.}}, DOI = {{10.1103/PhysRevD.98.122003}}, Article-Number = {{122003}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Mangano, Valentina/AAC-9281-2020 }}, ORCID-Numbers = {{Mangano, Valentina/0000-0001-7902-8505 Masso Reid, Mariela/0000-0001-6177-8105 Hennig, Margot Hensler/0000-0003-1531-8460}}, Unique-ID = {{ISI:000452689300002}}, } @article{ ISI:000450235800007, Author = {Alexander, Stephon and McDonough, Evan and Sims, Robert and Yunes, Nicolas}, Title = {{Hidden-sector modifications to gravitational waves from binary inspirals}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2018}}, Volume = {{35}}, Number = {{23}}, Month = {{DEC 6}}, Abstract = {{Gravitational wave astronomy has placed strong constraints on fundamental physics, and there is every expectation that future observations will continue to do so. In this work we quantify this expectation for future binary merger observations to constrain hidden sectors, such as scalar-tensor gravity or dark matter, which induce a Yukawa-type modification to the gravitational potential. We explicitly compute the gravitational waveform, and perform a Fisher information matrix analysis to estimate the sensitivity of next generation gravitational wave detectors to these modifications. We find an optimal sensitivity to the Yukawa interaction strength of 10(-5) and to the associated dipole emission parameter of 10(-7), with the best constraints arising from the Einstein telescope. When applied to a minimal model of dark matter, this provides an exquisite probe of dark matter accumulation by neutron stars, and for sub-TeV dark matter gravitational waves are able to detect mass fractions m(DM)/m(Ns) less then 1 part in 10(15).}}, DOI = {{10.1088/1361-6382/aaeb5c}}, Article-Number = {{235012}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Yunes, Nicolas/AAG-3146-2019}}, ORCID-Numbers = {{Yunes, Nicolas/0000-0001-6147-1736}}, Unique-ID = {{ISI:000450235800007}}, } @article{ ISI:000450221800029, Author = {Wei, Jun-Jie}, Title = {{Model-independent Curvature Determination from Gravitational-wave Standard Sirens and Cosmic Chronometers}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2018}}, Volume = {{868}}, Number = {{1}}, Month = {{NOV 20}}, Abstract = {{The detection of gravitational waves (GWs) provides a direct way to measure the luminosity distance, which enables us to probe cosmology. In this paper, we continue to expand the application of GW standard sirens in cosmology, and propose that the spatial curvature can be estimated in a model-independent way by comparing the distances from future GW sources and current cosmic-chronometer observations. We expect an electromagnetic counterpart of the GW event to give the source redshift, and simulate hundreds of GW data from the coalescence of double neutron stars and black hole-neutron star binaries using the Einstein Telescope as a reference. Our simulations show that, fr(o)m 100 simulated GW events and 31 current cosmic-chronometer measurements, the error of the curvature parameter Omega(K) is expected to be constrained at the level of similar to 0.125. If 1000 GW events were observed, the uncertainty of Omega(K) would be further reduced to similar to 0.040. We also find that adding 50 mock H(z) data points (consisting of 81 cosmic-chronometer data points and 1000 simulated GW events) could result in a much tighter constraint on the zero cosmic curvature, for which Omega(K) = -0.002 +/- 0.028. Compared to some actual model-independent curvature tests involving distances from other cosmic probes, this method using GW data achieves constraints with much higher precision.}}, DOI = {{10.3847/1538-4357/aae696}}, Article-Number = {{29}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Wei, Jun-Jie/0000-0003-0162-2488}}, Unique-ID = {{ISI:000450221800029}}, } @article{ ISI:000449412000008, Author = {Fragione, Giacomo and Leigh, Nathan W. C. and Ginsburg, Idan and Kocsis, Bence}, Title = {{Tidal Disruption Events and Gravitational Waves from Intermediate-mass Black Holes in Evolving Globular Clusters across Space and Time}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2018}}, Volume = {{867}}, Number = {{2}}, Month = {{NOV 10}}, Abstract = {{We present a semi-analytic model for self-consistently evolving a population of globular clusters (GCs) in a given host galaxy across cosmic time. We compute the fraction of GCs still hosting intermediate-mass black holes (IMBHs) at a given redshift in early and late -type galaxies of different masses and sizes, and the corresponding rate of tidal disruption events (TDEs), both main-sequence (MS) and white dwarf (WD) stars. We find that the integrated TDE rate for the entire GC population can exceed the corresponding rate in a given galactic nucleus and that similar to 90\% of the TDEs reside in GCs within a maximum radius of similar to 2-15 kpc from the host galaxy's center. This suggests that observational efforts designed to identify TDEs should not confine themselves to galactic nuclei alone, but should also consider the outer galactic halo where massive old GCs hosting IMBHs would reside. Indeed, such off-center TDEs as predicted here may already have been observed. MS TDE rates are more common than WD TDE rates by a factor of 30 (100) at z less than or similar to 0.5 (z = 2). We also calculate the rate of IMBH-SBH mergers across cosmic time, finding that the typical IMRI rate at low redshift is of the order of similar to 0.5-3 Gpc(-3) yr(-1), which becomes as high as similar to 100 Gpc(-3) yr(-1) near the peak of GC formation. Advanced LIGO, combined with VIRGO, KAGRA, the Einstein Telescope, and LISA will be able to observe the bottom end and top end of the IMBH population.}}, DOI = {{10.3847/1538-4357/aae486}}, Article-Number = {{119}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Kocsis, Bence/AAX-1181-2020 Fragione, Giacomo/ABC-2055-2020 Kocsis, Bence/C-3061-2013}}, ORCID-Numbers = {{Kocsis, Bence/0000-0002-4865-7517 Kocsis, Bence/0000-0002-4865-7517}}, Unique-ID = {{ISI:000449412000008}}, } @article{ ISI:000448756300005, Author = {Lai, Kwun-Hang and Li, Tjonnie Guang Feng}, Title = {{Constraining black hole horizon effects by LIGO-Virgo detections of inspiralling binary black holes}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{8}}, Month = {{OCT 30}}, Abstract = {{General relativity predicts mass and spin growth of an inspiralling black hole due to an energy-momentum flux flowing through the black-hole horizon. The leading-order terms of this horizon flux introduce 2.5 and 3.5 post-Newtonian corrections to inspiral motions of binary black holes. The corrections may be measurable by gravitational waves detectors. Since the proper improvements to general relativity are still a mystery, it is possible that the true modified gravity theory introduces negligible direct corrections to the geodesics of test masses, while near-horizon corrections are observable. We introduce a parametrization to describe arbitrary mass and spin growth of inspiralling black holes. Comparing signals of gravitational waves and a waveform model with parametrized horizon flux corrections, deviations from general relativity can be constrained. We simulate a set of gravitational wave signals following an astrophysical distribution with horizon flux modifications. Then, we perform a Bayesian analysis to obtain the expected constraints from the simulated response of the Advanced LIGO-Virgo detector network to the simulated signals. We show that the constraint can be improved by stacking multiple detections. The constraints of modified horizon flux can be used to test a specific class of modified gravity theories which predict dominant corrections near black-hole horizons over other types of corrections to general relativity. To support Hawking's area theorem at 90\% confidence level, over 10000 LIGO-Virgo detections are required. Within the lifetime of the LIGO and Einstein Telescope, a future ground-based gravitational wave detector, near-horizon corrections of modified gravity theories are potentially detectable if one of the modified gravity theories is true and the theory predicts a strong correction.}}, DOI = {{10.1103/PhysRevD.98.084059}}, Article-Number = {{084059}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Lai, Kwun-Hang/0000-0003-0446-119X}}, Unique-ID = {{ISI:000448756300005}}, } @article{ ISI:000448284600004, Author = {Liu, Tan and Zhang, Xing and Zhao, Wen and Lin, Kai and Zhang, Chao and Zhang, Shaojun and Zhao, Xiang and Zhu, Tao and Wang, Anzhong}, Title = {{Waveforms of compact binary inspiral gravitational radiation in screened modified gravity}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{8}}, Month = {{OCT 25}}, Abstract = {{Scalar-tensor gravity, with the screening mechanisms to avoid the severe constraints of the fifth force in the Solar System, can be described with a unified theoretical framework, the so-called screened modified gravity (SMG). Within this framework, in this paper we calculate the waveforms of gravitational-waves (GWs) emitted by inspiral compact binaries, which include four polarization modes, the plus h(+), cross h(x), breathing h(b), and longitudinal h(L) modes. The scalar polarizations h(b) and h(L) are both caused by the scalar field of SMG, and satisfy a simple linear relation. With the stationary phase approximations, we obtain their Fourier transforms, and derive the correction terms in the amplitude, phase, and polarizations of GWs, relative to the corresponding results in general relativity. The corresponding parametrized post-Einsteinian parameters in the general SMG are also identified. Imposing the noise level of the ground-based Einstein Telescope, we find that GW detections from inspiral compact binaries composed of a neutron star and a black hole can place stringent constraints on the sensitivities of neutron stars, and the bound is applicable to any SMG theory. Finally, we apply these results to some specific theories of SMG, including chameleon, symmetron, dilaton and f (R).}}, DOI = {{10.1103/PhysRevD.98.083023}}, Article-Number = {{083023}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Zhu, Tao/P-6343-2019 Wang, Anzhong/AAS-9614-2020 }}, ORCID-Numbers = {{Zhu, Tao/0000-0003-2286-9009 Zhang, Chao/0000-0001-9915-8649 Zhao, Wen/0000-0002-1330-2329 Zhang, Xing/0000-0001-5435-6502}}, Unique-ID = {{ISI:000448284600004}}, } @article{ ISI:000448052300002, Author = {Dickmann, Johannes and Kroker, Stefanie}, Title = {{Highly reflective low-noise etalon-based meta-mirror}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{8}}, Month = {{OCT 23}}, Abstract = {{We present a concept of a mirror for application in high-reflectivity low-noise instruments such as interferometers. The concept is based on an etalon with a metasurface (meta-etalon) on the front and a conventional multilayer stack on the rear surface. The etalon in combination with the metasurface enables a dedicated spatial weighing of the relevant thermal noise processes and by this a substantial reduction of the overall readout thermal noise. As examples, we illustrate the benefit of the proposed etalon for thermal noise in two applications: the test masses of the Einstein Telescope gravitational wave detector and a single-crystalline cavity for laser frequency stabilization. In the Einstein Telescope, the thermal noise of the etalon even at room temperature outperforms existing concepts for operation temperatures at 10 K. For the laser stabilization cavity, a reduction of the modified Allan deviation of an order of magnitude is predicted.}}, DOI = {{10.1103/PhysRevD.98.082003}}, Article-Number = {{082003}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Kroker, Stefanie/Q-8871-2016 }}, ORCID-Numbers = {{Kroker, Stefanie/0000-0002-7584-7359 Dickmann, Johannes/0000-0002-4700-5912}}, Unique-ID = {{ISI:000448052300002}}, } @article{ ISI:000447467800007, Author = {Osato, Ken}, Title = {{Exploring the distance-redshift relation with gravitational wave standard sirens and tomographic weak lensing}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{8}}, Month = {{OCT 16}}, Abstract = {{Gravitational waves from inspiraling compact objects provide us with information of the distance scale since we can infer the absolute luminosity of the source from analysis of the wave form, which is known as standard sirens. The first detection of the gravitational wave signal of the binary black hole merger event by Advanced LIGO has opened up the possibility of utilizing standard sirens as cosmological probe. In order to extract information of the distance-redshift relation, we cross-correlate weak lensing, which is an unbiased tracer of matter distribution in the Universe, with the projected number density of gravitational wave sources. For weak lensing, we employ tomography technique to efficiently obtain information of large-scale structures at wide ranges of redshifts. Making use of the cross-correlations along with the autocorrelations, we present forecast of constraints on four cosmological parameters, i.e., Hubble parameter, matter density, the equation of state parameter of dark energy, and the amplitude of matter fluctuation. To fully explore the ability of cross-correlations, which require large overlapping sky coverage, we consider the specific case with the upcoming surveys by Euclid for weak lensing and Einstein Telescope for standard sirens. We show that cosmological parameters can be tightly constrained solely by these auto-and cross-correlations of standard sirens and weak lensing. For example, the 1-sigma error of Hubble parameter is expected to be sigma(H-0) = 0.33 km s(-1) Mpc(-1). Thus, the proposed statistics will be a promising probe into the distance scale.}}, DOI = {{10.1103/PhysRevD.98.083524}}, Article-Number = {{083524}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Osato, Ken/0000-0002-7934-2569}}, Unique-ID = {{ISI:000447467800007}}, } @article{ ISI:000442567900032, Author = {Du, Shuang and Li, Xiao-Dong and Hu, Yi-Ming and Peng, Fang-Kun and Li, Miao}, Title = {{Gravitational waves induced by the asymmetric jets of gamma-ray bursts}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2018}}, Volume = {{480}}, Number = {{1}}, Pages = {{402-406}}, Month = {{OCT}}, Abstract = {{We study the gravitational wave (GW) production induced by the asymmetric jets of gamma-ray bursts (GRBs). The asymmetric jets result in a recoil force acted on the central compact object, whose motion leads to the emission of GWs. Under reasonable assumptions and simplifications, we derive the analytic form of the produced GWs. The amplitude of emitted GWs is estimated to be relatively low, but possibility exists that they can be detected by future experiments such as the Einstein Telescope. We find the dynamical properties of the central object, which is difficult to be studied via the electromagnetic channel, can be inferred by measuring the emitted GWs. Moreover, we find the emitted GWs can be used to determine whether the relativistic jets are launched by the neutrino annihilation process or the Blandford-Znajek process, which cannot be clearly distinguished by the current GRB observations. Our work manifests the importance of the GW channel in multimessenger astronomy. The physical information encoded in the GW and electromagnetic wave (EW) emissions of an astrophysical object is complementary to each other; in case some physics cannot be effectively investigated using the EW channel alone, including the GW channel can be very helpful.}}, DOI = {{10.1093/mnras/sty1800}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Hu, Yi-Ming/0000-0002-7869-0174 Peng, Fangkun/0000-0001-7171-5132 Du, Shuang/0000-0001-5247-5559 Li, Xiao-Dong/0000-0003-3964-0438}}, Unique-ID = {{ISI:000442567900032}}, } @article{ ISI:000445504200003, Author = {Amaro-Seoane, Pau}, Title = {{Detecting intermediate-mass ratio inspirals from the ground and space}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{6}}, Month = {{SEP 24}}, Abstract = {{The detection of the gravitational capture of a stellar-mass compact object by a massive black hole (MBH) will allow us to test gravity in the strong regime. The repeated, accumulated bursts of gravitational radiation from these sources can be envisaged as a geodesic mapping of space-time around the MBH. These sources form via two-body relaxation, by exchanging energy and angular momentum, and inspiral in a slow, progressive way down to the final merger. The frequencies fall in the millihertz range for MBHs with masses similar to 10(6) M-circle dot, i.e., that of space-borne gravitational-wave observatories such as LISA. In this article we show that, depending on their orbital parameters, intermediate-mass ratio inspirals (IMRIs) of MBHs with masses between a hundred and a few thousand M-circle dot have frequencies that make them detectable (i) with ground-based observatories, or (ii) with both LISA and ground-based observatories (such as advanced LIGO/Virgo) and third-generation observatories {[}such as the Einstein Telescope (ET)]. The binaries have a signal-to-noise ratio large enough to ensure detection. More extreme values of the orbital parameters correspond to systems that are only detectable with ground-based detectors and in particular enter the LIGO/Virgo band in many different harmonics for masses up to 2000 M-circle dot. We show that environmental effects are negligible, so the source should not have this kind of complication. The accumulated phase shift is measurable with LISA and ET, and for some cases also with LIGO, so that it is possible to recover information about the eccentricity and formation scenario. For IMRIs with a total mass (sic) 2000 M-circle dot and initial eccentricities up to 0.999, LISA can give a advanced warning to ground-based detectors with seconds of precision. The possibility of detecting IMRIs from the ground alone or combined with spac-borne observatories opens new possibilities for gravitational-wave astronomy.}}, DOI = {{10.1103/PhysRevD.98.063018}}, Article-Number = {{063018}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Amaro Seoane, Pau/0000-0003-3993-3249}}, Unique-ID = {{ISI:000445504200003}}, } @article{ ISI:000445103800012, Author = {Megias, Eugenio and Nardini, Germano and Quiros, Mariano}, Title = {{Cosmological phase transitions in warped space: gravitational waves and collider signatures}}, Journal = {{JOURNAL OF HIGH ENERGY PHYSICS}}, Year = {{2018}}, Number = {{9}}, Month = {{SEP 17}}, Abstract = {{We study the electroweak phase transition within a 5D warped model including a scalar potential with an exponential behavior, and strong back-reaction over the metric, in the infrared. By means of a novel treatment of the superpotential formalism, we explore parameter regions that were previously inaccessible. We find that for large enough values of the t'Hooft parameter (e.g. N similar or equal to 25) the holographic phase transition occurs, and it can force the Higgs to undergo a first order electroweak phase transition, suitable for electroweak baryogenesis. The model exhibits gravitational waves and colliders signatures. It typically predicts a stochastic gravitational wave background observable both at the Laser Interferometer Space Antenna and at the Einstein Telescope. Moreover the radion tends to be heavy enough such that it evades current constraints, but may show up in future LHC runs.}}, DOI = {{10.1007/JHEP09(2018)095}}, Article-Number = {{095}}, ISSN = {{1029-8479}}, ResearcherID-Numbers = {{Megias, Eugenio/D-8903-2019 }}, ORCID-Numbers = {{Megias, Eugenio/0000-0002-6735-9013 Nardini, Germano/0000-0002-3523-0477}}, Unique-ID = {{ISI:000445103800012}}, } @article{ ISI:000444424700001, Author = {Espinosa, J. R. and Racco, D. and Riotto, A.}, Title = {{A cosmological signature of the SM Higgs instability: gravitational waves}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2018}}, Number = {{9}}, Month = {{SEP}}, Abstract = {{A fundamental property of the Standard Model is that the Higgs potential becomes unstable at large values of the Higgs field. For the current central values of the Higgs and top masses, the instability scale is about 10(11) GeV and therefore not accessible by colliders. We show that a possible signature of the Standard Model Higgs instability is the production of gravitational waves sourced by Higgs fluctuations generated during inflation. We fully characterise the two-point correlator of such gravitational waves by computing its amplitude, the frequency at peak, the spectral index, as well as their three-point correlators for various polarisations. We show that, depending on the Higgs and top masses, either LISA or the Einstein Telescope and Advanced-Ligo, could detect such stochastic background of gravitational waves. In this sense, collider and gravitational wave physics can provide fundamental and complementary informations. Furthermore, the consistency relation among the three- and the two-point correlators could provide an efficient tool to ascribe the detected gravitational waves to the Standard Model itself. Since the mechanism described in this paper might also be responsible for the generation of dark matter under the form of primordial black holes, this latter hypothesis may find its confirmation through the detection of gravitational waves.}}, DOI = {{10.1088/1475-7516/2018/09/012}}, Article-Number = {{012}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Racco, Davide/AAB-3133-2020 }}, ORCID-Numbers = {{Racco, Davide/0000-0002-0859-8751 Espinosa, Jose R./0000-0002-7069-5050}}, Unique-ID = {{ISI:000444424700001}}, } @article{ ISI:000442886000008, Author = {Miao, Haixing and Yang, Huan and Martynov, Denis}, Title = {{Towards the design of gravitational-wave detectors for probing neutron-star physics}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{4}}, Month = {{AUG 28}}, Abstract = {{The gravitational waveform of merging binary neutron stars encodes information about extreme states of matter. Probing these gravitational emissions requires the gravitational-wave detectors to have high sensitivity above 1 kHz. Fortunately for current advanced detectors, there is a sizeable gap between the quantum-limited sensitivity and the classical noise at high frequencies. Here we propose a detector design that closes such a gap by reducing the high-frequency quantum noise with an active optomechanical filter, frequency-dependent squeezing, and high optical power. The resulting noise level from 1 to 4 kHz approaches the current facility limit and is a factor of 20 to 30 below the design of existing advanced detectors. This will allow for precision measurements of (i) the postmerger signal of the binary neutron star, (ii) late-time inspiral, merger, and ringdown of low-mass black hole-neutron star systems, and possible detection of (iii) high-frequency modes during supernovae explosions. This design tries to maximize the science return of current facilities by achieving a sensitive frequency band that is complementary to the longer-baseline third-generation detectors: the 10 km Einstein Telescope and 40 km Cosmic Explorer. We have highlighted the main technical challenges towards realizing the design, which requires dedicated research programs. If demonstrated in current facilities, the techniques can be transferred to new facilities with longer baselines.}}, DOI = {{10.1103/PhysRevD.98.044044}}, Article-Number = {{044044}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Miao, Haixing/0000-0003-2879-5821 Denis, Martynov/0000-0003-0679-1344}}, Unique-ID = {{ISI:000442886000008}}, } @article{ ISI:000438833800016, Author = {Strigin, S. E.}, Title = {{Parametric oscillatory instability in a Fabry-Perot cavity of the Einstein Telescope with different mirror's materials}}, Journal = {{PHYSICS LETTERS A}}, Year = {{2018}}, Volume = {{382}}, Number = {{33, SI}}, Pages = {{2256-2258}}, Month = {{AUG 25}}, Abstract = {{We discuss the parametric oscillatory instability in a Fabry-Perot cavity of the Einstein Telescope. Unstable combinations of elastic and optical modes for two possible configurations of gravitational wave third-generation detector are deduced. The results are compared with the results for gravitational wave interferometers LIGO and LIGO Voyager. (C) 2017 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.physleta.2017.05.049}}, ISSN = {{0375-9601}}, EISSN = {{1873-2429}}, ResearcherID-Numbers = {{Strigin, Sergey E/I-8337-2012}}, Unique-ID = {{ISI:000438833800016}}, } @article{ ISI:000439188700001, Author = {Caprini, Chiara and Figueroa, Daniel G.}, Title = {{Cosmological backgrounds of gravitational waves}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2018}}, Volume = {{35}}, Number = {{16}}, Month = {{AUG 23}}, Abstract = {{Gravitational waves (GWs) have a great potential to probe cosmology. We review early universe sources that can lead to cosmological backgrounds of GWs. We begin by presenting proper definitions of GWs in flat space-time and in a cosmological setting (section 2). Following, we discuss the reasons why early universe GW backgrounds are of a stochastic nature, and describe the general properties of a stochastic background (section 3). We recap current observational constraints on stochastic backgrounds, and discuss the basic characteristics of present and future GW detectors, including advanced LIGO, advanced Virgo, the Einstein telescope, KAGRA, and LISA (section 4). We then review in detail early universe GW generation mechanisms, as well as the properties of the GW backgrounds they give rise to. We classify the backgrounds in five categories: GWs from quantum vacuum fluctuations during standard slow-roll inflation (section 5), GWs from processes that operate within extensions of the standard inflationary paradigm (section 6), GWs from post-inflationary preheating and related non-perturbative phenomena (section 7), GWs from first order phase transitions related or not to the electroweak symmetry breaking (section 8), and GWs from general topological defects, and from cosmic strings in particular (section 9). The phenomenology of these early universe processes is extremely rich, and some of the GW backgrounds they generate can be within the reach of near-future GW detectors. A future detection of any of these backgrounds will provide crucial information on the underlying high energy theory describing the early universe, probing energy scales well beyond the reach of particle accelerators.}}, DOI = {{10.1088/1361-6382/aac608}}, Article-Number = {{163001}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Figueroa, Daniel G./B-3893-2017}}, ORCID-Numbers = {{Figueroa, Daniel G./0000-0002-4005-8915}}, Unique-ID = {{ISI:000439188700001}}, } @article{ ISI:000441858300005, Author = {Philippoz, Lionel and Boitier, Adrian and Jetzer, Philippe}, Title = {{Gravitational wave polarization from combined Earth-space detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{4}}, Month = {{AUG 16}}, Abstract = {{In this paper, we investigate the sensitivity to additional gravitational wave polarization modes of future detectors. We first look at the upcoming Einstein Telescope and its combination with existing or planned Earth-based detectors in the case of a stochastic gravitational wave background. We then study its correlation with a possible future space-borne detector sensitive to high frequencies, like DECIGO. Finally, we adapt those results for a single gravitational wave source and establish the sensitivity of the modes as well as the localization on the sky.}}, DOI = {{10.1103/PhysRevD.98.044025}}, Article-Number = {{044025}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Boitier, Adrian/0000-0002-8395-2538}}, Unique-ID = {{ISI:000441858300005}}, } @article{ ISI:000441719300001, Author = {Sarin, Nikhil and Lasky, Paul D. and Sammut, Letizia and Ashton, Greg}, Title = {{X-ray guided gravitational-wave search for binary neutron star merger remnants}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{4}}, Month = {{AUG 15}}, Abstract = {{X-ray observations of some short gamma-ray bursts indicate that a long-lived neutron star can form as a remnant of a binary neutron star merger. We develop a gravitational-wave detection pipeline for a long-lived binary neutron star merger remnant guided by these counterpart electromagnetic observations. We determine the distance out to which a gravitational-wave signal can be detected with Advanced LIGO at design sensitivity and the Einstein Telescope using this method, guided by x-ray data from GRB140903A as an example. Such gravitational waves can, in principle, be detected out to similar to 20 Mpc for Advanced LIGO and similar to 450 Mpc for the Einstein Telescope assuming a fiducial ellipticity of 10(-2). However, in practice, we can rule out such high values of the ellipticity as the total energy emitted in gravitational waves would be greater than the total rotational energy budget of the system. We show how these observations can be used to place upper limits on the ellipticity using these energy considerations. For GRB140903A, the upper limit on the ellipticity is 10(-3), which lowers the detectable distance to similar to 2 Mpc and similar to 45 Mpc for Advanced LIGO and the Einstein Telescope, respectively.}}, DOI = {{10.1103/PhysRevD.98.043011}}, Article-Number = {{043011}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Lasky, Paul/0000-0003-3763-1386}}, Unique-ID = {{ISI:000441719300001}}, } @article{ ISI:000441335000002, Author = {Testa, Adriano and Pani, Paolo}, Title = {{Analytical template for gravitational-wave echoes: Signal characterization and prospects of detection with current and future interferometers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{4}}, Month = {{AUG 10}}, Abstract = {{Gravitational-wave echoes in the postmerger ringdown phase are under intense scrutiny as probes of near-horizon quantum structures and as signatures of exotic states of matter in ultracompact stars. We present an analytical template that describes the ringdown and the echo signal for nonspinning objects in terms of two physical parameters: the reflectivity and the redshift at the surface of the object. We characterize the properties of the template and adopt it in a preliminary parameter estimation with current (aLIGO) and future (Cosmic Explorer, Einstein Telescope, LISA) gravitational-wave detectors. For fixed signal-to-noise ratio in the postmerger phase, the constraints on the model parameters depend only mildly on the details of the detector sensitivity curve, but depend strongly on the reflectivity. Our analysis suggests that it might be possible to detect or rule out Planckian corrections at the horizon scale for perfectly reflecting ultracompact objects at 5 sigma confidence level with Advanced LIGO/Virgo. On the other hand, signal-to-noise ratios in the ringdown phase equal to approximate to 100 (as achievable with future interferometers) might allow us to probe near-horizon quantum structures with reflectivity greater than or similar to 30\% (greater than or similar to 85\%) at 2 sigma (3 sigma) level.}}, DOI = {{10.1103/PhysRevD.98.044018}}, Article-Number = {{044018}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Pani, Paolo/G-7412-2012 }}, ORCID-Numbers = {{Pani, Paolo/0000-0003-4443-1761 Testa, Adriano/0000-0003-4423-9243}}, Unique-ID = {{ISI:000441335000002}}, } @article{ ISI:000442429700006, Author = {Nair, Remya and Tanaka, Takahiro}, Title = {{Synergy between ground and space based gravitational wave detectors. Part II: Localisation}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2018}}, Number = {{8}}, Month = {{AUG}}, Abstract = {{We study the advantage of combining measurements from future ground and space based gravitational wave detectors in estimating the parameters of a black-hole binary coalescence. This is an extension of our previous work (Prog. Theor. Exp. Phys. 2016 (2016) 053E01) where we used pattern averaged waveform to study non-spinning binaries. In this work we study the localisation and binary plane orientation, including the (non-precessing) spin of binaries. We focus on the third generation terrestrial detector `Einstein telescope' and a proposed space based detector `Deci-Hertz Interferometer Gravitational wave Observatory' (DECIGO). We consider two possible orbits for DECIGO, a helio-centric orbit and a Sun-synchronous geo-centric orbit. We demonstrate that one can obtain order of magnitude improvement in the localisation from the space-ground combined measurements, even with a precursor-DECIGO mission (B-DECIGO). This is especially important for the future of gravitational wave astronomy as improving the localisation accuracy further improves our chances of identifying the host galaxies of these binary systems.}}, DOI = {{10.1088/1475-7516/2018/08/033}}, Article-Number = {{033}}, ISSN = {{1475-7516}}, Unique-ID = {{ISI:000442429700006}}, } @article{ ISI:000438496600005, Author = {Belgacem, Enis and Dirian, Yves and Foffa, Stefano and Maggiore, Michele}, Title = {{Modified gravitational-wave propagation and standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{2}}, Month = {{JUL 13}}, Abstract = {{Studies of dark energy at advanced gravitational-wave (GW) interferometers normally focus on the dark energy equation of state w(DE)(z). However, modified gravity theories that predict a nontrivial dark energy equation of state generically also predict deviations from general relativity in the propagation of GWs across cosmological distances, even in theories where the speed of gravity is equal to c. We find that, in generic modified gravity models, the effect of modified GW propagation dominates over that of w(DE)(z), making modified GW propagation a crucial observable for dark energy studies with standard sirens. We present a convenient parametrization of the effect in terms of two parameters (Xi(0), n), analogue to the (w(0), w(a)) parametrization of the dark energy equation of state, and we give a limit from the LIGO/Virgo measurement of H-0 with the neutron star binary GW170817. We then perform a Markov chain Monte Carlo analysis to estimate the sensitivity of the Einstein Telescope (ET) to the cosmological parameters, including (Xi(0), n), both using only standard sirens, and combining them with other cosmological data sets. In particular, the Hubble parameter can be measured with an accuracy better than 1\% already using only standard sirens while, when combining ET with current CMB + BAO + SNe data, Xi(0) can be measured to 0.8\%. We discuss the predictions for modified GW propagation of a specific nonlocal modification of gravity, recently developed by our group, and we show that they are within the reach of ET. Modified GW propagation also affects the GW transfer function, and therefore the tensor contribution to the ISW effect.}}, DOI = {{10.1103/PhysRevD.98.023510}}, Article-Number = {{023510}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X}}, Unique-ID = {{ISI:000438496600005}}, } @article{ ISI:000438486900014, Author = {Wang, Ling-Feng and Zhang, Xuan-Neng and Zhang, Jing-Fei and Zhang, Xin}, Title = {{Impacts of gravitational-wave standard siren observation of the Einstein Telescope on weighing neutrinos in cosmology}}, Journal = {{PHYSICS LETTERS B}}, Year = {{2018}}, Volume = {{782}}, Pages = {{87-93}}, Month = {{JUL 10}}, Abstract = {{We investigate the impacts of the gravitational-wave (GW) standard siren observation of the Einstein Telescope (ET) on constraining the total neutrino mass. We simulate 1000 GW events that would be observed by the ET in its 10-year observation by taking the standard Lambda CDM cosmology as a fiducial model. We combine the simulated GW data with other cosmological observations including cosmic microwave background (CMB), baryon acoustic oscillations (BAO), and type Ia supernovae (SN). We consider three mass hierarchy cases for the neutrino mass, i.e., normal hierarchy (NH), inverted hierarchy (IH), and degenerate hierarchy (DH). Using Planck+BAO+SN, we obtain Sigma m(nu) < 0.175 eV for the NH case, Sigma m(nu) < 0.200 eV for the IH case, and Sigma m(nu) < 0.136 eV for the DH case. After considering the GW data, i.e., using Planck+ BAO+SN+GW, the constraint results become Sigma m(nu) < 0.151 eV for the NH case, Sigma m(nu) < 0.185 eV for the IH case, and Sigma m(nu) < 0.122 eV for the DH case. We find that the GW data can help reduce the upper limits of Sigma m(nu) by 13.7\%, 7.5\%, and 10.3\% for the NH, IH, and DH cases, respectively. In addition, we find that the GW data can also help break the degeneracies between Sigma m(nu) and other parameters. We show that the GW data of the ET could greatly improve the constraint accuracies of cosmological parameters. (C) 2018 The Authors. Published by Elsevier B.V.}}, DOI = {{10.1016/j.physletb.2018.05.027}}, ISSN = {{0370-2693}}, EISSN = {{1873-2445}}, ORCID-Numbers = {{Zhang, Xin/0000-0002-6029-1933}}, Unique-ID = {{ISI:000438486900014}}, } @article{ ISI:000437113500005, Author = {Nair, Remya and Bose, Sukanta and Saini, Tarun Deep}, Title = {{Measuring the Hubble constant: Gravitational wave observations meet galaxy clustering}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{98}}, Number = {{2}}, Month = {{JUL 3}}, Abstract = {{We show how the distances to binary black holes measured in gravitational wave observations with ground-based interferometers can be used to constrain the redshift-distance relation and, thereby, measure the Hubble constant (H-0). Gravitational wave observations of stellar-mass binary black holes are not expected to be accompanied by any electromagnetic event that may help in accessing their redshifts. We address this deficiency by using an optical catalog to get the distribution of galaxies in redshift. Assuming that the clustering of the binaries is correlated with that of the galaxies, we propose using that correlation to measure H-0. We show that by employing this method on simulated data obtained for second-generation networks comprising at least three detectors, e.g., the advanced LIGO-advanced VIRGO network, one can measure H-0 with an accuracy of similar to 8\% with detection of a reference population of 25 binaries, each with black holes of mass 10 M-circle dot. As expected, with third-generation detectors like the Einstein telescope (ET), which will measure distances much more accurately and to greater depths, one can obtain better estimates for H-0. Specifically, we show that with 25 observations, the ET can constrain H-0 to an accuracy of similar to 7\%. This method can also be used to estimate other cosmological parameters like the matter density Omega(m) and the dark energy equation of state.}}, DOI = {{10.1103/PhysRevD.98.023502}}, Article-Number = {{023502}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000437113500005}}, } @article{ ISI:000436889000016, Author = {Amati, L. and O'Brien, P. and Gotz, D. and Bozzo, E. and Tenzer, C. and Frontera, F. and Ghirlanda, G. and Labanti, C. and Osborne, J. P. and Stratta, G. and Tanvir, N. and Willingale, R. and Attina, P. and Campana, R. and Castro-Tirado, A. J. and Contini, C. and Fuschino, F. and Gomboc, A. and Hudec, R. and Orleanski, P. and Renotte, E. and Rodic, T. and Bagoly, Z. and Blain, A. and Callanan, P. and Covino, S. and Ferrara, A. and Le Floch, E. and Marisaldi, M. and Mereghetti, S. and Rosati, P. and Vacchi, A. and D'Avanzo, P. and Giommi, P. and Piranomonte, S. and Piro, L. and Reglero, V and Rossi, A. and Santangelo, A. and Salvaterra, R. and Tagliaferri, G. and Vergani, S. and Vinciguerra, S. and Briggs, M. and Campolongo, E. and Ciolfi, R. and Connaughton, V and Cordier, B. and Morelli, B. and Orlandini, M. and Adami, C. and Argan, A. and Atteia, J-L and Auricchio, N. and Balazs, L. and Baldazzi, G. and Basa, S. and Basak, R. and Bellutti, P. and Bernardini, M. G. and Bertuccio, G. and Braga, J. and Branchesi, M. and Brandt, S. and Brocato, E. and Budtz-Jorgensen, C. and Bulgarelli, A. and Burderi, L. and Camp, J. and Capozziello, S. and Caruana, J. and Casella, P. and Cenko, B. and Chardonnet, P. and Ciardi, B. and Colafrancesco, S. and Dainotti, M. G. and D'Elia, V and De Martino, D. and De Pasquale, M. and Del Monte, E. and Della Valle, M. and Drago, A. and Evangelista, Y. and Feroci, M. and Finelli, F. and Fiorini, M. and Fynbo, J. and Gal-Yam, A. and Gendre, B. and Ghisellini, G. and Grado, A. and Guidorzi, C. and Hafizi, M. and Hanlon, L. and Hjorth, J. and Izzo, L. and Kiss, L. and Kumar, P. and Kuvvetli, I and Lavagna, M. and Li, T. and Longo, F. and Lyutikov, M. and Maio, U. and Maiorano, E. and Malcovati, P. and Malesani, D. and Margutti, R. and Martin-Carrillo, A. and Masetti, N. and McBreen, S. and Mignani, R. and Morgante, G. and Mundell, C. and Nargaard-Nielsen, H. U. and Nicastro, L. and Palazzi, E. and Paltani, S. and Panessa, F. and Pareschi, G. and Pe'er, A. and Penacchioni, V, A. and Pian, E. and Piedipalumbo, E. and Piran, T. and Rauw, G. and Razzano, M. and Read, A. and Rezzolla, L. and Romano, P. and Ruffini, R. and Savaglio, S. and Sguera, V and Schady, P. and Skidmore, W. and Song, L. and Stanway, E. and Starling, R. and Topinka, M. and Troja, E. and van Putten, M. and Vanzella, E. and Vercellone, S. and Wilson-Hodge, C. and Yonetoku, D. and Zampa, G. and Zampa, N. and Zhang, B. and Zhang, B. B. and Zhang, S. and Zhang, S-N and Antonelli, A. and Bianco, F. and Boci, S. and Boer, M. and Botticella, M. T. and Boulade, O. and Butler, C. and Campana, S. and Capitanio, F. and Celotti, A. and Chen, Y. and Colpi, M. and Comastri, A. and Cuby, J-G and Dadina, M. and De Luca, A. and Dong, Y-W and Ettori, S. and Gandhi, P. and Geza, E. and Greiner, J. and Guiriec, S. and Harms, J. and Hernanz, M. and Hornstrup, A. and Hutchinson, I and Israel, G. and Jonker, P. and Kaneko, Y. and Kawai, N. and Wiersema, K. and Korpela, S. and Lebrun, V and Lu, F. and MacFadyen, A. and Malaguti, G. and Maraschi, L. and Melandri, A. and Modjaz, M. and Morris, D. and Omodei, N. and Paizis, A. and Pata, P. and Petrosian, V and Rachevski, A. and Rhoads, J. and Ryde, F. and Sabau-Graziati, L. and Shigehiro, N. and Sims, M. and Soomin, J. and Szecsi, D. and Urata, Y. and Uslenghi, M. and Valenziano, L. and Vianello, G. and Vojtech, S. and Watson, D. and Zicha, J.}, Title = {{The THESEUS space mission concept: science case, design and expected performances}}, Journal = {{ADVANCES IN SPACE RESEARCH}}, Year = {{2018}}, Volume = {{62}}, Number = {{1}}, Pages = {{191-244}}, Month = {{JUL 1}}, Abstract = {{THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1 sr) with 0.5-1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift similar to 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late `20s/early `30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA). (C) 2018 COSPAR. Published by Elsevier Ltd. All rights reserved.}}, DOI = {{10.1016/j.asr.2018.03.010}}, ISSN = {{0273-1177}}, EISSN = {{1879-1948}}, ResearcherID-Numbers = {{Fiorini, Massimiliano/A-5354-2015 Harms, Jan/O-7967-2019 Vercellone, Stefano/ABC-7250-2020 Malcovati, Piero/S-2458-2016 Botticella, Maria Teresa/AAJ-9694-2020 van Putten, Maurice/R-3171-2019 Piedipalumbo, Ester/AAB-9195-2020 Bernardini, Maria Grazia/ABD-6115-2020 Orlandini, Mauro/H-3114-2014 Zhang, Bing/AAG-2824-2019 Campana, Sergio/AAL-6012-2020 Bertuccio, Giuseppe/AAA-7455-2020 Ryde, Felix/AAE-1086-2021 Rosati, Piero/ABI-7507-2020 ANTONELLI, ANTONELLA/C-6238-2011 Hernanz, Margarita/K-1770-2014 Nicastro, Luciano/F-5866-2015 Piedipalumbo, Ester/N-8824-2019 Uslenghi, Michela/ABA-8346-2020 Boer, Michel/Q-4428-2019 Lyutikov, Maxim/AAX-1992-2020 Izzo, Luca/AAH-9609-2019 Orleanski, Piotr/D-7277-2018 Vanzella, Eros/AAA-8640-2019 Braga, Joao/M-7493-2014 Kaneko, Yuki/V-2908-2019 Valle, Massimo Della/AAE-8884-2021 De Pasquale, Massimiliano/AAC-5695-2020 Grado, Aniello/AAA-1535-2019 Campana, Riccardo/F-5272-2015 Capozziello, Salvatore/AAA-6859-2019 Szecsi, Dorottya/N-7790-2019 Troja, Eleonora/AAB-3604-2020 Drago, Alessandro/F-6347-2012 Amati, Lorenzo/N-5586-2015 Comastri, Andrea/O-9543-2015 Rossi, Andrea/N-4674-2015 giommi, paolo/L-1006-2018 Piro, Luigi/E-4954-2013 Fynbo, Johan/L-8496-2014 Vacchi, Andrea/C-1291-2010 STRATTA, Maria Giuliana/L-3045-2016 Frontera, Filippo/B-4410-2014 de Martino, Domitilla/E-9567-2019 Gendre, Bruce/O-2923-2013 Ettori, Stefano/N-5004-2015 }}, ORCID-Numbers = {{Fiorini, Massimiliano/0000-0001-6559-2084 Harms, Jan/0000-0002-7332-9806 Vercellone, Stefano/0000-0003-1163-1396 Malcovati, Piero/0000-0001-6514-9672 Botticella, Maria Teresa/0000-0002-3938-692X Bernardini, Maria Grazia/0000-0001-6106-3046 Orlandini, Mauro/0000-0003-0946-3151 Campana, Sergio/0000-0001-6278-1576 Bertuccio, Giuseppe/0000-0002-7283-021X Hernanz, Margarita/0000-0002-8651-7910 Nicastro, Luciano/0000-0001-8534-6788 Boer, Michel/0000-0001-9157-4349 Orleanski, Piotr/0000-0003-3409-0692 Braga, Joao/0000-0003-3338-3186 Kaneko, Yuki/0000-0002-1861-5703 Valle, Massimo Della/0000-0003-3142-5020 Grado, Aniello/0000-0002-0501-8256 Campana, Riccardo/0000-0002-4794-5453 Capozziello, Salvatore/0000-0003-4886-2024 Szecsi, Dorottya/0000-0001-6473-7085 Troja, Eleonora/0000-0002-1869-7817 Tagliaferri, Gianpiero/0000-0003-0121-0723 Malaguti, Giuseppe/0000-0001-9872-3378 Martin Carrillo, Antonio/0000-0001-5108-0627 Amati, Lorenzo/0000-0001-5355-7388 Antonelli, Lucio Angelo/0000-0002-5037-9034 MacFadyen, Andrew/0000-0002-0106-9013 Ghirlanda, Giancarlo/0000-0001-5876-9259 Comastri, Andrea/0000-0003-3451-9970 Brandt, Soren/0000-0001-5689-3109 Salvaterra, Ruben/0000-0002-9393-8078 Brocato, Enzo/0000-0001-7988-8177 Rossi, Andrea/0000-0002-8860-6538 Bulgarelli, Andrea/0000-0001-6347-0649 Vanzella, Eros/0000-0002-5057-135X Morgante, Gianluca/0000-0001-9234-7412 giommi, paolo/0000-0002-2265-5003 O'Brien, Paul/0000-0002-5128-1899 Masetti, Nicola/0000-0001-9487-7740 Argan, Andrea/0000-0002-6230-665X Piro, Luigi/0000-0003-4159-3984 Greiner, Jochen/0000-0002-9875-426X Evangelista, Yuri/0000-0001-6096-6710 Mignani, Roberto/0000-0002-8685-583X MEREGHETTI, SANDRO/0000-0003-3259-7801 Capitanio, Fiamma/0000-0002-6384-3027 Finelli, Fabio/0000-0002-6694-3269 Santangelo, Andrea/0000-0003-4187-9560 Burderi, Luciano/0000-0001-5458-891X Pareschi, Giovanni/0000-0003-3967-403X Caruana, Joseph/0000-0002-6089-0768 RAZZANO, MASSIMILIANO/0000-0003-4825-1629 Fynbo, Johan/0000-0002-8149-8298 Labanti, Claudio/0000-0002-5086-3619 Panessa, Francesca/0000-0003-0543-3617 Ghisellini, Gabriele/0000-0002-0037-1974 Pian, Elena/0000-0001-8646-4858 Del Monte, Ettore/0000-0002-3013-6334 Covino, Stefano/0000-0001-9078-5507 Valenziano, Luca/0000-0002-1170-0104 D'Avanzo, Paolo/0000-0001-7164-1508 Vacchi, Andrea/0000-0003-3855-5856 STRATTA, Maria Giuliana/0000-0003-1055-7980 Basak, Rupal/0000-0001-5488-7258 Israel, GianLuca/0000-0001-5480-6438 Feroci, Marco/0000-0002-7617-3421 Dadina, Mauro/0000-0002-7858-7564 Frontera, Filippo/0000-0003-2284-571X Pascal, Chardonnet/0000-0002-4049-8582 D'Elia, Valerio/0000-0002-7320-5862 Ciolfi, Riccardo/0000-0003-3140-8933 Casella, Piergiorgio/0000-0002-0752-3301 sguera, vito/0000-0001-8202-9381 de Martino, Domitilla/0000-0002-5069-4202 Fiorini, Mauro/0000-0001-8297-1983 Lu, F.J./0000-0003-3248-6087 Palazzi, Eliana/0000-0002-8691-7666 Izzo, Luca/0000-0001-9695-8472 Melandri, Andrea/0000-0002-2810-2143 Kuvvetli, Irfan/0000-0001-8749-4274 Paizis, Adamantia/0000-0001-5067-0377 Schady, Patricia/0000-0002-1214-770X Gendre, Bruce/0000-0002-9077-2025 De Luca, Andrea/0000-0001-6739-687X Maiorano, Elisabetta/0000-0003-2593-4355 Romano, Patrizia/0000-0003-0258-7469 Ettori, Stefano/0000-0003-4117-8617 Uslenghi, Michela/0000-0002-7585-8605}}, Unique-ID = {{ISI:000436889000016}}, } @article{ ISI:000436629300001, Author = {Chan, Man Leong and Messenger, Chris and Heng, Ik Siong and Hendry, Martin}, Title = {{Binary neutron star mergers and third generation detectors: Localization and early warning}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{97}}, Number = {{12}}, Month = {{JUN 28}}, Abstract = {{For third generation gravitational wave detectors, such as the Einstein Telescope, gravitational wave signals from binary neutron stars can last up to a few days before the neutron stars merge. To estimate the measurement uncertainties of key signal parameters, we develop a Fisher matrix approach which accounts for effects on such long duration signals of the time-dependent detector response and the Earth's rotation. We use this approach to characterize the sky localization uncertainty for gravitational waves from binary neutron stars at 40, 200, 400, 800, and 1600 Mpc, for the Einstein Telescope and Cosmic Explorer individually and operating as a network. We find that the Einstein Telescope alone can localize the majority of detectable binary neutron stars at a distance of <= 200 Mpc to within 100 deg(2) with 90\% confidence. A network consisting of the Einstein Telescope and Cosmic Explorer can enhance the sky localization performance significantly-with the 90\% credible region of O(1) deg(2) for most sources at <= 200 Mpc and <= 100 deg(2) for most sources at <= 1600 Mpc. We also investigate the prospects for third generation detectors identifying the presence of a signal prior to merger. To do this, we require a signal to have a network signal-to-noise ratio of >= 12 and >= 5.5 for at least two interferometers, and to have a 90\% credible region for the sky localization that is no larger than 100 deg(2). We find that the Einstein Telescope can send out such ``earlywarning{''} detection alerts 1-20 hours before merger for 100\% of detectable binary neutron stars at 40 Mpc and for similar to 58\% of sources at 200 Mpc. For sources at a distance of 400 Mpc, a network of the Einstein telescope and Cosmic Explorer can produce detection alerts up to similar to 3 hours prior to merger for 98\% of detectable binary neutron stars.}}, DOI = {{10.1103/PhysRevD.97.123014}}, Article-Number = {{123014}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Messenger, Chris/0000-0001-7488-5022}}, Unique-ID = {{ISI:000436629300001}}, } @article{ ISI:000434937000003, Author = {Shandera, Sarah and Jeong, Donghui and Gebhardt, Henry S. Grasshorn}, Title = {{Gravitational Waves from Binary Mergers of Subsolar Mass Dark Black Holes}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2018}}, Volume = {{120}}, Number = {{24}}, Month = {{JUN 12}}, Abstract = {{We explore the possible spectrum of binary mergers of subsolar mass black holes formed out of dark matter particles interacting via a dark electromagnetism. We estimate the properties of these dark black holes by assuming that their formation process is parallel to Population-III star formation, except that dark molecular cooling can yield a smaller opacity limit. We estimate the binary coalescence rates for the Advanced LIGO and Einstein telescope, and find that scenarios compatible with all current constraints could produce dark black holes at rates high enough for detection by Advanced LIGO.}}, DOI = {{10.1103/PhysRevLett.120.241102}}, Article-Number = {{241102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ORCID-Numbers = {{Grasshorn Gebhardt, Henry/0000-0002-8158-0523 Jeong, Donghui/0000-0002-8434-979X}}, Unique-ID = {{ISI:000434937000003}}, } @article{ ISI:000433913000005, Author = {Belgacem, Enis and Dirian, Yves and Foffa, Stefano and Maggiore, Michele}, Title = {{Gravitational-wave luminosity distance in modified gravity theories}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{97}}, Number = {{10}}, Month = {{MAY 31}}, Abstract = {{In modified gravity the propagation of gravitational waves (GWs) is in general different from that in general relativity. As a result, the luminosity distance for GWs can differ from that for electromagnetic signals, and is affected both by the dark energy equation of state w(DE)(z) and by a function delta(z) describing modified propagation. We show that the effect of modified propagation in general dominates over the effect of the dark energy equation of state, making it easier to distinguish a modified gravity model from.CDM. We illustrate this using a nonlocal modification of gravity that has been shown to fit remarkably well cosmic microwave background, supernovae, baryon acoustic oscillation, and structure formation data, and we discuss the prospects for distinguishing nonlocal gravity from Lambda CDM with the Einstein Telescope. We find that, depending on the exact sensitivity, a few tens of standard sirens with measured redshift at z similar to 0.4, or a few hundreds at 1 <= z <= 2, could suffice.}}, DOI = {{10.1103/PhysRevD.97.104066}}, Article-Number = {{104066}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Maggiore, Michele/0000-0001-7348-047X}}, Unique-ID = {{ISI:000433913000005}}, } @article{ ISI:000432965900001, Author = {Cai, Rong-Gen and Liu, Tong-Bo and Liu, Xue-Wen and Wang, Shao-Jiang and Yang, Tao}, Title = {{Probing cosmic anisotropy with gravitational waves as standard sirens}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{97}}, Number = {{10}}, Month = {{MAY 4}}, Abstract = {{The gravitational wave (GW) as a standard siren directly determines the luminosity distance from the gravitational waveform without reference to the specific cosmological model, of which the redshift can be obtained separately by means of the electromagnetic counterpart like GW events from binary neutron stars and massive black hole binaries (MBEIBs). To see to what extent the standard siren can reproduce the presumed dipole anisotropy written in the simulated data of standard siren events from typical configurations of GW detectors, we find that (1) for the Laser Interferometer Space Antenna with different MBHB models during five-year observations, the cosmic isotropy can be ruled out at 3 sigma confidence level (C.L.) and the dipole direction can be constrained roughly around 20\% at 2 sigma C.L., as long as the dipole amplitude is larger than 0.04, 0.06 and 0.03 for MBHB models Q3d, pop III and Q3nod with increasing constraining ability, respectively; (2) for the Einstein telescope with no less than 200 standard siren events, the cosmic isotropy can be ruled out at 3 sigma C.L. if the dipole amplitude is larger than 0.06, and the dipole direction can be constrained within 20\% at 3 sigma C.L. if the dipole amplitude is near 0.1; (3) for the Deci-Hertz Interferometer Gravitational wave Observatory with no less than 100 standard siren events, the cosmic isotropy can be ruled out at 3 sigma C.L. for dipole amplitude larger than 0.03, and the dipole direction can even be constrained within 10\% at 3 sigma C.L. if the dipole amplitude is larger than 0.07. Our work manifests the promising perspective of the constraint ability on the cosmic anisotropy from the standard siren approach.}}, DOI = {{10.1103/PhysRevD.97.103005}}, Article-Number = {{103005}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Wang, Shao-Jiang/AAJ-8844-2020 }}, ORCID-Numbers = {{Wang, Shao-Jiang/0000-0003-4378-870X Yang, Tao/0000-0002-2161-0495}}, Unique-ID = {{ISI:000432965900001}}, } @article{ ISI:000430940900058, Author = {Li, Shun-Sheng and Mao, Shude and Zhao, Yuetong and Lu, Youjun}, Title = {{Gravitational lensing of gravitational waves: a statistical perspective}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2018}}, Volume = {{476}}, Number = {{2}}, Pages = {{2220-2229}}, Month = {{MAY}}, Abstract = {{In this paper, we study the strong gravitational lensing of gravitational waves (GWs) from a statistical perspective, with particular focus on the high frequency GWs from stellar binary black hole coalescences. These are most promising targets for ground-based detectors such as Advanced Laser Interferometer Gravitational Wave Observatory (aLIGO) and the proposed Einstein Telescope (ET) and can be safely treated under the geometrical optics limit for GW propagation. We perform a thorough calculation of the lensing rate, by taking account of effects caused by the ellipticity of lensing galaxies, lens environments, and magnification bias. We find that in certain GW source rate scenarios, we should be able to observe strongly lensed GW events once per year (similar to 1 yr(-1)) in the aLIGO survey at its design sensitivity; for the proposed ET survey, the rate could be as high as similar to 80 yr(-1). These results depend on the estimate of GW source abundance, and hence can be correspondingly modified with an improvement in our understanding of the merger rate of stellar binary black holes. We also compute the fraction of four-image lens systems in each survey, predicting it to be similar to 30 per cent for the aLIGO survey and similar to 6 per cent for the ET survey. Finally, we evaluate the possibility of missing some images due to the finite survey duration, by presenting the probability distribution of lensing time delays. We predict that this selection bias will be insignificant in future GW surveys, as most of the lens systems (similar to 90 per cent) will have time delays less than similar to 1 month, which will be far shorter than survey durations.}}, DOI = {{10.1093/mnras/sty411}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ORCID-Numbers = {{Li, Shun-Sheng/0000-0001-9952-7408}}, Unique-ID = {{ISI:000430940900058}}, } @article{ ISI:000428685000005, Author = {Fragione, Giacomo and Ginsburg, Idan and Kocsis, Bence}, Title = {{Gravitational Waves and Intermediate-mass Black Hole Retention in Globular Clusters}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2018}}, Volume = {{856}}, Number = {{2}}, Month = {{APR 1}}, Abstract = {{The recent discovery of gravitational waves (GWs) has opened new horizons for physics. Current and upcoming missions, such as LIGO, VIRGO, KAGRA, and LISA, promise to shed light on black holes of every size from stellar mass (SBH) sizes up to supermassive black holes. The intermediate-mass black hole (IMBH) family has not been detected beyond any reasonable doubt. Recent analyses suggest observational evidence for the presence of IMBHs in the centers of two Galactic globular clusters (GCs). In this paper, we investigate the possibility that GCs were born with a central IMBH, which undergoes repeated merger events with SBHs in the cluster core. By means of a semi-analytical method, we follow the evolution of the primordial cluster population in the galactic potential and the mergers of the binary IMBH-SBH systems. Our models predict approximate to 1000 IMBHs within 1 kpc from the galactic center and show that the IMBH-SBH merger rate density changes from R approximate to 1000 Gpc(-3) yr(-1) beyond z approximate to 2 to R approximate to 1-10 Gpc(-3) yr(-1) at z approximate to 0. The rates at low redshifts may be significantly higher if young massive star clusters host IMBHs. The merger rates are dominated by IMBHs with masses between 10(3) and 10(4) M-circle dot. Currently, there are no LIGO/VIRGO upper limits for GW sources in this mass range, but our results show that at design sensitivity, these instruments will detect IMBH-SBH mergers in the coming years. LISA and the Einstein Telescope will be best suited to detect these events. The inspirals of IMBH-SBH systems may also generate an unresolved GW background.}}, DOI = {{10.3847/1538-4357/aab368}}, Article-Number = {{92}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Kocsis, Bence/AAX-1181-2020 Kocsis, Bence/C-3061-2013 Fragione, Giacomo/ABC-2055-2020}}, ORCID-Numbers = {{Kocsis, Bence/0000-0002-4865-7517 Kocsis, Bence/0000-0002-4865-7517 }}, Unique-ID = {{ISI:000428685000005}}, } @article{ ISI:000428241300006, Author = {Zhao, Wen and Wen, Linqing}, Title = {{Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{97}}, Number = {{6}}, Month = {{MAR 26}}, Abstract = {{We use the Fisher information matrix to investigate the angular resolution and luminosity distance uncertainty for coalescing binary neutron stars (BNSs) and neutron star-black hole binaries (NSBHs) detected by the third-generation (3G) gravitational-wave (GW) detectors. Our study focuses on an individual 3G detector and a network of up to four 3G detectors at different locations including the United States, Europe, China, and Australia for the proposed Einstein Telescope (ET) and Cosmic Explorer (CE) detectors. In particular, we examine the effect of the Earth's rotation, as GW signals from BNS and low-mass NSBH systems could be hours long for 3G detectors. In this case, an individual detector can be effectively treated as a detector network with long baselines formed by the trajectory of the detector as it rotates with the Earth. Therefore, a single detector or two-detector networks could also be used to localize the GW sources effectively. We find that a time-dependent antenna beam-pattern function can help better localize BNS and NSBH sources, especially edge-on ones. The medium angular resolution for one ET-D detector is around 150 deg(2) for BNSs at a redshift of z = 0.1, which improves rapidly with a decreasing low-frequency cutoff f(low) in sensitivity. The medium angular resolution for a network of two CE detectors in the United States and Europe, respectively, is around 20 deg(2) at z = 0.2 for the simulated BNS and NSBH samples. While for a network of two ET-D detectors, the similar angular resolution can be achieved at a much higher redshift of z = 0.5. The angular resolution of a network of three detectors is mainly determined by the baselines between detectors regardless of the CE or ET detector type. The medium angular resolution of BNS for a network of three detectors of the ET-D or CE type in the United States, Europe, and Australia is around 10 deg(2) at z = 2. We discuss the implications of our results for multimessenger astronomy and, in particular, for using GW sources as independent tools to constrain the Hubble constant H-0, the deceleration parameter q(0), and the equation-of-state (EoS) of dark energy. We find that, in general, if 10 BNSs or NSBHs at z = 0.1 with known redshifts are detected by 3G networks consisting of two ET-like detectors, H-0 can be measured with an accuracy of 0.9\%. If 1000 face-on BNSs at z < 2 are detected with known redshifts, we are able to achieve Delta q(0) = 0.002 for the deceleration parameter, or Delta w(0) = 0.03 and Delta w(a) = 0.2 for EoS of dark energy, respectively.}}, DOI = {{10.1103/PhysRevD.97.064031}}, Article-Number = {{064031}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Wen, Linqing/0000-0001-7987-295X Zhao, Wen/0000-0002-1330-2329}}, Unique-ID = {{ISI:000428241300006}}, } @article{ ISI:000430617800009, Author = {Van den Brand, Jo}, Title = {{Gravitational Waves: Physics at the Extreme}}, Journal = {{EUROPEAN REVIEW}}, Year = {{2018}}, Volume = {{26}}, Number = {{1}}, Pages = {{90-99}}, Month = {{FEB}}, Abstract = {{Last year, the LIGO Scientific Collaboration and the Virgo Collaboration announced the first detection of a gravitational wave. A century after the fundamental predictions of Einstein, the first direct observation of a binary black hole system merging to form a single black hole was made. The observations provide unique access to the properties of spacetime at extreme curvatures: the strong-field and high-velocity regime. It allows unprecedented tests of general relativity for the nonlinear dynamics of highly disturbed black holes. LIGO and Virgo realized a global interferometer network, and more detections were made, including a signal from a binary neutron star merger. The scientific impact of the various detections will be explained. In addition, key technological aspects will be addressed, such as the interferometric detection principle, optics, as well as sensors and actuators. Attention is paid to Advanced Virgo, the European detector near Pisa, which came online in 2017. We end with a discussion of the largest challenges in the field, including plans for the Einstein Telescope, a large underground observatory for gravitational-wave science.}}, DOI = {{10.1017/S1062798717000801}}, ISSN = {{1062-7987}}, EISSN = {{1474-0575}}, ORCID-Numbers = {{van den Brand, Johannes/0000-0003-4434-5353}}, Unique-ID = {{ISI:000430617800009}}, } @article{ ISI:000423434600018, Author = {Yang, Huan and Paschalidis, Vasileios and Yagi, Kent and Lehner, Luis and Pretorius, Frans and Yunes, Nicolas}, Title = {{Gravitational wave spectroscopy of binary neutron star merger remnants with mode stacking}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2018}}, Volume = {{97}}, Number = {{2}}, Month = {{JAN 29}}, Abstract = {{A binary neutron star coalescence event has recently been observed for the first time in gravitational waves, and many more detections are expected once current ground-based detectors begin operating at design sensitivity. As in the case of binary black holes, gravitational waves generated by binary neutron stars consist of inspiral, merger, and postmerger components. Detecting the latter is important because it encodes information about the nuclear equation of state in a regime that cannot be probed prior to merger. The postmerger signal, however, can only be expected to be measurable by current detectors for events closer than roughly ten megaparsecs, which given merger rate estimates implies a low probability of observation within the expected lifetime of these detectors. We carry out Monte Carlo simulations showing that the dominant postmerger signal (the l = m = 2 mode) from individual binary neutron star mergers may not have a good chance of observation even with the most sensitive future ground-based gravitational wave detectors proposed so far (the Einstein Telescope and Cosmic Explorer, for certain equations of state, assuming a full year of operation, the latest merger rates, and a detection threshold corresponding to a signal-to-noise ratio of 5). For this reason, we propose two methods that stack the postmerger signal from multiple binary neutron star observations to boost the postmerger detection probability. The first method follows a commonly used practice of multiplying the Bayes factors of individual events. The second method relies on an assumption that the mode phase can be determined from the inspiral waveform, so that coherent mode stacking of the data from different events becomes possible. We find that both methods significantly improve the chances of detecting the dominant postmerger signal, making a detection very likely after a year of observation with Cosmic Explorer for certain equations of state. We also show that in terms of detection, coherent stacking is more efficient in accumulating confidence for the presence of postmerger oscillations in a signal than the first method. Moreover, assuming the postmerger signal is detected with Cosmic Explorer via stacking, we estimate through a Fisher analysis that the peak frequency can be measured to a statistical error of similar to 4-20 Hz for certain equations of state. Such an error corresponds to a neutron star radius measurement to within similar to 15-56 m, a fractional relative error similar to 4\%, suggesting that systematic errors from theoretical modeling greater than or similar to 100 m) may dominate the error budget.}}, DOI = {{10.1103/PhysRevD.97.024049}}, Article-Number = {{024049}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Yunes, Nicolas/AAG-3146-2019 }}, ORCID-Numbers = {{Yunes, Nicolas/0000-0001-6147-1736 Paschalidis, Vasileios/0000-0002-8099-9023}}, Unique-ID = {{ISI:000423434600018}}, } @article{ ISI:000423131700003, Author = {Bose, Sukanta and Chakravarti, Kabir and Rezzolla, Luciano and Sathyaprakash, B. S. and Takami, Kentaro}, Title = {{Neutron-Star Radius from a Population of Binary Neutron Star Mergers}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2018}}, Volume = {{120}}, Number = {{3}}, Month = {{JAN 16}}, Abstract = {{We show how gravitational-wave observations with advanced detectors of tens to several tens of neutron-star binaries can measure the neutron-star radius with an accuracy of several to a few percent, for mass and spatial distributions that are realistic, and with none of the sources located within 100 Mpc. We achieve such an accuracy by combining measurements of the total mass from the inspiral phase with those of the compactness from the postmerger oscillation frequencies. For estimating the measurement errors of these frequencies, we utilize analytical fits to postmerger numerical relativity waveforms in the time domain, obtained here for the first time, for four nuclear-physics equations of state and a couple of values for the mass. We further exploit quasiuniversal relations to derive errors in compactness from those frequencies. Measuring the average radius to well within 10\% is possible for a sample of 100 binaries distributed uniformly in volume between 100 and 300 Mpc, so long as the equation of state is not too soft or the binaries are not too heavy. We also give error estimates for the Einstein Telescope.}}, DOI = {{10.1103/PhysRevLett.120.031102}}, Article-Number = {{031102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014 }}, ORCID-Numbers = {{Sathyaprakash, Bangalore/0000-0003-3845-7586 Bose, Sukanta/0000-0002-4151-1347}}, Unique-ID = {{ISI:000423131700003}}, } @inproceedings{ ISI:000452819200058, Author = {Tatischeff, V. and De Angelis, A. and Tavani, M. and Grenier, I. and Oberlack, U. and Hanlon, L. and Walter, R. and Argan, A. and von Ballmoos, P. and Bulgarelli, A. and Donnarumma, I. and Hernanz, M. and Kuvvetli, I. and Mallamaci, M. and Pearce, M. and Zdziarski, A. and Aboudan, A. and Ajello, M. and Ambrosi, G. and Bernard, D. and Bernardini, E. and Bonvicini, V. and Brogna, A. and Branchesi, M. and Budtz-Jorgensen, C. and Bykov, A. and Campana, R. and Cardillo, M. and Ciprini, S. and Coppi, P. and Cumani, P. and da Silva, R. M. Curado and De Martino, D. and Diehl, R. and Doro, M. and Fioretti, V. and Funk, S. and Ghisellini, G. and Giordano, F. and Grove, J. E. and Hamadache, C. and Hartmann, D. H. and Hayashida, M. and Isern, J. and Kanbach, G. and Kiener, J. and Knodlseder, J. and Labanti, C. and Laurent, P. and Leising, M. and Limousin, O. and Longo, F. and Mannheim, K. and Marisaldi, M. and Martinez, M. and Mazziotta, M. N. and McEnery, J. E. and Mereghetti, S. and Minervini, G. and Moiseev, A. and Morselli, A. and Nakazawa, K. and Orleanski, P. and Paredes, J. M. and Patricelli, B. and Peyre, J. and Piano, G. and Pohl, M. and Rando, R. and Roncadelli, M. and Tavecchio, F. and Thompson, D. J. and Turolla, R. and Ulyanov, A. and Vacchi, A. and Wu, X. and Zoglauer, A.}, Editor = {{DenHerder, JWA and Nikzad, S and Nakazawa, K}}, Title = {{The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s}}, Booktitle = {{SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY}}, Series = {{Proceedings of SPIE}}, Year = {{2018}}, Volume = {{10699}}, Note = {{Conference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray, Austin, TX, JUN 10-15, 2018}}, Organization = {{SPIE; 4D Technol; Andor Technol Ltd; Astron Consultants \& Equipment, Inc; Giant Magellan Telescope; GPixel, Inc; Harris Corp; Mater Corp; Optimax Syst, Inc; Princeton Infrared Technologies; Symetrie; Teledyne Technologies Inc; Thirty Meter Telescope}}, Abstract = {{e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array.}}, DOI = {{10.1117/12.2315151}}, Article-Number = {{UNSP 106992J}}, ISSN = {{0277-786X}}, EISSN = {{1996-756X}}, ISBN = {{978-1-5106-1952-4}}, ResearcherID-Numbers = {{Funk, Stefan/B-7629-2015 Pohl, Martin/P-4920-2017 da Silva, Rui M Curado/A-3425-2013 Hernanz, Margarita/K-1770-2014 Fioretti, Valentina/N-5589-2015 MALLAMACI, MANUELA/AAA-5598-2020 Orleanski, Piotr/D-7277-2018 Morselli, Aldo/G-6769-2011 Campana, Riccardo/F-5272-2015 Bernardini, Elisa/AAA-4810-2020 Oberlack, Uwe/AAP-4464-2020 Bykov, Andrei/E-3131-2014 Vacchi, Andrea/C-1291-2010 de Martino, Domitilla/E-9567-2019 }}, ORCID-Numbers = {{Funk, Stefan/0000-0002-2012-0080 Pohl, Martin/0000-0001-7861-1707 da Silva, Rui M Curado/0000-0002-9961-965X Hernanz, Margarita/0000-0002-8651-7910 Fioretti, Valentina/0000-0002-6082-5384 MALLAMACI, MANUELA/0000-0003-4068-0496 Orleanski, Piotr/0000-0003-3409-0692 Morselli, Aldo/0000-0002-7704-9553 Campana, Riccardo/0000-0002-4794-5453 Bernardini, Elisa/0000-0003-3108-1141 TUROLLA, ROBERTO/0000-0002-5825-8149 Piano, Giovanni/0000-0002-9332-5319 Ciprini, Stefano/0000-0002-0712-2479 Kuvvetli, Irfan/0000-0001-8749-4274 Vacchi, Andrea/0000-0003-3855-5856 Ghisellini, Gabriele/0000-0002-0037-1974 Tavecchio, Fabrizio/0000-0003-0256-0995 Labanti, Claudio/0000-0002-5086-3619 Cumani, Paolo/0000-0001-9322-8298 Paredes, Josep M./0000-0002-1566-9044 MEREGHETTI, SANDRO/0000-0003-3259-7801 de Martino, Domitilla/0000-0002-5069-4202 Aboudan, Alessio/0000-0002-8290-2184 Bulgarelli, Andrea/0000-0001-6347-0649 Grenier, Isabelle/0000-0003-3274-674X Argan, Andrea/0000-0002-6230-665X Coppi, Paolo/0000-0001-9604-2325 Cardillo, Martina/0000-0001-8877-3996 von Ballmoos, Peter/0000-0002-0917-3392}}, Unique-ID = {{ISI:000452819200058}}, } @article{ ISI:000415297500010, Author = {Liu, Tong and Lin, Chao-Yang and Song, Cui-Ying and Li, Ang}, Title = {{Comparison of Gravitational Waves from Central Engines of Gamma-Ray Bursts: Neutrino-dominated Accretion Flows, Blandford-Znajek Mechanisms, and Millisecond Magnetars}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2017}}, Volume = {{850}}, Number = {{1}}, Month = {{NOV 20}}, Abstract = {{Neutrino-dominated accretion flow (NDAF) around a rotating stellar-mass black hole (BH) is one of the plausible candidates for the central engines of gamma-ray bursts (GRBs). Because the time-variant and anisotropic emission of neutrinos from NDAFs leads to GRB variability, NDAFs can be regarded as the sources of strong gravitational waves (GWs). We calculate the dependences of the GW strains on both the BH spin and the accretion rate. We demonstrate that, for typical GRBs with either a single pulse or multiple pulses, the GWs from NDAFs might be detected at a distance of similar to 100 kpc/similar to 1 Mpc by the advanced LIGO/Einstein Telescope with a typical frequency of similar to 10-100 Hz. Besides NDAFs, the other two competitive candidates for the GRB central engine are the Blandford-Znajek (BZ) mechanism and millisecond magnetars. We explore the GW signals from these two as well, and compare the corresponding results with NDAFs'. We find that for a certain GRB, the possible detected distance from NDAFs is about two orders of magnitude higher than that from the BZ mechanism, but at least two orders of magnitude lower than that from magnetars. The typical GW frequency for the BZ mechanism is the same as that of NDAFs, similar to 10-100 Hz, while the typical frequency for magnetars is similar to 2000 Hz. Therefore, the GWs released by the central engines of adjacent GRBs might be used to determine whether there is an NDAF, a BZ jet, or a magnetar in the GRB center.}}, DOI = {{10.3847/1538-4357/aa92c4}}, Article-Number = {{30}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Liu, Tong/U-3225-2019 liu, tong/C-4841-2014 Li, Ang/G-3957-2010 }}, ORCID-Numbers = {{Li, Ang/0000-0001-9849-3656 Song, Cui-Ying/0000-0001-8390-9962 Liu, Tong/0000-0001-8678-6291}}, Unique-ID = {{ISI:000415297500010}}, } @article{ ISI:000415600400008, Author = {Samajdar, Anuradha and Arun, K. G.}, Title = {{Projected constraints on the dispersion of gravitational waves using advanced ground- and space-based interferometers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{96}}, Number = {{10}}, Month = {{NOV 17}}, Abstract = {{Certain alternative theories of gravity predict that gravitational waves will disperse as they travel from the source to the observer. The recent binary black hole observations by Advanced-LIGO have set limits on a modified dispersion relation from the constraints on their effects on gravitational-wave propagation. Using an identical modified dispersion, of the form E2 = p(2)c(2) + Ap(alpha)c(alpha), where A denotes the magnitude of dispersion and E and p are the energy and momentum of the gravitational wave, we estimate the projected constraints on the modified dispersion from observations of compact binary mergers by third-generation ground-based detectors such as the Einstein Telescope and Cosmic Explorer as well as the space-based detector Laser Interferometer Space Antenna. We find that third-generation detectors would bound dispersion of gravitational waves much better than their second-generation counterparts. The Laser Interferometer Space Antenna, with its extremely good low-frequency sensitivity, would place stronger constraints than the ground-based detectors for alpha <= 1, whereas for alpha > 1, the bounds are weaker. We also study the effect of the spins of the compact binary constituents on the bounds.}}, DOI = {{10.1103/PhysRevD.96.104027}}, Article-Number = {{104027}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000415600400008}}, } @article{ ISI:000413832800003, Author = {Liao, Kai and Fan, Xi-Long and Ding, Xuheng and Biesiada, Marek and Zhu, Zong-Hong}, Title = {{Precision cosmology from future lensed gravitational wave and electromagnetic signals}}, Journal = {{NATURE COMMUNICATIONS}}, Year = {{2017}}, Volume = {{8}}, Month = {{OCT 27}}, Abstract = {{The standard siren approach of gravitational wave cosmology appeals to the direct luminosity distance estimation through the waveform signals from inspiralling double compact binaries, especially those with electromagnetic counterparts providing redshifts. It is limited by the calibration uncertainties in strain amplitude and relies on the fine details of the waveform. The Einstein telescope is expected to produce 104-105 gravitational wave detections per year, 50-100 of which will be lensed. Here, we report a waveform-independent strategy to achieve precise cosmography by combining the accurately measured time delays from strongly lensed gravitational wave signals with the images and redshifts observed in the electromagnetic domain. We demonstrate that just 10 such systems can provide a Hubble constant uncertainty of 0.68\% for a flat lambda cold dark matter universe in the era of third-generation ground-based detectors.}}, DOI = {{10.1038/s41467-017-01152-9}}, Article-Number = {{1148}}, ISSN = {{2041-1723}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Fan, Xilong/0000-0002-8174-0128 Ding, Xuheng/0000-0001-8917-2148}}, Unique-ID = {{ISI:000413832800003}}, } @article{ ISI:000413850800004, Author = {Shao, Lijing and Sennett, Noah and Buonanno, Alessandra and Kramer, Michael and Wex, Norbert}, Title = {{Constraining Nonperturbative Strong-Field Effects in Scalar-Tensor Gravity by Combining Pulsar Timing and Laser-Interferometer Gravitational-Wave Detectors}}, Journal = {{PHYSICAL REVIEW X}}, Year = {{2017}}, Volume = {{7}}, Number = {{4}}, Month = {{OCT 27}}, Abstract = {{Pulsar timing and laser-interferometer gravitational-wave (GW) detectors are superb laboratories to study gravity theories in the strong-field regime. Here, we combine these tools to test the mono-scalar-tensor theory of Damour and Esposito-Farese (DEF), which predicts nonperturbative scalarization phenomena for neutron stars (NSs). First, applying Markov-chain Monte Carlo techniques, we use the absence of dipolar radiation in the pulsar-timing observations of five binary systems composed of a NS and a white dwarf, and eleven equations of state (EOSs) for NSs, to derive the most stringent constraints on the two free parameters of the DEF scalar-tensor theory. Since the binary-pulsar bounds depend on the NS mass and the EOS, we find that current pulsar-timing observations leave scalarization windows, i.e., regions of parameter space where scalarization can still be prominent. Then, we investigate if these scalarization windows could be closed and if pulsar-timing constraints could be improved by laser-interferometer GW detectors, when spontaneous (or dynamical) scalarization sets in during the early (or late) stages of a binary NS (BNS) evolution. For the early inspiral of a BNS carrying constant scalar charge, we employ a Fisher-matrix analysis to show that Advanced LIGO can improve pulsar-timing constraints for some EOSs, and next-generation detectors, such as the Cosmic Explorer and Einstein Telescope, will be able to improve those bounds for all eleven EOSs. Using the late inspiral of a BNS, we estimate that for some of the EOSs under consideration, the onset of dynamical scalarization can happen early enough to improve the constraints on the DEF parameters obtained by combining the five binary pulsars. Thus, in the near future, the complementarity of pulsar timing and direct observations of GWs on the ground will be extremely valuable in probing gravity theories in the strong-field regime.}}, DOI = {{10.1103/PhysRevX.7.041025}}, Article-Number = {{041025}}, ISSN = {{2160-3308}}, ORCID-Numbers = {{Shao, Lijing/0000-0002-1334-8853 Kramer, Michael/0000-0002-4175-2271}}, Unique-ID = {{ISI:000413850800004}}, } @article{ ISI:000413169300004, Author = {Chamberlain, Katie and Yunes, Nicolas}, Title = {{Theoretical physics implications of gravitational wave observation with future detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{96}}, Number = {{8}}, Month = {{OCT 18}}, Abstract = {{Gravitational waves encode invaluable information about the nature of the relatively unexplored extreme gravity regime, where the gravitational interaction is strong, nonlinear and highly dynamical. Recent gravitational wave observations by advanced LIGO have provided the first glimpses into this regime, allowing for the extraction of new inferences on different aspects of theoretical physics. For example, these detections provide constraints on the mass of the graviton, Lorentz violation in the gravitational sector, the existence of large extra dimensions, the temporal variability of Newton's gravitational constant, and modified dispersion relations of gravitational waves. Many of these constraints, however, are not yet competitive with constraints obtained, for example, through Solar System observations or binary pulsar observations. In this paper, we study the degree to which theoretical physics inferences drawn from gravitational wave observations will strengthen with detections from future detectors. We consider future ground-based detectors, such as the LIGO-class expansions A+, Voyager, Cosmic Explorer and the Einstein Telescope, as well as space-based detectors, such as various configurations of eLISA and the recently proposed LISA mission. We find that space-based detectors will place constraints on general relativity up to 12 orders of magnitude more stringently than current aLIGO bounds, but these space-based constraints are comparable to those obtained with the ground-based Cosmic Explorer or the Einstein Telescope (A+ and Voyager only lead to modest improvements in constraints). We also generically find that improvements in the instrument sensitivity band at low frequencies lead to large improvements in certain classes of constraints, while sensitivity improvements at high frequencies lead to more modest gains. These results strengthen the case for the development of future detectors, while providing additional information that could be useful in future design decisions.}}, DOI = {{10.1103/PhysRevD.96.084039}}, Article-Number = {{084039}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Yunes, Nicolas/AAG-3146-2019 }}, ORCID-Numbers = {{Yunes, Nicolas/0000-0001-6147-1736 Chamberlain, Katie/0000-0001-8765-8670}}, Unique-ID = {{ISI:000413169300004}}, } @article{ ISI:000406476400001, Author = {Gao, He and Cao, Zhoujian and Zhang, Bing}, Title = {{Magnetic-distortion-induced Ellipticity and Gravitational Wave Radiation of Neutron Stars: Millisecond Magnetars in Short GRBs, Galactic Pulsars, and Magnetars}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2017}}, Volume = {{844}}, Number = {{2}}, Month = {{AUG 1}}, Abstract = {{Neutron stars may sustain a non-axisymmetric deformation due to magnetic distortion and are potential sources of continuous gravitational waves (GWs) for ground-based interferometric detectors. With decades of searches using available GW detectors, no evidence of a GW signal from any pulsar has been observed. Progressively stringent upper limits of ellipticity have been placed on Galactic pulsars. In this work, we use the ellipticity inferred from the putative millisecond magnetars in short gamma-ray bursts (SGRBs) to estimate their detectability by current and future GW detectors. For similar to 1 ms magnetars inferred from the SGRB data, the detection horizon is similar to 30 Mpc and similar to 600 Mpc for the advanced LIGO (aLIGO) and Einstein Telescope (ET), respectively. Using the ellipticity of SGRB millisecond magnetars as calibration, we estimate the ellipticity and GW strain of Galactic pulsars and magnetars assuming that the ellipticity is magnetic-distortion-induced. We find that the results are consistent with the null detection results of Galactic pulsars and magnetars with the aLIGO O1. We further predict that the GW signals from these pulsars/magnetars may not be detectable by the currently designed aLIGO detector. The ET detector may be able to detect some relatively low-frequency signals (<50 Hz) from some of these pulsars. Limited by its design sensitivity, the eLISA detector seems to not be suitable for detecting the signals from Galactic pulsars and magnetars.}}, DOI = {{10.3847/1538-4357/aa7d00}}, Article-Number = {{112}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Cao, Zhoujian/AAH-2470-2020 Zhang, Bing/AAG-2824-2019}}, ORCID-Numbers = {{Cao, Zhoujian/0000-0002-1932-7295 }}, Unique-ID = {{ISI:000406476400001}}, } @article{ ISI:000406619100033, Author = {Wang, Jie-Shuang and Dai, Zi-Gao}, Title = {{Evolution of newborn rapidly rotating magnetars: Effects of R-mode and fall-back accretion}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2017}}, Volume = {{603}}, Month = {{JUL}}, Abstract = {{In this paper we investigate effects of the r-mode instability on a newborn rapidly-rotating magnetar with fall-back accretion. Such a magnetar could usually occur in core-collapse supernovae and gamma-ray bursts. We find that the magnetar's spin and r-mode evolution are influenced by accretion. If the magnetar is sufficiently spun up to a few milliseconds, gravitational radiation leads to the growth of the r-mode amplitude significantly. The maximum r-mode amplitude reaches an order of similar to 0.001 when the damping due to the growth of a toroidal magnetic field balances the growth of the r-mode amplitude. If such a sufficiently spun-up magnetar was located at a distance less than 1 Mpc, then gravitational waves would be detectable by the Einstein Telescope but would have an extremely low event rate. However, if the spin-up is insufficient, the growth of the r-mode amplitude is mainly due to the accretion torque. In this case, the maximum r-mode amplitude is of the order of similar to 10(-6)-10(-5).}}, DOI = {{10.1051/0004-6361/201629610}}, Article-Number = {{A9}}, ISSN = {{1432-0746}}, ORCID-Numbers = {{Wang, Jie-Shuang/0000-0002-2662-6912}}, Unique-ID = {{ISI:000406619100033}}, } @article{ ISI:000402399700006, Author = {Vinciguerra, Serena and Veitch, John and Mandel, Ilya}, Title = {{Accelerating gravitational wave parameter estimation with multi-band template interpolation}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2017}}, Volume = {{34}}, Number = {{11}}, Month = {{JUN 8}}, Abstract = {{Parameter estimation on gravitational wave signals from compact binary coalescence (CBC) requires the evaluation of computationally intensive waveform models, typically the bottleneck in the analysis. This cost will increase further as low frequency sensitivity in later second and third generation detectors motivates the use of longer waveforms. We describe a method for accelerating parameter estimation by exploiting the chirping behaviour of the signals to sample the waveform sparsely for portions where the full frequency resolution is not required. We demonstrate that the method can reproduce the original results with a waveform mismatch of <= 5x 10(-7), but with a waveform generation cost up to similar to 50 times lower for computationally costly frequency-domain waveforms starting from below 8 Hz.}}, DOI = {{10.1088/1361-6382/aa6d44}}, Article-Number = {{115006}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ORCID-Numbers = {{/0000-0003-3068-6974 Mandel, Ilya/0000-0002-6134-8946 Veitch, John/0000-0002-6508-0713}}, Unique-ID = {{ISI:000402399700006}}, } @article{ ISI:000400409800001, Author = {Barnafoeldi, G. G. and Bulik, T. and Cieslar, M. and David, E. and Dobroka, M. and Fenyvesi, E. and Gondek-Rosinska, D. and Graczer, Z. and Hamar, G. and Huba, G. and Kis, A. and Kovacs, R. and Lemperger, I. and Levai, P. and Molnar, J. and Nagy, D. and Novak, A. and Olah, L. and Pazmandi, P. and Piri, D. and Somlai, L. and Starecki, T. and Suchenek, M. and Suranyi, G. and Szalai, S. and Varga, D. and Vasuth, M. and Van, P. and Vasarhelyi, B. and Wesztergom, V. and Weber, Z.}, Title = {{First report of long term measurements of the MGGL laboratory in the Matra mountain range}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2017}}, Volume = {{34}}, Number = {{11}}, Month = {{JUN 8}}, Abstract = {{Matra Gravitational and Geophysical Laboratory (MGGL) was established near Gyongyosoroszi, Hungary in 2015, in the cavern system of an unused ore mine. The laboratory is located 88 m below the surface, with the aim of measuring and analysing the advantages of the underground installation's third generation gravitational wave detectors. Specialized instruments have been installed to measure seismic, infrasound and electromagnetic noise, and the variation of the cosmic muon flux. In the preliminary (RUN-0) test period, March-August 2016, data collection was accomplished. In this paper we describe the research potential of the MGGL, list the installed equipment and summarize the experimental results of RUN-0. Here we report on the RUN-0 data, that prepares the systematic and synchronized data collection of the next run period.}}, DOI = {{10.1088/1361-6382/aa69e3}}, Article-Number = {{114001}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Weber, Zoltan/A-7375-2009 Dobroka, Mihaly/B-4908-2018 Van, Peter/F-8579-2010 Kovacs, Robert/P-8911-2015 Barnafoldi, Gergely Gabor/AAB-5738-2021 Vasarhelyi, Balazs/G-9270-2011 Suchenek, Mariusz/AAZ-2790-2020 Bulik, Tomasz/AAJ-6742-2020 Fenyvesi, Edit/B-9076-2018 }}, ORCID-Numbers = {{Weber, Zoltan/0000-0002-0017-3505 Dobroka, Mihaly/0000-0003-3956-2070 Van, Peter/0000-0002-9396-4073 Kovacs, Robert/0000-0001-5822-6035 Barnafoldi, Gergely Gabor/0000-0001-9223-6480 Suchenek, Mariusz/0000-0003-1865-2894 Fenyvesi, Edit/0000-0003-2777-3719 Starecki, Tomasz/0000-0002-4730-6803 Kis, Arpad/0000-0003-1841-7202 Bulik, Tomasz/0000-0003-2045-4803 Rosinska, Dorota/0000-0002-3681-9304}}, Unique-ID = {{ISI:000400409800001}}, } @article{ ISI:000402807100004, Author = {Zhang, Xing and Yu, Jiming and Liu, Tan and Zhao, Wen and Wang, Anzhong}, Title = {{Testing Brans-Dicke gravity using the Einstein telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{12}}, Month = {{JUN 6}}, Abstract = {{Gravitational radiation is an excellent field for testing theories of gravity in strong gravitational fields. The current observations on the gravitational-wave (GW) bursts by LIGO have already placed various constraints on the alternative theories of gravity. In this paper, we investigate the possible bounds which could be placed on the Brans-Dicke gravity using GW detection from inspiraling compact binaries with the proposed Einstein Telescope, a third-generation GW detector. We first calculate in detail the waveforms of gravitational radiation in the lowest post-Newtonian approximation, including the tensor and scalar fields, which can be divided into the three polarization modes, i.e., ``plus mode,{''} ``cross mode,{''} and `` breathing mode.{''} Applying the stationary phase approximation, we obtain their Fourier transforms, and derive the correction terms in amplitude, phase, and polarization of GWs, relative to the corresponding results in general relativity. Imposing the noise level of the Einstein Telescope, we find that the GW detection from inspiraling compact binaries, composed of a neutron star and a black hole, can place stringent constraints on the Brans-Dicke gravity. The bound on the coupling constant.BD depends on the mass, sky position, inclination angle, polarization angle, luminosity distance, redshift distribution, and total observed number NGW of the binary systems. Taking into account all the burst events up to redshift z = 5, we find that the bound could be omega(BD) greater than or similar to 10(6) x (N-GW/10(4))(1/2). Even for the conservative estimation with 104 observed events, the bound is still more than one order tighter than the current limit from Solar System experiments. So, we conclude that the Einstein Telescope will provide a powerful platform to test alternative theories of gravity.}}, DOI = {{10.1103/PhysRevD.95.124008}}, Article-Number = {{124008}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Wang, Anzhong/AAS-9614-2020 }}, ORCID-Numbers = {{Zhang, Xing/0000-0001-5435-6502 Zhao, Wen/0000-0002-1330-2329}}, Unique-ID = {{ISI:000402807100004}}, } @article{ ISI:000408310600007, Author = {Cholis, Ilias}, Title = {{On the gravitational wave background from black hole binaries after the first LIGO detections}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2017}}, Number = {{6}}, Month = {{JUN}}, Abstract = {{The detection of gravitational waves from the merger of binary black holes by the LIGO Collaboration has opened a new window to astrophysics. With the sensitivities of ground based detectors in the coming years, we will principally detect local binary black hole mergers. The integrated merger rate can instead be probed by the gravitational-wave background, the incoherent superposition of the released energy in gravitational waves during binary-black-hole coalescence. Through that, the properties of the binary black holes can be studied. In this work we show that by measuring the energy density Omega(GW) (in units of the cosmic critical density) of the gravitational-wave background, we can search for the rare similar to 100 M-circle dot massive black holes formed in the Universe. In addition, we can answer how often the least massive BHs of mass greater than or similar to 3M(circle dot) form. Finally, if there are multiple channels for the formation of binary black holes and if any of them predicts a narrow mass range for the black holes, then the total Omega(GW) spectrum may have features that with the future Einstein Telescope can be detected.}}, DOI = {{10.1088/1475-7516/2017/06/037}}, Article-Number = {{037}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Cholis, Ilias/V-7306-2018}}, ORCID-Numbers = {{Cholis, Ilias/0000-0002-3805-6478}}, Unique-ID = {{ISI:000408310600007}}, } @article{ ISI:000402203800002, Author = {de Araujo, Jose C. N. and Coelho, Jaziel G. and Costa, Cesar A.}, Title = {{Gravitational waves from pulsars in the context of magnetic ellipticity}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2017}}, Volume = {{77}}, Number = {{5}}, Month = {{MAY 26}}, Abstract = {{In one of our previous articles we have considered the role of a time dependent magnetic ellipticity on the pulsars' braking indices and on the putative gravitational waves these objects can emit. Since only nine of more than 2000 known pulsars have accurately measured braking indices, it is of interest to extend this study to all known pulsars, in particular as regards gravitational wave generation. To do so, as shown in our previous article, we need to know some pulsars' observable quantities such as: periods and their time derivatives, and estimated distances to the Earth. Moreover, we also need to know the pulsars' masses and radii, for which we are adopting current fiducial values. Our results show that the gravitational wave amplitude is at best h similar to 10(-28). This leads to a pessimistic prospect for the detection of gravitational waves generated by these pulsars, even for Advanced LIGO and Advanced Virgo, and the planned Einstein Telescope, if the ellipticity has a magnetic origin.}}, DOI = {{10.1140/epjc/s10052-017-4925-3}}, Article-Number = {{350}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ResearcherID-Numbers = {{de Araujo, Jose C N/C-5181-2013 Costa, Cesar A/G-7588-2012 Coelho, Jaziel Goulart/D-8679-2013}}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289 Costa, Cesar A/0000-0003-4853-758X Coelho, Jaziel Goulart/0000-0001-9386-1042}}, Unique-ID = {{ISI:000402203800002}}, } @article{ ISI:000400677700024, Author = {Davoudiasl, Hooman and Giardino, Pier Paolo}, Title = {{Gravitational waves from primordial black holes and new weak scale phenomena}}, Journal = {{PHYSICS LETTERS B}}, Year = {{2017}}, Volume = {{768}}, Pages = {{198-202}}, Month = {{MAY 10}}, Abstract = {{We entertain the possibility that primordial black holes of mass similar to (10(26)-10(29)) g, with Schwarzschild radii of O(cm), constitute similar to 10\% or more of cosmic dark matter, as allowed by various constraints. These black holes would typically originate from cosmological eras corresponding to temperatures O(10-100) GeV, and may be associated with first order phase transitions in the visible or hidden sectors. In case these small primordial black holes get captured in orbits around neutron stars or astrophysical black holes in our galactic neighborhood, gravitational waves from the resulting ``David and Goliath (D\&G){''} binaries could be detectable at Advanced LIGO or Advanced Virgo for hours or more, possibly over distances of O(10) Mpc encompassing the Local Supercluster of galaxies. The proposed Einstein Telescope would further expand the reach for these signals. A positive signal could be further corroborated by the discovery of new particles in the O(10-100) GeV mass range, and potentially also the detection of long wavelength gravitational waves originating from the first order phase transition era. (C) 2017 The Authors. Published by Elsevier B.V.}}, DOI = {{10.1016/j.physletb.2017.02.054}}, ISSN = {{0370-2693}}, EISSN = {{1873-2445}}, ORCID-Numbers = {{Giardino, Pier Paolo/0000-0002-3379-5917}}, Unique-ID = {{ISI:000400677700024}}, } @article{ ISI:000399961300001, Author = {Regimbau, T. and Evans, M. and Christensen, N. and Katsavounidis, E. and Sathyaprakash, B. and Vitale, S.}, Title = {{Digging Deeper: Observing Primordial Gravitational Waves below the Binary-Black-Hole-Produced Stochastic Background}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2017}}, Volume = {{118}}, Number = {{15}}, Month = {{APR 14}}, Abstract = {{The merger rate of black hole binaries inferred from the detections in the first Advanced LIGO science run implies that a stochastic background produced by a cosmological population of mergers will likely mask the primordial gravitational wave background. Here we demonstrate that the next generation of ground-based detectors, such as the Einstein Telescope and Cosmic Explorer, will be able to observe binary black hole mergers throughout the Universe with sufficient efficiency that the confusion background can potentially be subtracted to observe the primordial background at the level of Omega(GW) similar or equal to 10(-13) after 5 years of observation.}}, DOI = {{10.1103/PhysRevLett.118.151105}}, Article-Number = {{151105}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Christensen, Nelson/AAH-9184-2019 Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Christensen, Nelson/0000-0002-6870-4202 Vitale, Salvatore/0000-0003-2700-0767 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000399961300001}}, } @article{ ISI:000406878500002, Author = {Cheng, Quan and Zhang, Shuang-Nan and Zheng, Xiao-Ping}, Title = {{Stochastic gravitational wave background from newly born massive magnetars: The role of a dense matter equation of state}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{8}}, Month = {{APR 7}}, Abstract = {{Newly born massive magnetars are generally considered to be produced by binary neutron star (NS) mergers, which could give rise to short gamma-ray bursts (SGRBs). The strong magnetic fields and fast rotation of these magnetars make them promising sources for gravitational wave (GW) detection using ground based GWinterferometers. Based on the observed masses of Galactic NS-NS binaries, by assuming different equations of state (EOSs) of dense matter, we investigate the stochastic gravitational wave background (SGWB) produced by an ensemble of newly born massive magnetars. The massive magnetar formation rate is estimated through: (i) the SGRB formation rate (hereafter entitled as MFR1); (ii) the NS-NS merger rate (hereafter entitled as MFR2). We find that for massive magnetars with masses M-mg = 2.4743 M-circle dot, if EOS CDDM2 is assumed, the resultant SGWBs may be detected by the future Einstein Telescope (ET) even for MFR1 with minimal local formation rate, and for MFR2 with a local merger rate rho(o)(c) (0) less than or similar to 10 Mpc(-3) Myr(-1). However, if EOS BSk21 is assumed, the SGWB may be detectable by the ET for MFR1 with the maximal local formation rate. Moreover, the background spectra show cutoffs at about 350 Hz in the case of EOS BSk21, and at 124 Hz for CDDM2, respectively. We suggest that if the cutoff at similar to 100 Hz in the background spectrum from massive magnetars could be detected, then the quark star EOS CDDM2 seems to be favorable. Moreover, the EOSs, which present relatively small TOV maximum masses, would be excluded.}}, DOI = {{10.1103/PhysRevD.95.083003}}, Article-Number = {{083003}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Zhang, Shuang-Nan/0000-0001-5586-1017}}, Unique-ID = {{ISI:000406878500002}}, } @article{ ISI:000399146300009, Author = {Vitale, Salvatore and Evans, Matthew}, Title = {{Parameter estimation for binary black holes with networks of third-generation gravitational-wave detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{6}}, Month = {{MAR 28}}, Abstract = {{The two binary black hole (BBH) coalescences detected by LIGO, GW150914, and GW151226, were relatively nearby sources, with a redshift of similar to 0.1. As the sensitivity of Advanced LIGO and Virgo increases in the next few years, they will eventually detect stellar-mass BBHs up to redshifts of similar to 1. However, these are still relatively small distances compared with the size of the Universe, or with those encountered in most areas of astrophysics. In order to study BBH during the epoch of reionization, or black holes born from population III stars, more sensitive instruments are needed. Third-generation gravitational-wave detectors, such as the Einstein Telescope or the Cosmic Explorer, are already in an advanced R\& D stage. These detectors will be roughly a factor of 10 more sensitive in strain than the current generation, and they will be able to detect BBH mergers beyond a redshift of 20. In this paper we quantify the precision with which these new facilities will be able to estimate the parameters of stellar-mass, heavy, and intermediate-mass BBHs as a function of their redshifts and the number of detectors. We show that having only two detectors would result in relatively poor estimates of black hole intrinsic masses: a situation improved with three or four instruments. Larger improvements are visible for the sky localization, although it is not yet clear whether BBHs are luminous in the electromagnetic or neutrino band. The measurement of the spin parameters, on the other hand, does not improve significantly as more detectors are added to the network since redshift information is not required to measure spin.}}, DOI = {{10.1103/PhysRevD.95.064052}}, Article-Number = {{064052}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Vitale, Salvatore/0000-0003-2700-0767}}, Unique-ID = {{ISI:000399146300009}}, } @article{ ISI:000399146000002, Author = {Crocker, K. and Prestegard, T. and Mandic, V. and Regimbau, T. and Olive, K. and Vangioni, E.}, Title = {{Systematic study of the stochastic gravitational-wave background due to stellar core collapse}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{6}}, Month = {{MAR 27}}, Abstract = {{Stellar core collapse events are expected to produce gravitational waves via several mechanisms, most of which are not yet fully understood due to the current limitations in the numerical simulations of these events. In this paper, we begin with an empirical functional form that fits the gravitational-wave spectra from existing simulations of stellar core collapse and integrate over all collapse events in the Universe to estimate the resulting stochastic gravitational-wave background. We then use a Gaussian functional form to separately fit and model a low-frequency peak in the core-collapse strain spectra, which likely occurs due to prompt convection. We systematically study the parameter space of both models, as well as the combined case, and investigate their detectability by upcoming gravitational-wave detectors, such as Advanced LIGO and the Einstein Telescope. Assuming realistic formation rates for progenitors of core-collapse supernovae, our results indicate that both models are 2-4 orders of magnitude below the expected sensitivity of Advanced LIGO, and 1-2 orders of magnitude below that of the Einstein Telescope.}}, DOI = {{10.1103/PhysRevD.95.063015}}, Article-Number = {{063015}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000399146000002}}, } @article{ ISI:000396044600001, Author = {Collett, Thomas E. and Bacon, David}, Title = {{Testing the Speed of Gravitational Waves over Cosmological Distances with Strong Gravitational Lensing}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2017}}, Volume = {{118}}, Number = {{9}}, Month = {{MAR 2}}, Abstract = {{Probing the relative speeds of gravitational waves and light acts as an important test of general relativity and alternative theories of gravity. Measuring the arrival time of gravitational waves (GWs) and electromagnetic (EM) counterparts can be used to measure the relative speeds, but only if the intrinsic time lag between emission of the photons and gravitational waves is well understood. Here we suggest a method that does not make such an assumption, using future strongly lensed GW events and EM counterparts; Biesiada et al. {[}J. Cosmol. Astropart. Phys. 10 (2014) 080] forecast that 50-100 strongly lensed GW events will be observed each year with the Einstein Telescope. A single strongly lensed GW event would produce robust constraints on c(GW)/c(gamma) at the 10(-7) level, if a high-energy EM counterpart is observed within the field of view of an observing gamma-ray burst monitor.}}, DOI = {{10.1103/PhysRevLett.118.091101}}, Article-Number = {{091101}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ORCID-Numbers = {{Collett, Thomas/0000-0001-5564-3140}}, Unique-ID = {{ISI:000396044600001}}, } @article{ ISI:000396087700008, Author = {Chirenti, Cecilia and Gold, Roman and Miller, M. Coleman}, Title = {{Gravitational Waves from F-modes Excited by the Inspiral of Highly Eccentric Neutron Star Binaries}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2017}}, Volume = {{837}}, Number = {{1}}, Month = {{MAR 1}}, Abstract = {{As gravitational wave instrumentation becomes more sensitive, it is interesting to speculate about subtle effects that could be analyzed using upcoming generations of detectors. One such effect that has great potential for revealing the properties of very dense matter is fluid oscillations of neutron stars. These have been found in numerical simulations of the hypermassive remnants of double neutron star mergers and of highly eccentric neutron star orbits. Here we focus on the latter and sketch out some ideas for the production, gravitational-wave detection, and analysis of neutron star oscillations. These events will be rare (perhaps up to several tens per year could be detected using third-generation detectors such as the Einstein Telescope or the Cosmic Explorer), but they would have unique diagnostic power for the analysis of cold, catalyzed, dense matter. Furthermore, these systems are unusual in that analysis of the tidally excited f-modes of the stars could yield simultaneous measurements of their masses, moments of inertia, and tidal Love numbers, using the frequency, damping time, and amplitude of the modes. They would thus present a nearly unique opportunity to test the I-Love-Q relation observationally. The analysis of such events will require significant further work in nuclear physics and general relativistic nonlinear mode coupling, and thus we discuss further directions that will need to be pursued. For example, we note that for nearly grazing encounters, numerical simulations show that the energy delivered to the f-modes may be up to two orders of magnitude greater than predicted in the linear theory.}}, DOI = {{10.3847/1538-4357/aa5ebb}}, Article-Number = {{67}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Gold, Roman/0000-0003-2492-1966 Miller, Cole/0000-0002-2666-728X}}, Unique-ID = {{ISI:000396087700008}}, } @article{ ISI:000394664300009, Author = {Smith, Tristan L. and Caldwell, Robert}, Title = {{Sensitivity to a frequency-dependent circular polarization in an isotropic stochastic gravitational wave background}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{4}}, Month = {{FEB 22}}, Abstract = {{We calculate the sensitivity to a circular polarization of an isotropic stochastic gravitational wave background (ISGWB) as a function of frequency for ground- and space-based interferometers and observations of the cosmic microwave background. The origin of a circularly polarized ISGWB may be due to exotic primordial physics (i.e., parity violation in the early universe) and may be strongly frequency dependent. We present calculations within a coherent framework which clarifies the basic requirements for sensitivity to circular polarization, in distinction from previous work which focused on each of these techniques separately. We find that the addition of an interferometer with the sensitivity of the Einstein Telescope in the southern hemisphere improves the sensitivity of the ground-based network to circular polarization by about a factor of two. The sensitivity curves presented in this paper make clear that the wide range in frequencies of current and planned observations (10(-18) Hz less than or similar to f less than or similar to 100 Hz) will be critical to determining the physics that underlies any positive detection of circular polarization in the ISGWB. We also identify a desert in circular polarization sensitivity for frequencies between 10(-15) Hz less than or similar to f less than or similar to 10(-3) Hz, given the inability for pulsar timing arrays and indirect-detection methods to distinguish the gravitational wave polarization.}}, DOI = {{10.1103/PhysRevD.95.044036}}, Article-Number = {{044036}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Caldwell, Robert/0000-0001-7490-7463}}, Unique-ID = {{ISI:000394664300009}}, } @article{ ISI:000394370500006, Author = {Cai, Rong-Gen and Yang, Tao}, Title = {{Estimating cosmological parameters by the simulated data of gravitational waves from the Einstein Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{4}}, Month = {{FEB 17}}, Abstract = {{We investigate the constraint ability of the gravitational wave (GW) as the standard siren on the cosmological parameters by using the third-generation gravitational wave detector: the Einstein Telescope. The binary merger of a neutron with either a neutron or black hole is hypothesized to be the progenitor of a short and intense burst of gamma rays; some fraction of those binary mergers could be detected both through electromagnetic radiation and gravitational waves. Thus we can determine both the luminosity distance and redshift of the source separately. We simulate the luminosity distances and redshift measurements from 100 to 1000 GWevents. We use two different algorithms to constrain the cosmological parameters. For the Hubble constant H-0 and dark matter density parameter Omega(m), we adopt the Markov chain Monte Carlo approach. We find that with about 500-600 GW events we can constrain the Hubble constant with an accuracy comparable to Planck temperature data and Planck lensing combined results, while for the dark matter density, GWs alone seem not able to provide the constraints as good as for the Hubble constant; the sensitivity of 1000 GWevents is a little lower than that of Planck data. It should require more than 1000 events to match the Planck sensitivity. Yet, for analyzing the more complex dynamical property of dark energy, i. e., the equation of state w, we adopt a new powerful nonparametric method: the Gaussian process. We can reconstruct w directly from the observational luminosity distance at every redshift. In the low redshift region, we find that about 700 GW events can give the constraints of w(z)comparable to the constraints of a constant w by Planck data with type-Ia supernovae. Those results show that GWs as the standard sirens to probe the cosmological parameters can provide an independent and complementary alternative to current experiments.}}, DOI = {{10.1103/PhysRevD.95.044024}}, Article-Number = {{044024}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Yang, Tao/0000-0002-2161-0495}}, Unique-ID = {{ISI:000394370500006}}, } @article{ ISI:000402240300002, Author = {Del Pozzo, Walter and Li, Tjonnie G. F. and Messenger, Chris}, Title = {{Cosmological inference using only gravitational wave observations of binary neutron stars}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2017}}, Volume = {{95}}, Number = {{4}}, Month = {{FEB 2}}, Abstract = {{Gravitational waves emitted during the coalescence of binary neutron star systems are self-calibrating signals. As such, they can provide a direct measurement of the luminosity distance to a source without the need for a cross-calibrated cosmic distance-scale ladder. In general, however, the corresponding redshift measurement needs to be obtained via electromagnetic observations since it is totally degenerate with the total mass of the system. Nevertheless, Fisher matrix studies have shown that, if information about the equation of state of the neutron stars is available, it is possible to extract redshift information from the gravitational wave signal alone. Therefore, measuring the cosmological parameters in pure gravitational-wave fashion is possible. Furthermore, the huge number of sources potentially observable by the Einstein Telescope has led to speculations that the gravitational wave measurement is potentially competitive with traditional methods. The Einstein Telescope is a conceptual study for a third generation gravitational wave detector which is designed to yield 10(3)-10(7) detections of binary neutron star systems per year. This study presents the first Bayesian investigation of the accuracy with which the cosmological parameters can be measured using information coming only from the gravitational wave observations of binary neutron star systems by the Einstein Telescope. We find, by direct simulation of 10(3) detections of binary neutron stars, that, within our simplifying assumptions, H-0, Omega(m), Omega(Lambda), w(0) and w(1) can be measured at the 95\% level with an accuracy of similar to 8\%, 65\%, 39\%, 80\% and 90\%, respectively. We also find, by extrapolation, that a measurement accuracy comparable with current measurements by Planck is possible if the number of gravitational wave events observed is O(10(6-7)). We conclude that, while not competitive with electromagnetic missions in terms of significant digits, gravitational waves alone are capable of providing a complementary determination of the dynamics of the Universe.}}, DOI = {{10.1103/PhysRevD.95.043502}}, Article-Number = {{043502}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ORCID-Numbers = {{Del Pozzo, Walter/0000-0003-3978-2030 Messenger, Chris/0000-0001-7488-5022 Li, Tjonnie Guang Feng/0000-0003-4297-7365}}, Unique-ID = {{ISI:000402240300002}}, } @article{ ISI:000401145500010, Author = {Lu, Hou-Jun and Zhang, Hai-Ming and Zhong, Shu-Qing and Hou, Shu-Jin and Sun, Hui and Rice, Jared and Liang, En-Wei}, Title = {{Magnetar Central Engine and Possible Gravitational Wave Emission of Nearby Short GRB 160821B}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2017}}, Volume = {{835}}, Number = {{2}}, Month = {{FEB 1}}, Abstract = {{GRB 160821B is a short gamma-ray burst (SGRB) at redshift z = 0.16, with a duration less than 1 s and without any ``extended emission{''} detected up to more than 100 s in both Swift/BAT and Fermi/GBM bands. An X-ray plateau with a sharp drop 180 s after the BAT trigger was observed with Swift/XRT. No supernova or kilo-nova signature was detected. Assuming the central engine of this SGRB is a recently born supra-massive magnetar, we can explain the SGRB as jet radiation and its X-ray plateau as the internal energy dissipation of the pulsar wind as it spins down. We constrain its surface magnetic field to B-p < 3.12 x 10(16) G and initial spin period to P-0 < 8.5 x 10(-3) s. Its equation of state is consistent with the GM1 model with M-TOV similar to 2.37 circle dot Me and ellipticity is an element of< 0.07. Its gravitational wave (GW) radiation may be detectable with the future Einstein Telescope, but is much weaker than the current detectability limit of Advanced LIGO. The GW radiation of such an event would be detectable by Advanced LIGO if it occurred at a distance of 100 Mpc (z = 0.023).}}, DOI = {{10.3847/1538-4357/835/2/181}}, Article-Number = {{181}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Zhang, Hai-Ming/0000-0001-6863-5369 Zhong, Shu-Qing/0000-0002-1766-6947 Rice, Jared/0000-0003-3887-091X}}, Unique-ID = {{ISI:000401145500010}}, } @article{ ISI:000399409800010, Author = {Wang, Yu-Tong and Cai, Yong and Liu, Zhi-Guo and Piao, Yun-Song}, Title = {{Probing the primordial universe with gravitational waves detectors}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2017}}, Number = {{1}}, Month = {{JAN}}, Abstract = {{The spectrum of primordial gravitational waves (GWis), especially Us tilt n(T) carries significant information about the primordial universe. (.;Combining recent AKA) and Planck2015+BK14 data, we find that the current limit n(T) = 0.016(-0.989)(+0.614) at 95\% also estimate the impacts of Einstein Telescope and LISA on constraining n(T). Moreover, based on the effective field theory of cosmological perturbations, we make an attempt to confront some models of early universe scenarios, which produce blue-tilted CWs spectrum (n(T) > 0), with the corresponding datasets.}}, DOI = {{10.1088/1475-7516/2017/01/010}}, Article-Number = {{010}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Cai, Yong/AAC-9930-2019 }}, ORCID-Numbers = {{Cai, Yong/0000-0002-3823-8159}}, Unique-ID = {{ISI:000399409800010}}, } @article{ ISI:000386173200001, Author = {Bhagwat, Swetha and Brown, Duncan A. and Ballmer, Stefan W.}, Title = {{Spectroscopic analysis of stellar mass black-hole mergers in our local universe with ground-based gravitational wave detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{94}}, Number = {{8}}, Month = {{OCT 17}}, Abstract = {{Motivated by the recent discoveries of binary black-hole mergers by the Advanced Laser Interferometer Gravitational-Wave Observatory (Advanced LIGO), we investigate the prospects of ground-based detectors to perform a spectroscopic analysis of signals emitted during the ringdown of the final Kerr black hole formed by a stellar mass binary black-hole merger. Although it is unlikely that Advanced LIGO can measure multiple modes of the ringdown, assuming an optimistic rate of 240 Gpc(-3) yr(-1), upgrades to the existing LIGO detectors could measure multiple ringdown modes in similar to 6 detections per year. New ground-based facilities such as Einstein Telescope or Cosmic Explorer could measure multiple ringdown modes in over 300 events per year. We perform Monte Carlo injections of 106 binary black-hole mergers in a search volume defined by a sphere of radius 1500 Mpc centered at the detector, for various proposed ground-based detector models. We assume a uniform random distribution in component masses of the progenitor binaries, sky positions and orientations to investigate the fraction of the population that satisfies our criteria for detectability and resolvability of multiple ringdown modes. We investigate the detectability and resolvability of the subdominant modes l = m = 3, l = m = 4 and l = 2, m = 1. Our results indicate that the modes with l = m = 3 and l = 2, m = 1 are the most promising candidates for subdominant mode measurability. We find that for stellar mass black-hole mergers, resolvability is not a limiting criteria for these modes. We emphasize that the measurability of the l = 2, m = 1 mode is not impeded by the resolvability criterion.}}, DOI = {{10.1103/PhysRevD.94.084024}}, Article-Number = {{084024}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Brown, Duncan/U-2343-2019 }}, ORCID-Numbers = {{Brown, Duncan/0000-0002-9180-5765 Bhagwat, Swetha/0000-0003-4700-5274}}, Unique-ID = {{ISI:000386173200001}}, } @article{ ISI:000385246500010, Author = {Cholis, Ilias and Kovetz, Ely D. and Ali-Haimoud, Yacine and Bird, Simeon and Kamionkowski, Marc and Munoz, Julian B. and Raccanelli, Alvise}, Title = {{Orbital eccentricities in primordial black hole binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{94}}, Number = {{8}}, Month = {{OCT 6}}, Abstract = {{It was recently suggested that the merger of similar to 30 M-circle dot primordial black holes (PBHs) may provide a significant number of events in gravitational-wave observatories over the next decade, if they make up an appreciable fraction of the dark matter. Here we show that measurement of the eccentricities of the inspiralling binary black holes can be used to distinguish these binaries from those produced by more traditional astrophysical mechanisms. These PBH binaries are formed on highly eccentric orbits and can then merge on time scales that in some cases are years or less, retaining some eccentricity in the last seconds before the merger. This is to be contrasted with massive-stellar-binary, globular-cluster, or other astrophysical origins for binary black holes (BBHs) in which the orbits have very effectively circularized by the time the BBH enters the observable LIGO window. Here we discuss the features of the gravitational-wave signals that indicate this eccentricity and forecast the sensitivity of LIGO and the Einstein Telescope to such effects. We show that if PBHs make up the dark matter, then roughly one event should have a detectable eccentricity given LIGO's expected sensitivity and observing time of six years. The Einstein Telescope should see O (10) such events after ten years.}}, DOI = {{10.1103/PhysRevD.94.084013}}, Article-Number = {{084013}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Raccanelli, Alvise/M-9879-2019 Raccanelli, Alvise/N-7473-2018 Cholis, Ilias/V-7306-2018 }}, ORCID-Numbers = {{Raccanelli, Alvise/0000-0001-6726-0438 Cholis, Ilias/0000-0002-3805-6478 Kovetz, Ely/0000-0001-9256-1144}}, Unique-ID = {{ISI:000385246500010}}, } @article{ ISI:000388578300007, Author = {Kinugawa, Tomoya and Nakano, Hiroyuki and Nakamura, Takashi}, Title = {{Gravitational wave quasinormal mode from Population III massive black hole binaries in various models of population synthesis}}, Journal = {{PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS}}, Year = {{2016}}, Volume = {{2016}}, Number = {{10}}, Month = {{OCT}}, Abstract = {{Focusing on the remnant black holes after merging binary black holes, we show that ringdown gravitational waves of Population III binary black hole mergers can be detected at the rate of 5.9-500 events yr(-1) (SFRp/(10(-2.5) M-circle dot yr(-1) Mpc(-3))) . ({[}f(b)/(1 + f(b))]/0.33) for various parameters and functions. This rate is estimated for events with SNR > 8 for second-generation gravitational wave detectors such as KAGRA. Here, SFRp and f(b) are the peak value of the Population III star formation rate and the fraction of binaries, respectively. When we consider only events with SNR > 35, the event rate becomes 0.0464.21 events yr(-1) (SFRp/(10(-2.5) M-circle dot yr(-1) Mpc(-3))) . ({[}fb/(1 + f(b))]/0.33). This suggest that for a remnant black hole spin of q(f) > 0.95 we have an event rate of quasinormal modes with SNR > 35 of less than 0.037 events yr(-1) (SFRp/(10(-2.5) M-circle dot yr(-1) Mpc(-3))) . ({[}fb/(1 + f(b))]/0.33), while it is 3-30 events yr(-1) (SFRp/(10(-2.5) M-circle dot yr(-1) Mpc-3)) . ({[}f(b)/(1 + f(b))]/0.33) for third-generation detectors such as the Einstein Telescope. If we detect many Population III binary black hole mergers, it may be possible to constrain the Population III binary evolution paths not only by the mass distribution but also by the spin distribution.}}, DOI = {{10.1093/ptep/ptw143}}, Article-Number = {{103E01}}, ISSN = {{2050-3911}}, ResearcherID-Numbers = {{Kinugawa, Tomoya/AAU-3650-2020 }}, ORCID-Numbers = {{Nakano, Hiroyuki/0000-0001-7665-0796}}, Unique-ID = {{ISI:000388578300007}}, } @article{ ISI:000383481100033, Author = {Inayoshi, Kohei and Kashiyama, Kazumi and Visbal, Eli and Haiman, Zoltan}, Title = {{Gravitational wave background from Population III binary black holes consistent with cosmic reionization}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2016}}, Volume = {{461}}, Number = {{3}}, Pages = {{2722-2727}}, Month = {{SEP 21}}, Abstract = {{The recent discovery of the gravitational wave source GW150914 has revealed a coalescing binary black hole (BBH) with masses of similar to 30 M-circle dot. Previous proposals for the origin of such a massive binary include Population III (PopIII) stars. PopIII stars are efficient producers of BBHs and of a gravitational wave background (GWB) in the 10-100 Hz band, and also of ionizing radiation in the early Universe. We quantify the relation between the amplitude of the GWB (Omega(gw)) and the electron scattering optical depth (tau(e)), produced by PopIII stars, assuming that f(esc) approximate to 10 per cent of their ionizing radiation escapes into the intergalactic medium. We find that PopIII stars would produce a GWB that is detectable by the future O5 LIGO/Virgo if tau(e) greater than or similar to 0.07, consistent with the recent Planck measurement of tau(e) = 0.055 +/- 0.09. Moreover, the spectral index of the background from PopIII BBHs becomes as small as d ln Omega(gw)/d ln f less than or similar to 0.3 at f greater than or similar to 30 Hz, which is significantly flatter than the value similar to 2/3 generically produced by lower redshift and less-massive BBHs. A detection of the unique flattening at such low frequencies by the O5 LIGO/Virgo will indicate the existence of a high-chirp mass, high-redshift BBH population, which is consistent with the PopIII origin. A precise characterization of the spectral shape near 30-50 Hz by the Einstein Telescope could also constrain the PopIII initial mass function and star formation rate.}}, DOI = {{10.1093/mnras/stw1431}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Inayoshi, Kohei/AAW-2098-2020 Kashiyama, Kazumi/AAW-2077-2020 }}, ORCID-Numbers = {{Kashiyama, Kazumi/0000-0003-4299-8799 Haiman, Zoltan/0000-0003-3633-5403}}, Unique-ID = {{ISI:000383481100033}}, } @article{ ISI:000385374500029, Author = {Tan, Wei-Wei and Wang, F. Y. and Cheng, K. S.}, Title = {{CONSTRAINING WARM DARK MATTER MASS WITH COSMIC REIONIZATION AND GRAVITATIONAL WAVES}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2016}}, Volume = {{829}}, Number = {{1}}, Month = {{SEP 20}}, Abstract = {{We constrain the warm dark matter (WDM) particle mass with observations of cosmic reionization and CMB optical depth. We suggest that the gravitational waves (GWs) from stellar-mass black holes (BHs) could give a further constraint on WDM particle mass for future observations. The star formation rates (SFRs) of Population I/II (Pop I/II) and Population III (Pop III) stars are also derived. If the metallicity of the universe is enriched beyond the critical value of Z(crit) = 10(-3.5) Z(circle dot), the star formation shifts from Pop III to Pop I/II stars. Our results show that the SFRs are quite dependent on the WDM particle mass, especially at high redshifts. Combined with the reionization history and CMB optical depth derived from the recent Planck mission, we find that the current data require the WDM particle mass to be in a narrow range of 1 keV less than or similar to m(x) less than or similar to 3 keV. Furthermore, we suggest that the stochastic gravitational wave background (SGWB) produced by stellar BHs could give a further constraint on the WDM particle mass for future observations. For m(x) = 3 keV, with Salpeter (Chabrier) initial mass function (IMF), the SGWB from Pop I/II BHs has a peak amplitude of Omega(GW) approximate to 2.8 x 10(-9) (5.0 x 10(-9)) at f = 316Hz, while the GW radiation at f < 10 Hz is seriously suppressed. For m(x) = 1 keV, the SGWB peak amplitude is the same as that for m(x) = 1 keV, but a little lower at low frequencies. Therefore, it is hard to constrain the WDM particle mass by the SGWB from Pop I/II BHs. To assess the detectability of the GW signal, we also calculate the signal-to-noise ratios (S/N), which are S/N = 37.7(66.5) and 27 (47.7) for m(x) = 3 keV and m(x) = 1 keV for the Einstein Telescope with Salpeter (Chabrier) IMF, respectively. The SGWB from Pop III BHs is very dependent on the WDM particle mass, the GW strength could be an order of magnitude different, and the frequency band could be two times different for m(x) = 1 keV and m(x) = 3 keV. Moreover, the SGWB from Pop III BHs with m(x) = 1 keV could be detected by the Laser Interferometer Space Antenna for one year of observation, but it cannot be detected for those with m(x) = 3 keV.}}, DOI = {{10.3847/0004-637X/829/1/29}}, Article-Number = {{29}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Wang, Fayin/B-1479-2009}}, ORCID-Numbers = {{Wang, Fayin/0000-0003-4157-7714}}, Unique-ID = {{ISI:000385374500029}}, } @article{ ISI:000383241400003, Author = {Radice, David and Bernuzzi, Sebastiano and Ott, Christian D.}, Title = {{One-armed spiral instability in neutron star mergers and its detectability in gravitational waves}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{94}}, Number = {{6}}, Month = {{SEP 6}}, Abstract = {{We study the development and saturation of the m = 1 one-armed spiral instability in remnants of binary neutron star mergers by means of high-resolution long-term numerical relativity simulations. Our results suggest that this instability is a generic outcome of neutron star mergers in astrophysically relevant configurations, including both ``stiff{''} and ``soft{''} nuclear equations of state. We find that, once seeded at merger, the m = 1 mode saturates within similar to 10 ms and persists over secular time scales. Gravitational waves emitted by the m = 1 instability have a peak frequency around 1-2 kHz and, if detected, they could be used to constrain the equation of state of neutron stars. We construct hybrid waveforms spanning the entire Advanced LIGO band by combining our high-resolution numerical data with state-of-the-art effective-one-body waveforms including tidal effects. We use the complete hybrid waveforms to study the detectability of the one-armed spiral instability for both Advanced LIGO and the Einstein Telescope. We conclude that the one-armed spiral instability is not an efficient gravitational wave emitter. Even under very optimistic assumptions, Advanced LIGO will only be able to detect the one-armed instability up to similar to 3 Mpc, which corresponds to an event rate of 10(-7) yr(-1) to 10(-4) yr(-1). Third-generation detectors or better will likely be required to observe the one-armed instability.}}, DOI = {{10.1103/PhysRevD.94.064011}}, Article-Number = {{064011}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000383241400003}}, } @article{ ISI:000383044700004, Author = {Berti, Emanuele and Sesana, Alberto and Barausse, Enrico and Cardoso, Vitor and Belczynski, Krzysztof}, Title = {{Spectroscopy of Kerr Black Holes with Earth- and Space-Based Interferometers}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2016}}, Volume = {{117}}, Number = {{10}}, Month = {{SEP 2}}, Abstract = {{We estimate the potential of present and future interferometric gravitational-wave detectors to test the Kerr nature of black holes through ``gravitational spectroscopy,{''} i.e., the measurement of multiple quasinormal mode frequencies from the remnant of a black hole merger. Using population synthesis models of the formation and evolution of stellar-mass black hole binaries, we find that Voyager-class interferometers will be necessary to perform these tests. Gravitational spectroscopy in the local Universe may become routine with the Einstein Telescope, but a 40-km facility like Cosmic Explorer is necessary to go beyond z similar to 3. In contrast, detectors like eLISA (evolved Laser Interferometer Space Antenna) should carry out a few-or even hundreds-of these tests every year, depending on uncertainties in massive black hole formation models. Many space-based spectroscopical measurements will occur at high redshift, testing the strong gravity dynamics of Kerr black holes in domains where cosmological corrections to general relativity (if they occur in nature) must be significant.}}, DOI = {{10.1103/PhysRevLett.117.101102}}, Article-Number = {{101102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{barausse, enrico/M-3755-2017 Berti, Emanuele/AAI-1513-2019 Cardoso, Vitor/AAG-7689-2020 Berti, Emanuele/C-9331-2016 Sesana, Alberto/Q-9826-2016 }}, ORCID-Numbers = {{Cardoso, Vitor/0000-0003-0553-0433 Berti, Emanuele/0000-0003-0751-5130 Sesana, Alberto/0000-0003-4961-1606 Barausse, Enrico/0000-0001-6499-6263}}, Unique-ID = {{ISI:000383044700004}}, } @article{ ISI:000382738500003, Author = {de Araujoa, Jose C. N. and Coelho, Jaziel G. and Costa, Cesar A.}, Title = {{Gravitational waves from pulsars with measured braking index}}, Journal = {{EUROPEAN PHYSICAL JOURNAL C}}, Year = {{2016}}, Volume = {{76}}, Number = {{9}}, Month = {{AUG 31}}, Abstract = {{We study the putative emission of gravitational waves (GWs) in particular for pulsars with measured braking index. We show that the appropriate combination of both GW emission and magnetic dipole brakes can naturally explain the measured braking index, when the surface magnetic field and the angle between the magnetic dipole and rotation axes are time dependent. Then we discuss the detectability of these very pulsars by aLIGO and the Einstein Telescope. We call attention to the realistic possibility that aLIGO can detect the GWs generated by at least some of these pulsars, such as Vela, for example.}}, DOI = {{10.1140/epjc/s10052-016-4327-y}}, Article-Number = {{481}}, ISSN = {{1434-6044}}, EISSN = {{1434-6052}}, ResearcherID-Numbers = {{Costa, Cesar A/G-7588-2012 Coelho, Jaziel Goulart/D-8679-2013 Costa, Cesar/V-9846-2019 de Araujo, Jose C N/C-5181-2013}}, ORCID-Numbers = {{Costa, Cesar A/0000-0003-4853-758X Coelho, Jaziel Goulart/0000-0001-9386-1042 Costa, Cesar/0000-0003-4853-758X de Araujo, Jose C N/0000-0003-4418-4289}}, Unique-ID = {{ISI:000382738500003}}, } @article{ ISI:000380114700004, Author = {Raccanelli, Alvise and Kovetz, Ely D. and Bird, Simeon and Cholis, Ilias and Munoz, Julian B.}, Title = {{Determining the progenitors of merging black-hole binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{94}}, Number = {{2}}, Month = {{JUL 19}}, Abstract = {{We investigate a possible method for determining the progenitors of black-hole (BH) mergers observed via their gravitational wave (GW) signal. We argue that measurements of the cross-correlation of the GW events with overlapping galaxy catalogs may provide an additional tool in determining if BH mergers trace the stellar mass of the Universe, as would be expected from mergers of the end points of stellar evolution. If, on the other hand, the BHs are of primordial origin, as has been recently suggested, their merging would be preferentially hosted by lower biased objects and thus have a lower cross-correlation with luminous galaxies. Here, we forecast the expected precision of the cross-correlation measurement for current and future GW detectors such as LIGO and the Einstein Telescope. We then predict how well these instruments can distinguish the model that identifies high-mass BH-BH mergers as the merger of primordial black holes that constitute the dark matter in the Universe from more traditional astrophysical sources.}}, DOI = {{10.1103/PhysRevD.94.023516}}, Article-Number = {{023516}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Bird, Simeon/ABH-5012-2020 Raccanelli, Alvise/M-9879-2019 Raccanelli, Alvise/N-7473-2018 Cholis, Ilias/V-7306-2018 }}, ORCID-Numbers = {{Bird, Simeon/0000-0001-5803-5490 Raccanelli, Alvise/0000-0001-6726-0438 Cholis, Ilias/0000-0002-3805-6478 Kovetz, Ely/0000-0001-9256-1144}}, Unique-ID = {{ISI:000380114700004}}, } @article{ ISI:000381830000024, Author = {de Araujo, Jose C. N. and Coelho, Jaziel G. and Costa, Cesar A.}, Title = {{Gravitational wave emission by the high braking index pulsar PSR J1640-4631}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2016}}, Number = {{7}}, Month = {{JUL}}, Abstract = {{Recently, a braking index for the pulsar PSR J1640-4631 has been measured. With a braking index of n = 3.15 +/- 0.03, this pulsar has the highest braking index ever measured. As it is well known, a pure magnetic dipole brake yields n = 3, whereas a pure gravitational wave (GW) brake yields n = 5. Therefore, each of these mechanisms alone can not account for the braking index found for PSR J1640-4631. Here we consider in detail that such a braking index could be accounted for if the spindown model combines magnetic dipole and GW brakes. Then, we briefly discuss the detectability of this pulsar by aLIGO and the planned Einstein Telescope. In particular, we show that the amplitude of the GW that comes from our model is around a factor four lower than the amplitude modeled exclusively by GW energy loss. Another interesting outcome of our modeling is that it is possible to obtain the ellipticity from the braking index and other pulsar parameters.}}, DOI = {{10.1088/1475-7516/2016/07/023}}, Article-Number = {{023}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{de Araujo, Jose C N/C-5181-2013 Coelho, Jaziel Goulart/D-8679-2013 Costa, Cesar/V-9846-2019 Costa, Cesar A/G-7588-2012}}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289 Coelho, Jaziel Goulart/0000-0001-9386-1042 Costa, Cesar/0000-0003-4853-758X Costa, Cesar A/0000-0003-4853-758X}}, Unique-ID = {{ISI:000381830000024}}, } @article{ ISI:000377806300004, Author = {Nishizawa, Atsushi}, Title = {{Constraining the propagation speed of gravitational waves with compact binaries at cosmological distances}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{93}}, Number = {{12}}, Month = {{JUN 15}}, Abstract = {{When testing gravity in a model-independent way, one of the crucial tests is measuring the propagation speed of a gravitational wave (GW). In general relativity, a GW propagates with the speed of light, while in the alternative theories of gravity, the propagation speed could deviate from the speed of light due to the modification of gravity or spacetime structure at a quantum level. Previously, we proposed a method to measure the GW speed by directly comparing the arrival times between a GW and a photon from the binary merger of neutron stars or a neutron star and black hole, assuming that it is associated with a short gammaray burst. The sensitivity is limited by the intrinsic time delay between a GW and a photon at the source. In this paper, we extend the method to distinguish the intrinsic time delay from the true signal caused by anomalous GW speed with multiple events at cosmological distances, considering the redshift distribution of GW sources, redshift-dependent GW propagation speed, and the statistics of intrinsic time delays. We show that an advanced GW detector such as the Einstein Telescope will be able to robustly constrain the GW propagation speed at a precision of similar to 10(-16). We also discuss the optimal statistic to measure the GW speed by performing numerical simulations.}}, DOI = {{10.1103/PhysRevD.93.124036}}, Article-Number = {{124036}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, Unique-ID = {{ISI:000377806300004}}, } @article{ ISI:000381226500011, Author = {Nair, Remya and Jhingan, Sanjay and Tanaka, Takahiro}, Title = {{Synergy between ground- and space-based gravitational-wave detectors for estimation of binary coalescence parameters}}, Journal = {{PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS}}, Year = {{2016}}, Volume = {{2016}}, Number = {{5}}, Month = {{MAY}}, Abstract = {{We study the advantages of the coexistence of future ground- and space-based gravitational-wave detectors in estimating the parameters of a binary coalescence. Space measurements will act as a precursor to ground measurements. Also, since space measurements will provide much better localization information on the source, they will aid electromagnetic follow-up of the source and hence increase the probability of finding an electromagnetic counterpart of the gravitational-wave event. Using the post-Newtonian waveform for the inspiral of nonspinning neutron star-black hole binaries in circular orbits, we analyze how estimates for the chirp mass, the symmetric mass ratio, and the time and phase at coalescence are improved by combining the data from different space-ground detector pairs. Since the gravitational waves produced by binary coalescence also provide a suitable domain where we can investigate strong field gravity, we also study the deviations from general relativity using the parameterized post-Einsteinian framework. As an example, focusing on the Einstein telescope and DECIGO pair, we demonstrate that there exists a sweet-spot range of sensitivity in the pre-DECIGO period where the best enhancement due to the synergy effect can be obtained for estimates of the post-Newtonian waveform parameters. Similar results are obtained for the parameter that characterizes deviation from general relativity.}}, DOI = {{10.1093/ptep/ptw043}}, Article-Number = {{053E01}}, ISSN = {{2050-3911}}, ResearcherID-Numbers = {{Jhingan, Sanjay/AAF-1103-2020}}, ORCID-Numbers = {{Jhingan, Sanjay/0000-0003-2081-5197}}, Unique-ID = {{ISI:000381226500011}}, } @article{ ISI:000372729200004, Author = {Namikawa, Toshiya and Nishizawa, Atsushi and Taruya, Atsushi}, Title = {{Anisotropies of Gravitational-Wave Standard Sirens as a New Cosmological Probe without Redshift Information}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2016}}, Volume = {{116}}, Number = {{12}}, Month = {{MAR 24}}, Abstract = {{Gravitational waves (GWs) from compact binary stars at cosmological distances are promising and powerful cosmological probes, referred to as the GW standard sirens. With future GW detectors, we will be able to precisely measure source luminosity distances out to a redshift z similar to 5. To extract cosmological information, previously proposed cosmological studies using the GW standard sirens rely on source redshift information obtained through an extensive electromagnetic follow-up campaign. However, the redshift identification is typically time consuming and rather challenging. Here, we propose a novel method for cosmology with the GW standard sirens free from the redshift measurements. Utilizing the anisotropies of the number density and luminosity distances of compact binaries originated from the large-scale structure, we show that, once GW observations will be well established in the future, (i) these anisotropies can be measured even at very high redshifts (z >= 2), where the identification of the electromagnetic counterpart is difficult, (ii) the expected constraints on the primordial non-Gaussianity with the Einstein Telescope would be comparable to or even better than the other large-scale structure probes at the same epoch, and (iii) the cross-correlation with other cosmological observations is found to have high-statistical significance, providing additional cosmological information at very high redshifts.}}, DOI = {{10.1103/PhysRevLett.116.121302}}, Article-Number = {{121302}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Jung, David/Q-4068-2016 }}, ORCID-Numbers = {{Jung, David/0000-0001-8631-610X Taruya, Atsushi/0000-0002-4016-1955 Namikawa, Toshiya/0000-0003-3070-9240}}, Unique-ID = {{ISI:000372729200004}}, } @article{ ISI:000369715900097, Author = {Surace, M. and Kokkotas, K. D. and Pnigouras, P.}, Title = {{The stochastic background of gravitational waves due to the f-mode instability in neutron stars}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2016}}, Volume = {{586}}, Month = {{FEB}}, Abstract = {{This paper presents an estimate for the spectral properties of the stochastic background of gravitational waves emitted by a population of hot, young, rapidly rotating neutron stars throughout the Universe undergoing f-mode instabilities, formed through either core-collapse supernova explosions or the merger of binary neutron star systems. Their formation rate, from which the gravitational wave event rate is obtained, is deduced from observation-based determinations of the cosmic star formation rate. The gravitational wave emission occurs during the spin-down phase of the f-mode instability. For low magnetized neutron stars and assuming 10\% of supernova events lead to f-mode unstable neutron stars, the background from supernova-derived neutron stars peaks at Omega(gw) similar to 10(-9) for the l = m = 2 f-mode, which should be detectable by cross-correlating a pair of second generation interferometers (e.g. Advanced LIGO/Virgo) with an upper estimate for the signal-to-noise ratio of approximate to 9.8. The background from supramassive neutron stars formed from binary mergers peaks at Omega(gw) similar to 10(-10) and should not be detectable, even with third generation interferometers (e.g. Einstein Telescope).}}, DOI = {{10.1051/0004-6361/201527197}}, Article-Number = {{A86}}, ISSN = {{0004-6361}}, EISSN = {{1432-0746}}, ResearcherID-Numbers = {{Kokkotas, Kostas D/B-7878-2010 }}, ORCID-Numbers = {{Kokkotas, Kostas D/0000-0001-6048-2919 Pnigouras, Pantelis/0000-0003-1895-9431 Armus, Lee/0000-0003-3498-2973}}, Unique-ID = {{ISI:000369715900097}}, } @article{ ISI:000367897000004, Author = {Meacher, Duncan and Cannon, Kipp and Hanna, Chad and Regimbau, Tania and Sathyaprakash, B. S.}, Title = {{Second Einstein Telescope mock data and science challenge: Low frequency binary neutron star data analysis}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2016}}, Volume = {{93}}, Number = {{2}}, Month = {{JAN 11}}, Abstract = {{The Einstein Telescope is a conceived third-generation gravitational-wave detector that is envisioned to be an order of magnitude more sensitive than advanced LIGO, Virgo, and Kagra, which would be able to detect gravitational-wave signals from the coalescence of compact objects with waveforms starting as low as 1 Hz. With this level of sensitivity, we expect to detect sources at cosmological distances. In this paper we introduce an improved method for the generation of mock data and analyze it with a new low-latency compact binary search pipeline called gstlal. We present the results from this analysis with a focus on low-frequency analysis of binary neutron stars. Despite compact binary coalescence signals lasting hours in the Einstein Telescope sensitivity band when starting at 5 Hz, we show that we are able to discern various overlapping signals from one another. We also determine the detection efficiency for each of the analysis runs conducted and show a proof of concept method for estimating the number signals as a function of redshift. Finally, we show that our ability to recover the signal parameters has improved by an order of magnitude when compared to the results of the first mock data and science challenge. For binary neutron stars we are able to recover the total mass and chirp mass to within 0.5\% and 0.05\%, respectively.}}, DOI = {{10.1103/PhysRevD.93.024018}}, Article-Number = {{024018}}, ISSN = {{2470-0010}}, EISSN = {{2470-0029}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Cannon, Kipp/0000-0003-4068-6572 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000367897000004}}, } @article{ ISI:000366361700012, Author = {Krueger, Christoph and Heinert, Daniel and Khalaidovski, Alexander and Steinlechner, Jessica and Nawrodt, Ronny and Schnabel, Roman and Lueck, Harald}, Title = {{Birefringence measurements on crystalline silicon}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2016}}, Volume = {{33}}, Number = {{1}}, Month = {{JAN 7}}, Abstract = {{Crystalline silicon has been proposed as a new test mass material in third generation gravitational wave detectors such as the Einstein telescope (ET). Birefringence can reduce the interferometric contrast and can produce dynamical disturbances in interferometers. In this work we use the method of polarization-dependent resonance-frequency analysis of Fabry-Perot-cavities containing silicon as a birefringent medium. Our measurements show a birefringence of silicon along the (111) axis of the order of Delta n approximate to 10(-7) at a laser wavelength of 1550 nm and room temperature. A model is presented that explains the results of different settings of our measurements as a superposition of elastic strains caused by external stresses in the sample and plastic strains possibly generated during the production process. An application of our theory on the proposed ET test mass geometry suggests no critical effect on birefringence due to elastic strains.}}, DOI = {{10.1088/0264-9381/33/1/015012}}, Article-Number = {{015012}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Schnabel, Roman/V-7759-2019 Lueck, Harald/F-7100-2011 }}, ORCID-Numbers = {{Lueck, Harald/0000-0001-9350-4846 Steinlechner, Jessica/0000-0002-6697-9026 Khalaidovski, Alexander/0000-0002-5163-4228}}, Unique-ID = {{ISI:000366361700012}}, } @inproceedings{ ISI:000386960500026, Author = {Eda, Kazunari and Ono, Kenji and Itoh, Yousuke}, Editor = {{Lee, HM and Oh, J}}, Title = {{Determination of mass of an isolated neutron star using continuous gravitational waves with two frequency modes: an effect of a misalignment angle}}, Booktitle = {{11TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES (AMALDI 11)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2016}}, Volume = {{716}}, Note = {{11th Edoardo Amaldi Conference on Gravitational Waves (AMALDI), Gwangju, SOUTH KOREA, JUN 21-26, 2015}}, Organization = {{Int Union Pure \& Appl Phys; Korean Astron Soc; Korean Phys Soc; Korean Federat Sci \& Technol; Natl Res Fdn; Korea Tourism Organism; Gwangju Convent Bur}}, Abstract = {{A rapidly spinning neutron star (NS) would emit a continuous gravitational wave (GW) detectable by the advanced LIGO, advanced Virgo, KAGRA and proposed third generation detectors such as the Einstein Telescope (ET). Such a GW does not propagate freely, but is affected by the Coulomb-type gravitational field of the NS itself. This effect appears as a phase shift in the GW depending on the NS mass. We have shown that mass of an isolated NS can, in principle, be determined if we could detect the continuous GW with two or more frequency modes. Indeed, our Monte Carlo simulations have demonstrated that mass of a NS with its ellipticity 10(-6) at 1 kpc is typically measurable with precision of 20\% using the ET, if the NS is precessing or has a pinned superfluid core and emits GWs with once and twice the spin frequencies. After briefly explaining our idea and results, this paper concerns with the effect of misalignment angle ({''}wobble angle{''} in the case of a precessing NS) on the mass measurement precision.}}, DOI = {{10.1088/1742-6596/716/1/012026}}, Article-Number = {{012026}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, Unique-ID = {{ISI:000386960500026}}, } @inproceedings{ ISI:000386960500030, Author = {Adya, Vaishali and Leavey, Sean and Lueck, Harald and Graef, Christian and Hild, Stefan}, Editor = {{Lee, HM and Oh, J}}, Title = {{Length sensing and control for Einstein Telescope Low Frequency}}, Booktitle = {{11TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES (AMALDI 11)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2016}}, Volume = {{716}}, Note = {{11th Edoardo Amaldi Conference on Gravitational Waves (AMALDI), Gwangju, SOUTH KOREA, JUN 21-26, 2015}}, Organization = {{Int Union Pure \& Appl Phys; Korean Astron Soc; Korean Phys Soc; Korean Federat Sci \& Technol; Natl Res Fdn; Korea Tourism Organism; Gwangju Convent Bur}}, Abstract = {{In this paper we describe a feasible length sensing and control scheme for the low frequency interferometers of the Einstein Telescope (ET-LF) along with the techniques used to optimise several optical parameters, including the length of the recycling cavities and the modulation frequencies, using two numerical interferometer simulation packages: Optickle and Finesse. The investigations have suggested the use of certain combinations of sidebands to obtain independent information about the different degrees of freedom.}}, DOI = {{10.1088/1742-6596/716/1/012030}}, Article-Number = {{012030}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, ResearcherID-Numbers = {{Lueck, Harald/F-7100-2011 Hild, Stefan/A-3864-2010 Adya, Vaishali/V-9014-2019}}, ORCID-Numbers = {{Lueck, Harald/0000-0001-9350-4846 Hild, Stefan/0000-0001-9221-6009 Adya, Vaishali/0000-0003-4955-6280}}, Unique-ID = {{ISI:000386960500030}}, } @article{ ISI:000367077100011, Author = {Jaranowski, Piotr and Schaefer, Gerhard}, Title = {{Derivation of local-in-time fourth post-Newtonian ADM Hamiltonian for spinless compact binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{92}}, Number = {{12}}, Month = {{DEC 22}}, Abstract = {{The paper gives full details of the computation within the canonical formalism of Arnowitt, Deser, and Misner of the local-in-time part of the fourth post-Newtonian, i.e. of power eight in one over speed of light, conservative Hamiltonian of spinless compact binary systems. The Hamiltonian depends only on the bodies' positions and momenta. Dirac delta distributions are taken as source functions. Their full control is furnished by dimensional continuation, by means of which the occurring ultraviolet (UV) divergences are uniquely regularized. The applied near-zone expansion of the time-symmetric Green function leads to infrared (IR) divergences. Their analytic regularization results in one single ambiguity parameter. Unique fixation of it was successfully performed in T. Damour, P. Jaranowski, and G. Schafer, Phys. Rev. D 89, 064058 (2014) through far-zone matching. Technically as well as conceptually (backscatter binding energy), the level of the Lamb shift in quantum electrodynamics is reached. In a first run a computation of all terms is performed in three-dimensional space using analytic Riesz-Hadamard regularization techniques. Then divergences are treated locally (i.e., around particles' positions for UV and in the vicinity of spatial infinity for IR divergences) by means of combined dimensional and analytic regularization. Various evolved analytic expressions are presented for the first time. The breakdown of the Leibniz rule for distributional derivatives is addressed as well as the in general nondistributive law when regularizing value of products of functions evaluated at their singular point.}}, DOI = {{10.1103/PhysRevD.92.124043}}, Article-Number = {{124043}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Jaranowski, Piotr/0000-0001-8085-3414}}, Unique-ID = {{ISI:000367077100011}}, } @article{ ISI:000368000400003, Author = {Cheng, Quan and Yu, Yun-Wei and Zheng, Xiao-Ping}, Title = {{Stochastic gravitational wave background from magnetic deformation of newly born magnetars}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2015}}, Volume = {{454}}, Number = {{3}}, Pages = {{2299-2304}}, Month = {{DEC 11}}, Abstract = {{Newly born magnetars are promising sources for gravitational wave (GW) detection due to their ultra-strong magnetic fields and high spin frequencies. Within the scenario of a growing tilt angle between the star's spin and magnetic axis, due to the effect of internal viscosity, we obtain improved estimates of the stochastic gravitational wave backgrounds (SGWBs) from magnetic deformation of newly born magnetars. We find that the GW background spectra contributed by the magnetars with ultra-strong toroidal magnetic fields of 10(17) G could roughly be divided into four segments. Most notably, in contrast to the background spectra calculated by assuming constant tilt angles chi = pi/2, the background radiation above 1000 Hz are seriously suppressed. However, the background radiation at the frequency band similar to 100-1000 Hz are moderately enhanced, depending on the strengths of the dipole magnetic fields. We suggest that if all newly born magnetars indeed have toroidal magnetic fields of 10(17) G, the produced SGWBs should show sharp variations with the observed frequency at several tens to about 100 hertz. If these features could be observed through sophisticated detection of the SGWB using the proposed Einstein Telescope, it will provide us a direct evidence of the tilt angle evolutions and further some deep understandings about the properties of newly born magnetars.}}, DOI = {{10.1093/mnras/stv2127}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Yu, Yun-Wei/G-3510-2010 yu, yun-wei/X-2088-2019}}, ORCID-Numbers = {{Yu, Yun-Wei/0000-0002-1067-1911 yu, yun-wei/0000-0002-1067-1911}}, Unique-ID = {{ISI:000368000400003}}, } @article{ ISI:000367884600006, Author = {Ding, Xuheng and Biesiada, Marek and Zhu, Zong-Hong}, Title = {{Strongly lensed gravitational waves from intrinsically faint double compact binaries - prediction for the Einstein Telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2015}}, Number = {{12}}, Month = {{DEC}}, Abstract = {{With a fantastic sensitivity improving significantly over the advanced GW detectors, Einstein Telescope (ET) will be able to observe hundreds of thousand inspiralling double compact objects per year. By virtue of gravitational lensing effect, intrinsically unobservable faint sources can be observed by ET due to the magnification by intervening galaxies. We explore the possibility of observing such faint sources amplified by strong gravitational lensing. Following our previous work, we use the merger rates of DCO (NS-NS,BH-NS,BH-BH systems) as calculated by IDominik et al.(2013). It turns out that tens to hundreds of such (lensed) extra events will be registered by ET. This will strongly broaden the ET's distance reach for signals from such coalescences to the redshift range z = 2 - 8. However, with respect to the full inspiral event catalog this magnification bias is at the level of 0.001 and should not affect much cosmological inferences.}}, DOI = {{10.1088/1475-7516/2015/12/006}}, Article-Number = {{006}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Ding, Xuheng/0000-0001-8917-2148}}, Unique-ID = {{ISI:000367884600006}}, } @article{ ISI:000365512100006, Author = {Doneva, Daniela D. and Kokkotas, Kostas D. and Pnigouras, Pantelis}, Title = {{Gravitational wave afterglow in binary neutron star mergers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{92}}, Number = {{10}}, Month = {{NOV 23}}, Abstract = {{We study in detail the f-mode secular instability for rapidly rotating neutron stars, putting emphasis on supramassive models which do not have a stable nonrotating counterpart. Such neutron stars are thought to be the generic outcome of the merger of two standard-mass neutron stars. In addition, we take into account the effects of a strong magnetic field and r-mode instability, that can drain a substantial amount of angular momentum. We find that the gravitational wave signal emitted by supramassive neutron stars can reach above the Advanced LIGO sensitivity at distance of about 20 Mpc, and the detectability is substantially enhanced for the Einstein Telescope. The event rate will be of the same order as the merging rates, while the analysis of the signal will carry information for the equation of state of the postmerging neutron stars and the strength of the magnetic fields.}}, DOI = {{10.1103/PhysRevD.92.104040}}, Article-Number = {{104040}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Kokkotas, Kostas D/B-7878-2010 }}, ORCID-Numbers = {{Kokkotas, Kostas D/0000-0001-6048-2919 Doneva, Daniela/0000-0001-6519-000X Pnigouras, Pantelis/0000-0003-1895-9431}}, Unique-ID = {{ISI:000365512100006}}, } @article{ ISI:000364412300001, Author = {Martellini, Lionel and Regimbau, Tania}, Title = {{Efficiency of the cross-correlation statistic for gravitational wave stochastic background signals with non-Gaussian noise and heterogeneous detector sensitivities}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{92}}, Number = {{10}}, Month = {{NOV 10}}, Abstract = {{Under standard assumptions including stationary and serially uncorrelated Gaussian gravitational wave stochastic background signal and noise distributions, as well as homogenous detector sensitivities, the standard cross-correlation detection statistic is known to be optimal in the sense of minimizing the probability of a false dismissal at a fixed value of the probability of a false alarm. The focus of this paper is to analyze the comparative efficiency of this statistic, vs a simple alternative statistic obtained by cross-correlating the squared measurements, in situations that deviate from such standard assumptions. We find that differences in detector sensitivities have a large impact on the comparative efficiency of the cross-correlation detection statistic, which is dominated by the alternative statistic when these differences reach 1 order of magnitude. This effect holds even when both the signal and noise distributions are Gaussian. While the presence of non-Gaussian signals has no material impact for reasonable parameter values, the relative inefficiency of the cross-correlation statistic is less prominent for fat-tailed noise distributions, but it is magnified in case noise distributions have skewness parameters of opposite signs. Our results suggest that introducing an alternative detection statistic can lead to noticeable sensitivity gains when noise distributions are possibly non-Gaussian and/or when detector sensitivities exhibit substantial differences, a situation that is expected to hold in joint detections from Advanced LIGO and Advanced Virgo, in particular in the early phases of development of the detectors, or in joint detections from Advanced LIGO and the Einstein Telescope.}}, DOI = {{10.1103/PhysRevD.92.104025}}, Article-Number = {{104025}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000364412300001}}, } @article{ ISI:000361800900027, Author = {Mytidis, Antonis and Coughlin, Michael and Whiting, Bernard}, Title = {{CONSTRAINING THE R-MODE SATURATION AMPLITUDE FROM A HYPOTHETICAL DETECTION OF R-MODE GRAVITATIONAL WAVES FROM A NEWBORN NEUTRON STAR: SENSITIVITY STUDY}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2015}}, Volume = {{810}}, Number = {{1}}, Month = {{SEP 1}}, Abstract = {{This paper consists of two related parts: in the first part we derive an expression of the moment of inertia (MOI) of a neutron star as a function of observables from a hypothetical r-mode gravitational-wave detection. For a given r-mode detection we show how the value of the MOI of a neutron star constrains the equation of state (EOS) of the matter in the core of the neutron star. Subsequently, for each candidate EOS, we derive a possible value of the saturation amplitude, a, of the r-mode oscillations on the neutron star. Additionally, we argue that an r-mode detection will provide clues about the cooling rate mechanism of the neutron star. The above physics that can be derived from a hypothetical r-mode detection constitutes our motivation for the second part of the paper. In that part we present a detection strategy to efficiently search for r-modes in gravitational-wave data. R-mode signals were injected into simulated noise colored with the advanced LIGO (aLIGO) and Einstein Telescope (ET) sensitivity curves. The r-mode waveforms used are those predicted by early theories based on polytropic EOS neutron star matter. In our best case scenario (a of order 10(-1)), the maximum detection distance when using the aLIGO sensitivity curve is similar to 1 Mpc (supernova event rate of 3-4 per century) while the maximum detection distance when using the ET sensitivity curve is similar to 10 Mpc (supernova event rate of 1-2 per year).}}, DOI = {{10.1088/0004-637X/810/1/27}}, Article-Number = {{27}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Whiting, Bernard F/0000-0002-8501-8669}}, Unique-ID = {{ISI:000361800900027}}, } @article{ ISI:000359867100004, Author = {Su, Baosan and Cao, Zhoujian and Wang, Yan and Yeh, Hsien-Chi}, Title = {{Parameter estimation of eccentric inspiraling compact binaries using an enhanced post circular model for ground-based detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{92}}, Number = {{4}}, Month = {{AUG 19}}, Abstract = {{Inspiraling compact binaries have been identified as one of the most promising sources for gravitational-wave detection. These binaries are always expected to have been circularized by the gravitational radiation when they enter the detector's frequency band. However, recent studies indicate that some binaries may still possess a significant eccentricity. In light of the enhanced post-circular waveform model for eccentric binaries in the frequency domain, we do a systematic study of the possible signal-to-noise ratio loss if one uses quasicircular waveform templates to analyze the eccentric signal, and revisit the problem of parameter estimation of gravitational-wave chirp signals from eccentric compact binaries. We confirm previous results from other researchers that the resulting signal-to-noise ratio loss becomes larger than 5\% for eccentricity bigger than 0.1 and the resulting parameter estimation bias is more than 0.1\%. We study the parameter estimation accuracy for such a waveform with different initial eccentricities from 0.1 to 0.4 by using the Fisher matrix method. As expected, the eccentricity improves the parameter estimation accuracy significantly by breaking degeneracies between different parameters. Particularly, we find that the eccentricity errors improve by 2 orders of magnitude from 10(-2) to 10(-4) when eccentricity grows from 0.1 to 0.4, and the estimated errors of the chirp mass are about 10(-3) for a binary black hole using the Advanced LIGO detector. For the Einstein Telescope detector, the estimated accuracy of parameters will be 2 orders of magnitude higher.}}, DOI = {{10.1103/PhysRevD.92.044034}}, Article-Number = {{044034}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Cao, Zhoujian/AAH-2470-2020}}, ORCID-Numbers = {{Cao, Zhoujian/0000-0002-1932-7295}}, Unique-ID = {{ISI:000359867100004}}, } @article{ ISI:000356339300012, Author = {Haskell, B. and Priymak, M. and Patruno, A. and Oppenoorth, M. and Melatos, A. and Lasky, P. D.}, Title = {{Detecting gravitational waves from mountains on neutron stars in the advanced detector era}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2015}}, Volume = {{450}}, Number = {{3}}, Pages = {{2393-2403}}, Month = {{JUL 1}}, Abstract = {{Rapidly rotating neutron stars (NSs) in low-mass X-ray binaries (LMXBs) are thought to be interesting sources of gravitational waves (GWs) for current and next generation ground-based detectors, such as Advanced LIGO and the Einstein Telescope. The main reason is that many of the NSs in these systems appear to be spinning well below their Keplerian break-up frequency, and it has been suggested that torques associated with GW emission may be setting the observed spin period. This assumption has been used extensively in the literature to assess the strength of the likely GW signal. There is now, however, a significant amount of theoretical and observation work that suggests that this may not be the case, and that GW emission is unlikely to be setting the spin equilibrium period in many systems. In this paper we take a different starting point and predict the GW signal strength for two physical mechanisms that are likely to be at work in LMXBs: crustal mountains due to thermal asymmetries and magnetically confined mountains. We find that thermal crustal mountains in transient LMXBs are unlikely to lead to detectable GW emission, while persistent systems are good candidates for detection by Advanced LIGO and by the Einstein Telescope. Detection prospects are pessimistic for the magnetic mountain case, unless the NS has a buried magnetic field of B a parts per thousand 10(12) G, well above the typically inferred exterior dipole fields of these objects. Nevertheless, if a system were to be detected by a GW observatory, cyclotron resonant scattering features in the X-ray emission could be used to distinguish between the two different scenarios.}}, DOI = {{10.1093/mnras/stv726}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Patruno, Alessandro/T-6621-2019}}, ORCID-Numbers = {{Lasky, Paul/0000-0003-3763-1386 Melatos, Andrew/0000-0003-4642-141X Haskell, Brynmor/0000-0002-8255-3519 Patruno, Alessandro/0000-0002-6459-0674}}, Unique-ID = {{ISI:000356339300012}}, } @article{ ISI:000354953600002, Author = {Kroker, Stefanie and Nawrodt, Ronny}, Title = {{The Einstein Telescope}}, Journal = {{IEEE INSTRUMENTATION \& MEASUREMENT MAGAZINE}}, Year = {{2015}}, Volume = {{18}}, Number = {{3}}, Pages = {{4-8}}, Month = {{JUN}}, DOI = {{10.1109/MIM.2015.7108211}}, ISSN = {{1094-6969}}, EISSN = {{1941-0123}}, ResearcherID-Numbers = {{Kroker, Stefanie/Q-8871-2016 Kroker, Stefanie/V-3419-2017}}, ORCID-Numbers = {{Kroker, Stefanie/0000-0002-7584-7359 Kroker, Stefanie/0000-0002-7584-7359}}, Unique-ID = {{ISI:000354953600002}}, } @article{ ISI:000354189500021, Author = {Geng, J. J. and Huang, Y. F. and Lu, T.}, Title = {{COALESCENCE OF STRANGE-QUARK PLANETS WITH STRANGE STARS: A NEW KIND OF SOURCE FOR GRAVITATIONAL WAVE BURSTS}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2015}}, Volume = {{804}}, Number = {{1}}, Month = {{MAY 1}}, Abstract = {{Strange-quark matter (SQM) may be the true ground state of hadronic matter, indicating that the observed pulsars may actually be strange stars (SSs), but not neutron stars. According to the SQM hypothesis, the existence of a hydrostatically stable sequence of SQM stars has been predicted, ranging from 1 to 2 solar mass SSs, to smaller strange dwarfs and even strange planets. While gravitational wave (GW) astronomy is expected to open a new window to the universe, it will shed light on the search for SQM stars. Here we show that due to their extreme compactness, strange planets can spiral very close to their host SSs without being tidally disrupted. Like inspiraling neutron stars or black holes, these systems would serve as new sources of GW bursts, producing strong GWs at the final stage. The events occurring in our local universe can be detected by upcoming GW detectors, such as Advanced LIGO and the Einstein Telescope. This effect provides a unique probe to SQM objects and is hopefully a powerful tool for testing the SQM hypothesis.}}, DOI = {{10.1088/0004-637X/804/1/21}}, Article-Number = {{21}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{GENG, Jin-Jun/K-1684-2019 Huang, Y.F./G-7274-2015 Geng, Jin-Jun/K-4623-2019}}, ORCID-Numbers = {{Geng, Jin-Jun/0000-0001-9648-7295}}, Unique-ID = {{ISI:000354189500021}}, } @article{ ISI:000354021000002, Author = {Danilishin, S. L. and Graef, C. and Leavey, S. S. and Hennig, J. and Houston, E. A. and Pascucci, D. and Steinlechner, S. and Wright, J. and Hild, S.}, Title = {{Quantum noise of non-ideal Sagnac speed meter interferometer with asymmetries}}, Journal = {{NEW JOURNAL OF PHYSICS}}, Year = {{2015}}, Volume = {{17}}, Month = {{APR 16}}, Abstract = {{The speed meter concept has been identified as a technique that can potentially provide laser-interferometric measurements at a sensitivity level which surpasses the standard quantum limit (SQL) over a broad frequency range. As with other sub-SQL measurement techniques, losses play a central role in speed meter interferometers and they ultimately determine the quantum noise limited sensitivity that can be achieved. So far in the literature, the quantum noise limited sensitivity has only been derived for lossless or lossy cases using certain approximations (for instance that the arm cavity round trip loss is small compared to the arm cavity mirror transmission). In this article we present a generalized, analytical treatment of losses in speed meters that allows accurate calculation of the quantum noise limited sensitivity of Sagnac speed meters with arm cavities. In addition, our analysis allows us to take into account potential imperfections in the interferometer such as an asymmetric beam splitter or differences of the reflectivities of the two arm cavity input mirrors. Finally, we use the examples of the proof-of-concept Sagnac speed meter currently under construction in Glasgow and a potential implementation of a Sagnac speed meter in the Einstein Telescope to illustrate how our findings affect Sagnac speed meters with metre-and kilometre-long baselines.}}, DOI = {{10.1088/1367-2630/17/4/043031}}, Article-Number = {{043031}}, ISSN = {{1367-2630}}, ResearcherID-Numbers = {{Steinlechner, Sebastian S/D-5781-2013 Danilishin, Stefan/K-7262-2012 Graef, Christian/J-3167-2015 Hild, Stefan/A-3864-2010 }}, ORCID-Numbers = {{Steinlechner, Sebastian S/0000-0003-4710-8548 Danilishin, Stefan/0000-0001-7758-7493 Graef, Christian/0000-0002-4535-2603 Hild, Stefan/0000-0001-9221-6009 Leavey, Sean/0000-0001-8253-0272}}, Unique-ID = {{ISI:000354021000002}}, } @article{ ISI:000352686600005, Author = {Ono, Kenji and Eda, Kazunari and Itoh, Yousuke}, Title = {{New estimation method for mass of an isolated neutron star using gravitational waves}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{91}}, Number = {{8}}, Month = {{APR 13}}, Abstract = {{We investigate the possibility of estimating the mass of an isolated rapidly rotating neutron star (NS) from a continuous gravitational wave (GW) signal emitted by the NS. When the GW passes through the gravitational potential of the NS, the GW takes a slightly longer time to travel to an observer than it does in the absence of the NS. Such a time dilation effect holds also for photons and is often referred to as the gravitational time delay (or the Shapiro time delay). Correspondingly, the phase of the GW from the NS shifts due to the Coulomb-type gravitational potential of the NS, and the resulting logarithmic phase shift depends on the mass, the spin frequency of the NS, and the distance to the NS. We show that the NS mass can, in principle, be obtained by making use of the phase-shift difference between two modes of the continuous GW such as once and twice spin frequency modes induced by a freely precessing NS or a NS containing a pinned superfluid core. We estimate the measurement accuracy of the NS mass using Monte Carlo simulations and find that the mass of the NS with its spin frequency 500 Hz and its ellipticity 10(-6) at 1 kpc is typically measurable with an accuracy of 20\% using the Einstein Telescope.}}, DOI = {{10.1103/PhysRevD.91.084032}}, Article-Number = {{084032}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000352686600005}}, } @article{ ISI:000352593900001, Author = {Damour, Thibault and Jaranowski, Piotr and Schaefer, Gerhard}, Title = {{Fourth post-Newtonian effective one-body dynamics}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{91}}, Number = {{8}}, Month = {{APR 10}}, Abstract = {{The conservative dynamics of gravitationally interacting two-point-mass systems has been recently determined at the fourth post-Newtonian (4PN) approximation {[}T. Damour, P. Jaranowski, and G. Schafer, Phys. Rev. D 89, 064058 (2014)], and found to be nonlocal in time. We show how to transcribe this dynamics within the effective one-body (EOB) formalism. To achieve this EOB transcription, we develop a new strategy involving the (infinite-)order-reduction of a nonlocal dynamics to an ordinary action-angle Hamiltonian. Our final, equivalent EOB dynamics comprises two (local) radial potentials, A(r) and (D) over bar (r), and a nongeodesic mass-shell contribution Q(r, p(r)) given by an infinite series of even powers of the radial momentum p(r). Using an effective action technique, we complete our 4PN-level results by deriving two different, higher-order conservative contributions linked to tail-transported hereditary effects: the 5PN-level EOB logarithmic terms, as well as the 5.5PN-level, half-integral terms. We compare our improved analytical knowledge to previous, numerical gravitational-self-force computation of precession effects.}}, DOI = {{10.1103/PhysRevD.91.084024}}, Article-Number = {{084024}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Jaranowski, Piotr/0000-0001-8085-3414}}, Unique-ID = {{ISI:000352593900001}}, } @article{ ISI:000349858800001, Author = {Steinlechner, Jessica and Martin, Iain W. and Hough, Jim and Krueger, Christoph and Rowan, Sheila and Schnabel, Roman}, Title = {{Thermal noise reduction and absorption optimization via multimaterial coatings}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{91}}, Number = {{4}}, Month = {{FEB 3}}, Abstract = {{Future gravitational wave detectors (GWDs) such as Advanced LIGO upgrades and the Einstein Telescope are planned to operate at cryogenic temperatures using crystalline silicon (cSi) test-mass mirrors at an operation wavelength of 1550 nm. The reduction in temperature in principle provides a direct reduction in coating thermal noise, but the presently used coating stacks which are composed of silica (SiO2) and tantala (Ta2O5) show cryogenic loss peaks which results in less thermal noise improvement than might be expected. Due to low mechanical loss at low temperature amorphous silicon (aSi) is a very promising candidate material for dielectric mirror coatings and could replace Ta2O5. Unfortunately, such an aSi/SiO2 coating is not suitable for use in GWDs due to high optical absorption in aSi coatings. We explore the use of a three material based coating stack. In this multimaterial design the low absorbing Ta2O5 in the outermost coating layers significantly reduces the incident light power, while aSi is used only in the lower bilayers to maintain low optical absorption. Such a coating design would enable a reduction of Brownian thermal noise by 25\%. We show experimentally that an optical absorption of only (5.3 +/- 0.4) ppm at 1550 nm should be achievable.}}, DOI = {{10.1103/PhysRevD.91.042001}}, Article-Number = {{042001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Martin, Iain/V-1198-2018 Schnabel, Roman/V-7759-2019 }}, ORCID-Numbers = {{Martin, Iain/0000-0001-7300-9151 Steinlechner, Jessica/0000-0002-6697-9026}}, Unique-ID = {{ISI:000349858800001}}, } @article{ ISI:000349467000058, Author = {Kowalska-Leszczynska, I. and Regimbau, T. and Bulik, T. and Dominik, M. and Belczynski, K.}, Title = {{Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2015}}, Volume = {{574}}, Month = {{FEB}}, Abstract = {{Context. Recent studies on stellar evolution have shown that the properties of compact objects strongly depend on the metallicity of the environment in which they were formed. Aims. Using some very simple assumptions on the metallicity of the stellar populations, we explore how this property affects the unresolved gravitational-wave background from extragalactic compact binaries. Methods. We obtained a suit of models using population synthesis code, estimated the gravitational-wave background they produce, and discuss its detectability with second-(advanced LIGO, advanced Virgo) and third-(Einstein Telescope) generation detectors. Results. Our results show that the background is dominated by binary black holes for all considered models in the frequency range of terrestrial detectors, and that it could be detected in most cases by advanced LIGO/Virgo, and with Einstein Telescope with a very high signal-to-noise ratio. The observed peak in a gravitational-wave spectrum depends on the metallicity of the stellar population.}}, DOI = {{10.1051/0004-6361/201424417}}, Article-Number = {{A58}}, ISSN = {{1432-0746}}, ResearcherID-Numbers = {{Bulik, Tomasz/AAJ-6742-2020 }}, ORCID-Numbers = {{Bulik, Tomasz/0000-0003-2045-4803 Kowalska-Leszczynska, Izabela/0000-0002-6569-3800}}, Unique-ID = {{ISI:000349467000058}}, } @article{ ISI:000349866000002, Author = {Jaranowski, Piotr and Mach, Patryk and Malec, Edward and Pirog, Michal}, Title = {{General-relativistic versus Newtonian: Geometric dragging and dynamic antidragging in stationary self-gravitating disks in the first post-Newtonian approximation}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2015}}, Volume = {{91}}, Number = {{2}}, Month = {{JAN 28}}, Abstract = {{We evaluate general-relativistic effects in the motion of stationary self-gravitating accretion disks around a Schwarzschild black hole, assuming the first post-Newtonian (1PN) approximation. There arises an integrability condition that leads to the emergence of two types of general-relativistic corrections to a Newtonian rotation curve. The well-known geometric dragging of frames accelerates rotation, but the hitherto unknown dynamic term, that reflects the disk structure, decelerates rotation. The net result can diminish the Newtonian angular velocity of rotation in a central disk zone, but the geometric dragging of frames dominates in the disk boundary zone. Both effects are nonlinear in nature, and they disappear in the limit of test fluids. Dust disks can only be geometrically dragged, while uniformly rotating gaseous disks are untouched at the 1PN order. General-relativistic contributions can strongly affect rotation periods in Keplerian motion for compact systems.}}, DOI = {{10.1103/PhysRevD.91.024039}}, Article-Number = {{024039}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Mach, Patryk/AAQ-5447-2020 Mach, Patryk/N-3511-2015 }}, ORCID-Numbers = {{Mach, Patryk/0000-0003-1493-8668 Jaranowski, Piotr/0000-0001-8085-3414}}, Unique-ID = {{ISI:000349866000002}}, } @article{ ISI:000347295300004, Author = {Beker, M. G. and van den Brand, J. F. J. and Rabeling, D. S.}, Title = {{Subterranean ground motion studies for the Einstein Telescope}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2015}}, Volume = {{32}}, Number = {{2}}, Month = {{JAN 22}}, Abstract = {{Seismic motion limits the low-frequency sensitivity of ground-based gravitational wave detectors. A conceptual design study into the feasibility of a future-generation gravitational wave observatory, coined the Einstein Telescope, has been completed. As part of this design phase, we performed a ground motion study to determine the seismic noise characteristics at various sites across the globe. This investigation focused on underground sites and encompassed a variety of geologies, including clay, salt, and hard rock, at 15 locations in nine European countries, the USA, and Japan. In addition, we analyzed data from the Virtual European Broadband Seismograph Network to characterize European seismic motion. We show that, in the region of interest for future-generation gravitational wave detectors (1-10 Hz), seismic motion is dominated by activity from anthropogenic sources. A number of sites were found that exhibited a reduction in seismic power of several orders of magnitude with respect to current detector sites, thus making it possible to set requirements for the Einstein Telescope seismic noise environment.}}, DOI = {{10.1088/0264-9381/32/2/025002}}, Article-Number = {{025002}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, Unique-ID = {{ISI:000347295300004}}, } @article{ ISI:000348214500067, Author = {Regimbau, T. and Siellez, K. and Meacher, D. and Gendre, B. and Boer, M.}, Title = {{REVISITING COINCIDENCE RATE BETWEEN GRAVITATIONAL WAVE DETECTION AND SHORT GAMMA-RAY BURST FOR THE ADVANCED AND THIRD GENERATION}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2015}}, Volume = {{799}}, Number = {{1}}, Month = {{JAN 20}}, Abstract = {{We use realistic Monte Carlo simulations including both gravitational-wave (GW) and short gamma-ray burst (sGRB) selection effects to revisit the coincident rate of binary systems composed of two neutron stars or a neutron star and a black hole. We show that the fraction of GW triggers that can be observed in coincidence with sGRBs is proportional to the beaming factor at z = 0, but increases with the distance until it reaches 100\% at the GW detector horizon distance. When this is taken into account the rate is improved by a factor of three compared to the simple beaming factor correction. We provide an estimate of the performance future GRB detectors should achieve in order to fully exploit the potentiality of the planned third-generation GW antenna Einstein Telescope, and we propose a simple method to constrain the beaming angle of sGRBs.}}, DOI = {{10.1088/0004-637X/799/1/69}}, Article-Number = {{69}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Boer, Michel/Q-4428-2019 Gendre, Bruce/O-2923-2013}}, ORCID-Numbers = {{Boer, Michel/0000-0001-9157-4349 Gendre, Bruce/0000-0002-9077-2025}}, Unique-ID = {{ISI:000348214500067}}, } @inproceedings{ ISI:000373970200006, Author = {Aloy, Miguel A. and Cerda-Duran, Pablo and Obergaulinger, Martin and DeBrye, Nicolas and Font, Jose A.}, Editor = {{Pogorelov, NV and Audit, E and Zank, GP}}, Title = {{Gravitational Wave Signals in Black-hole-forming Core Collapse}}, Booktitle = {{NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2014}}, Series = {{Astronomical Society of the Pacific Conference Series}}, Year = {{2015}}, Volume = {{498}}, Pages = {{35-40}}, Note = {{9th Annual International Conference on Numerical Modeling of Space Plasma Flows (ASTRONUM-2014), Long Beach, CA, JUN 23-27, 2014}}, Organization = {{Univ Alabama, Ctr Space Plasma \& Aeronomic Res; CEA-CNRS-INRIA-UPsud-UVSQ, Maison Simulat}}, Abstract = {{We aim to analyze the emission of gravitational waves in the collapsar scenario of long gamma-ray bursts using numerical simulations of collapsing stellar cores. Our general relativistic numerical simulations show that the phase during which the proto-neutron star (PNS) survives before ultimately collapsing to a black hole is particularly optimal for gravitational wave emission. The high-amplitude waves last for a couple of seconds and show a remarkable quasi-periodicity associated with the episodes of convection and the subsequent nonlinear development of the standing-accretion shock instability (SASI). We identify the frequencies associated with the presence of g-modes and with the SASI motions at the PNS surface. The gravitational waves emitted reach large enough amplitudes to be detected with third-generation detectors as the Einstein Telescope within a Virgo cluster volume at rates less than or similar to 0.1 y(-1).}}, ISSN = {{1050-3390}}, ISBN = {{978-1-58381-880-0}}, ResearcherID-Numbers = {{Cerda-Duran, Pablo/D-7857-2015 Font, Jose/K-5198-2014}}, ORCID-Numbers = {{Cerda-Duran, Pablo/0000-0003-4293-340X Font, Jose/0000-0001-6650-2634}}, Unique-ID = {{ISI:000373970200006}}, } @article{ ISI:000347245100025, Author = {Dall'Osso, Simone and Giacomazzo, Bruno and Perna, Rosalba and Stella, Luigi}, Title = {{GRAVITATIONAL WAVES FROM MASSIVE MAGNETARS FORMED IN BINARY NEUTRON STAR MERGERS}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2015}}, Volume = {{798}}, Number = {{1}}, Month = {{JAN 1}}, Abstract = {{Binary neutron star (NS) mergers are among the most promising sources of gravitational waves (GWs), as well as candidate progenitors for short gamma-ray bursts (SGRBs). Depending on the total initial mass of the system and the NS equation of state (EOS), the post-merger phase can be characterized by a prompt collapse to a black hole or by the formation of a supramassive NS, or even a stable NS. In the latter cases of post-merger NS (PMNS) formation, magnetic field amplification during the merger will produce a magnetar and induce a mass quadrupole moment in the newly formed NS. If the timescale for orthogonalization of the magnetic symmetry axis with the spin axis is smaller than the spindown time, the NS will radiate its spin down energy primarily via GWs. Here we study this scenario for the various outcomes of NS formation: we generalize the set of equilibrium states for a twisted torus magnetic configuration to include solutions that, for the same external dipolar field, carry a larger magnetic energy reservoir; we hence compute the magnetic ellipticity for such configurations, and the corresponding strength of the expected GW signal as a function of the relative magnitude of the dipolar and toroidal field components. The relative number of GW detections from PMNSs and from binary NSs is a very strong function of the NS EOS, being higher (similar to 1\%) for the stiffest EOSs and negligibly small for the softest ones. For intermediate-stiffness EOSs, such as the n = 4/7 polytrope recently used by Giacomazzo and Perna or the GM1 used by Lasky et al., the relative fraction is 0.3\%; correspondingly, we estimate a GW detection rate from stable PMNSs of similar to 0.1-1 yr(-1) with advanced detectors, and of similar to 100-1000 yr(-1) with detectors of third generation such as the Einstein Telescope. Measurement of such GW signals would provide constraints on the NS EOS and, in connection with an SGRB, on the nature of the binary progenitors giving rise to these events.}}, DOI = {{10.1088/0004-637X/798/1/25}}, Article-Number = {{25}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Giacomazzo, Bruno/I-8088-2012 }}, ORCID-Numbers = {{Giacomazzo, Bruno/0000-0002-6947-4023 Stella, Luigi/0000-0002-0018-1687}}, Unique-ID = {{ISI:000347245100025}}, } @article{ ISI:000345395400043, Author = {Moraes, Pedro H. R. S. and Miranda, Oswaldo D.}, Title = {{Constraining the brane tension in Randall-Sundrum cosmology through gravitational waves from binary neutron stars}}, Journal = {{ASTROPHYSICS AND SPACE SCIENCE}}, Year = {{2014}}, Volume = {{354}}, Number = {{2}}, Pages = {{645-649}}, Month = {{DEC}}, Abstract = {{When describing our world as a brane embedded in a higher dimensional hypersurface (or bulk) we are led to consider the existence of some new parameters related to the extra dimension or to the brane itself, as the brane tension density parameter Omega (lambda) . We show that gravitational waves emitted by binary neutron stars can constrain the values that Omega (lambda) might assume. Our approach is applied to the perspectives of Einstein Telescope gravitational wave detector and results in Omega (lambda) a parts per thousand currency sign0.037, which is in agreement with other estimates obtained from different methods in the literature.}}, DOI = {{10.1007/s10509-014-2121-6}}, ISSN = {{0004-640X}}, EISSN = {{1572-946X}}, ResearcherID-Numbers = {{Miranda, Oswaldo/C-4748-2012}}, ORCID-Numbers = {{Miranda, Oswaldo/0000-0002-0109-2483}}, Unique-ID = {{ISI:000345395400043}}, } @article{ ISI:000344607300017, Author = {Graef, C. and Barr, B. W. and Bell, A. S. and Campbell, F. and Cumming, A. V. and Danilishin, S. L. and Gordon, N. A. and Hammond, G. D. and Hennig, J. and Houston, E. A. and Huttner, S. H. and Jones, R. A. and Leavey, S. S. and Lueck, H. and Macarthur, J. and Marwick, M. and Rigby, S. and Schilling, R. and Sorazu, B. and Spencer, A. and Steinlechner, S. and Strain, K. A. and Hild, S.}, Title = {{Design of a speed meter interferometer proof-of-principle experiment}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2014}}, Volume = {{31}}, Number = {{21}}, Month = {{NOV 7}}, Abstract = {{The second generation of large scale interferometric gravitational wave (GW) detectors will be limited by quantum noise over a wide frequency range in their detection band. Further sensitivity improvements for future upgrades or new detectors beyond the second generation motivate the development of measurement schemes to mitigate the impact of quantum noise in these instruments. Two strands of development are being pursued to reach this goal, focusing both on modifications of the well-established Michelson detector configuration and development of different detector topologies. In this paper, we present the design of the world's first Sagnac speed meter (SSM) interferometer, which is currently being constructed at the University of Glasgow. With this proof-of-principle experiment we aim to demonstrate the theoretically predicted lower quantum noise in a Sagnac interferometer compared to an equivalent Michelson interferometer, to qualify SSM for further research towards an implementation in a future generation large scale GW detector, such as the planned Einstein telescope observatory.}}, DOI = {{10.1088/0264-9381/31/21/215009}}, Article-Number = {{215009}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Danilishin, Stefan/K-7262-2012 Steinlechner, Sebastian S/D-5781-2013 Lueck, Harald/F-7100-2011 Barr, Bryan/G-3348-2019 Bell, Angus/E-7312-2011 Hild, Stefan/A-3864-2010 Graef, Christian/J-3167-2015 Strain, Kenneth/D-5236-2011 Sorazu, Borja/H-6966-2018}}, ORCID-Numbers = {{Danilishin, Stefan/0000-0001-7758-7493 Steinlechner, Sebastian S/0000-0003-4710-8548 Lueck, Harald/0000-0001-9350-4846 Barr, Bryan/0000-0002-5232-2736 Bell, Angus/0000-0003-1523-0821 Hild, Stefan/0000-0001-9221-6009 Graef, Christian/0000-0002-4535-2603 Strain, Kenneth/0000-0002-2066-5355 Leavey, Sean/0000-0001-8253-0272 Spencer, Andrew/0000-0003-4418-3366 Hammond, Giles/0000-0002-1414-3622 Sorazu, Borja/0000-0002-6178-3198}}, Unique-ID = {{ISI:000344607300017}}, } @article{ ISI:000344030000006, Author = {Huerta, E. A. and Kumar, Prayush and McWilliams, Sean T. and O'Shaughnessy, Richard and Yunes, Nicolas}, Title = {{Accurate and efficient waveforms for compact binaries on eccentric orbits}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{90}}, Number = {{8}}, Month = {{OCT 10}}, Abstract = {{Compact binaries that emit gravitational waves in the sensitivity band of ground-based detectors can have non-negligible eccentricities just prior to merger, depending on the formation scenario. We develop a purely analytic, frequency-domain model for gravitational waves emitted by compact binaries on orbits with small eccentricity, which reduces to the quasicircular post-Newtonian approximant TAYLORF2 at zero eccentricity and to the postcircular approximation of Yunes et al. {[}Phys. Rev. D 80, 084001 (2009)] at small eccentricity. Our model uses a spectral approximation to the (post-Newtonian) Kepler problem to model the orbital phase as a function of frequency, accounting for eccentricity effects up to O(e(8) ) at each post-Newtonian order. Our approach accurately reproduces an alternative time-domain eccentric waveform model for e is an element of{[} 0, 0.4 and binaries with total mass. less than or similar to 12M(circle dot). As an application, we evaluate the signal amplitude that eccentric binaries produce in different networks of existing and forthcoming gravitational waves detectors. Assuming a population of eccentric systems containing black holes and neutron stars that is uniformly distributed in comoving volume, we estimate that second-generation detectors like Advanced LIGO could detect approximately 0.1-10 events per year out to redshift z similar to 0.2, while an array of Einstein Telescope detectors could detect hundreds of events per year to redshift z similar to 2.3.}}, DOI = {{10.1103/PhysRevD.90.084016}}, Article-Number = {{084016}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{O'Shaughnessy, Richard/AAA-3625-2021 Yunes, Nicolas/AAG-3146-2019 }}, ORCID-Numbers = {{O'Shaughnessy, Richard/0000-0001-5832-8517 Yunes, Nicolas/0000-0001-6147-1736 Huerta, Eliu/0000-0002-9682-3604 Kumar, Prayush/0000-0001-5523-4603}}, Unique-ID = {{ISI:000344030000006}}, } @article{ ISI:000344031800001, Author = {Messenger, C. and Takami, Kentaro and Gossan, Sarah and Rezzolla, Luciano and Sathyaprakash, B. S.}, Title = {{Source Redshifts from Gravitational-Wave Observations of Binary Neutron Star Mergers}}, Journal = {{PHYSICAL REVIEW X}}, Year = {{2014}}, Volume = {{4}}, Number = {{4}}, Month = {{OCT 8}}, Abstract = {{Inspiraling compact binaries as standard sirens will become an invaluable tool for cosmology when we enter the gravitational-wave detection era. However, a degeneracy in the information carried by gravitational waves between the total rest-frame mass M and the redshift z of the source implies that neither can be directly extracted from the signal; only the combination M(1 + z), the redshifted mass, can be directly extracted from the signal. Recent work has shown that for third-generation detectors, a tidal correction to the gravitational-wave phase in the late-inspiral signal of binary neutron star systems can be used to break the mass-redshift degeneracy. Here, we propose to use the signature encoded in the postmerger signal allowing the accurate extraction of the intrinsic rest-frame mass of the source, in turn permitting the determination of source redshift and luminosity distance. The entirety of this analysis method and any subsequent cosmological inference derived from it would be obtained solely from gravitational-wave observations and, hence, would be independent of the cosmological distance ladder. Using numerical simulations of binary neutron star mergers of different mass, we model gravitational-wave signals at different redshifts and use a Bayesian parameter estimation to determine the accuracy with which the redshift and mass can be extracted. We find that for a known illustrative neutron star equation of state and using the Einstein telescope, the median of the 1 sigma confidence regions in redshift corresponds to similar to 10\%-20\% uncertainties at redshifts of z < 0.04.}}, DOI = {{10.1103/PhysRevX.4.041004}}, Article-Number = {{041004}}, ISSN = {{2160-3308}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014 }}, ORCID-Numbers = {{Sathyaprakash, Bangalore/0000-0003-3845-7586 Messenger, Chris/0000-0001-7488-5022}}, Unique-ID = {{ISI:000344031800001}}, } @article{ ISI:000345990800081, Author = {Biesiada, Marek and Ding, Xuheng and Piorkowska, Aleksandra and Zhu, Zong-Hong}, Title = {{Strong gravitational lensing of gravitational waves from double compact binaries - perspectives for the Einstein Telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2014}}, Number = {{10}}, Month = {{OCT}}, Abstract = {{Gravitational wave (GW) experiments are entering their advanced stage which should soon open a new observational window on the Universe. Looking into this future, the Einstein Telescope (ET) was designed to have a fantastic sensitivity improving significantly over the advanced GW detectors. One of the most important astrophysical GW sources supposed to be detected by the ET in large numbers are double compact objects (DCO) and some of such events should be gravitationally lensed by intervening galaxies. We explore the prospects of observing gravitationally lensed inspiral DCO events in the ET. This analysis is a significant extension of our previous paper {[}6]. We are using the intrinsic merger rates of the whole class of DCO (NS-NS,BH-NS,BH-BH)located at different redshifts as calculated by {[}5] by using StarTrack population synthesis evolutionary code. We discuss in details predictions from each evolutionary scenario. Our general conclusion is that ET would register about 50-100 strongly lensed inspiral events per year. Only the scenario in which nascent BHs receive strong kick gives the predictions of a few events per year. Such lensed events would be dominated by the BH-BH merging binary systems. Our results suggest that during a few years of successful operation ET will provide a considerable catalog of strongly lensed events.}}, DOI = {{10.1088/1475-7516/2014/10/080}}, Article-Number = {{080}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020 }}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304 Ding, Xuheng/0000-0001-8917-2148}}, Unique-ID = {{ISI:000345990800081}}, } @article{ ISI:000341484200011, Author = {Degallaix, J. and Komma, J. and Forest, D. and Hofmann, G. and Granata, M. and Heinert, D. and Schwarz, C. and Nawrodt, R. and Pinard, L. and Michel, C. and Flaminio, R. and Cagnoli, G.}, Title = {{Measurement of the optical absorption of bulk silicon at cryogenic temperature and the implication for the Einstein Telescope}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2014}}, Volume = {{31}}, Number = {{18}}, Month = {{SEP 21}}, Abstract = {{We report in this article on the measurement of the optical absorption of moderately doped crystalline silicon samples at 1550 nm, which is a candidate material for the main optics of the low temperature interferometer of the Einstein Telescope (ET). We observe a nearly constant absorption from room temperature down to cryogenic temperatures for two silicon samples presenting an optical absorption of 0.029 cm(-1) and 780 ppm cm(-1), both crystals doped with boron. This is in contradiction to what was assumed previously-a negligible optical absorption at low temperature due to the carrier freezeout. As the main consequence, if the silicon intrinsic absorption can not be lowered, the cross section of the mirror suspension of the ET must be increased to be able to carry away the excess heat generated by the partially absorbed laser beam during the operation of the interferometer.}}, DOI = {{10.1088/0264-9381/31/18/185010}}, Article-Number = {{185010}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ORCID-Numbers = {{Granata, Massimo/0000-0003-3275-1186}}, Unique-ID = {{ISI:000341484200011}}, } @article{ ISI:000341265400002, Author = {Cao, Zhoujian and Li, Li-Fang and Wang, Yan}, Title = {{Gravitational lensing effects on parameter estimation in gravitational wave detection with advanced detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{90}}, Number = {{6}}, Month = {{SEP 4}}, Abstract = {{The gravitational lensing effect is important to the detection of electromagnetic signals in astrophysics. The gravitational wave lensing effect has also been found significant to gravitational wave detection in the past decade. Recent analysis shows that the lensing events for advanced detectors could be quite plausible. The black holes in our Milky Way Galaxy may play the role of lens objects. These facts motivate us to study the lensing effects on gravitational wave signals for advanced detectors. Taking advanced LIGO and Einstein Telescope for examples, we investigate the lensing effects on the parameter extraction of gravitational wave signals. Using the Markov chain Monte Carlo simulation together with matched filtering methods, we find that the lensing effect for a lens object with small mass is negligible. But when the mass of the lens object increases to larger than 1000M(circle dot) the lensing effect becomes important. Using the template without lensing corrections would result in loss of signal detections. In contrast if we consider templates with lensing effects, the lensed signal may provide much information about the lens black hole. These facts may give us a new way to determine the parameters of the lensing object. For example, this kind of signal may also help us estimate the mass and the distance of the supermassive black hole hosted at the center of our Galaxy.}}, DOI = {{10.1103/PhysRevD.90.062003}}, Article-Number = {{062003}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Cao, Zhoujian/AAH-2470-2020}}, ORCID-Numbers = {{Cao, Zhoujian/0000-0002-1932-7295}}, Unique-ID = {{ISI:000341265400002}}, } @article{ ISI:000341265400007, Author = {Meidam, J. and Agathos, M. and Van Den Broeck, C. and Veitch, J. and Sathyaprakash, B. S.}, Title = {{Testing the no-hair theorem with black hole ringdowns using TIGER}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{90}}, Number = {{6}}, Month = {{SEP 4}}, Abstract = {{The Einstein Telescope, a proposed third-generation gravitational-wave observatory, would enable tests of the no-hair theorem by looking at the characteristic frequencies and damping times of black hole ringdown signals. In previous work it was shown that with a single 500-1000 M-circle dot. black hole at a distance less than or similar to 6 Gpc (or redshift z less than or similar to 1), deviations of a few percent in the frequencies and damping times of dominant and subdominant modes would be within the range of detectability. Given that such sources may be relatively rare, it is of interest to see how well the no-hair theorem can be tested with events at much larger distances and with smaller signal-to-noise ratios, thus accessing a far bigger volume of space and a larger number of sources. We employ a model-selection scheme called TIGER (Test Infrastructure for GEneral Relativity), which was originally developed to test general relativity with weak binary coalescence signals that will be seen in second-generation detectors, such as Advanced LIGO and Advanced Virgo. TIGER is well suited for the regime of low signal-to-noise ratios, and information from a population of sources can be combined so as to arrive at a stronger test. By performing a range of simulations using the expected noise power spectral density of the Einstein Telescope, we show that with TIGER, similar deviations from the no-hair theorem (such as those considered in previous works) will be detectable with great confidence using O(10) sources distributed uniformly in a comoving volume out to 50 Gpc (z less than or similar to 5).}}, DOI = {{10.1103/PhysRevD.90.064009}}, Article-Number = {{064009}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Van Den Broeck, Chris/R-7871-2018 Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Van Den Broeck, Chris/0000-0001-6800-4006 Veitch, John/0000-0002-6508-0713 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000341265400007}}, } @article{ ISI:000338499100003, Author = {Talukder, Dipongkar and Thrane, Eric and Bose, Sukanta and Regimbau, Tania}, Title = {{Measuring neutron-star ellipticity with measurements of the stochastic gravitational-wave background}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{89}}, Number = {{12}}, Month = {{JUN 20}}, Abstract = {{Galactic neutron stars are a promising source of gravitational waves in the analysis band of detectors such as Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo. Previous searches for gravitational waves from neutron stars have focused on the detection of individual neutron stars, which are either nearby or highly nonspherical. Here, we consider the stochastic gravitational-wave signal arising from the ensemble of Galactic neutron stars. Using a population synthesis model, we estimate the single-sigma sensitivity of current and planned gravitational-wave observatories to average neutron star ellipticity. as a function of the number of in-band Galactic neutron stars N-tot. For the plausible case of N-tot approximate to 53000, and assuming one year of observation time with colocated initial LIGO detectors, we find it to be sigma(is an element of) = 2.1 x 10(-7), which is comparable to current bounds on some nearby neutron stars. (The current best 95\% upper limits are is an element of less than or similar to 7 x 10(-8).) It is unclear if Advanced LIGO can significantly improve on this sensitivity using spatially separated detectors. For the proposed Einstein Telescope, we estimate that sigma(is an element of) = 5.6 x 10(-10). Finally, we show that stochastic measurements can be combined with measurements of individual neutron stars in order to estimate the number of in-band Galactic neutron stars. In this way, measurements of stochastic gravitational waves provide a complementary tool for studying Galactic neutron stars.}}, DOI = {{10.1103/PhysRevD.89.123008}}, Article-Number = {{123008}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Talukder, Dipongkar/0000-0002-9178-8870 Thrane, Eric/0000-0002-4418-3895}}, Unique-ID = {{ISI:000338499100003}}, } @article{ ISI:000336614200012, Author = {Evangelista, Edgard F. D. and de Araujo, Jose C. N.}, Title = {{Stochastic Background of Gravitational Waves Generated by Compact Binary Systems}}, Journal = {{BRAZILIAN JOURNAL OF PHYSICS}}, Year = {{2014}}, Volume = {{44}}, Number = {{2-3}}, Pages = {{260-270}}, Month = {{JUN}}, Abstract = {{Binary systems are the most studied sources of gravitational waves. The mechanisms of emission and the behavior of the orbital parameters are well known and can be written in analytic form in several cases. Besides, the strongest indication of the existence of gravitational waves has arisen from the observation of binary systems. On the other hand, when the detection of gravitational radiation becomes a reality, one of the observed pattern of the signals will be probably of stochastic background nature, which are characterized by a superposition of signals emitted by many sources around the universe. Our aim here is to develop an alternative method of calculating such backgrounds emitted by cosmological compact binary systems during their periodic or quasiperiodic phases. We use an analogy with a problem of statistical mechanics in order to perform this sum as well as taking into account the temporal variation of the orbital parameters of the systems. Such a kind of background is of particular importance since it could well form an important foreground for the planned gravitational wave interferometers DECI-Hertz Interferometer Gravitational wave Observatory (DECIGO), Big Bang Observer (BBO), Laser Interferometer Space Antenna (LISA) or Evolved LISA (eLISA), Advanced Laser Interferometer Gravitational-Wave Observatory (ALIGO), and Einstein Telescope (ET).}}, DOI = {{10.1007/s13538-014-0178-x}}, ISSN = {{0103-9733}}, EISSN = {{1678-4448}}, ResearcherID-Numbers = {{de Araujo, Jose C N/C-5181-2013 Evangelista, Edgard F D/M-2670-2016}}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289 }}, Unique-ID = {{ISI:000336614200012}}, } @article{ ISI:000334335900009, Author = {Regimbau, Tania and Meacher, Duncan and Coughlin, Michael}, Title = {{Second Einstein Telescope mock science challenge: Detection of the gravitational-wave stochastic background from compact binary coalescences}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{89}}, Number = {{8}}, Month = {{APR 9}}, Abstract = {{We present the results of the search for an astrophysical gravitational-wave stochastic background during the second Einstein Telescope mock data and science challenge. Assuming that the loudest sources can be detected individually and removed from the data, we show that the residual background can be recovered with an accuracy of 1\% with the standard cross-correlation statistic, after correction of a systematic bias due to the anisotropy of the sources.}}, DOI = {{10.1103/PhysRevD.89.084046}}, Article-Number = {{084046}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000334335900009}}, } @article{ ISI:000332170900001, Author = {Lackey, Benjamin D. and Kyutoku, Koutarou and Shibata, Masaru and Brady, Patrick R. and Friedman, John L.}, Title = {{Extracting equation of state parameters from black hole-neutron star mergers: Aligned-spin black holes and a preliminary waveform model}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{89}}, Number = {{4}}, Month = {{FEB 21}}, Abstract = {{Information about the neutron-star equation of state is encoded in the waveform of a black hole-neutron star system through tidal interactions and the possible tidal disruption of the neutron star. During the inspiral this information depends on the tidal deformability. of the neutron star, and we find that the best-measured parameter during the merger and ringdown is consistent with. as well. We performed 134 simulations where we systematically varied the equation of state as well as the mass ratio, neutron star mass, and aligned spin of the black hole. Using these simulations we develop an analytic representation of the full inspiral-merger-ringdown waveform calibrated to these numerical waveforms; we use this analytic waveform and a Fisher matrix analysis to estimate the accuracy to which. can be measured with gravitational-wave detectors. We find that although the inspiral tidal signal is small, coherently combining this signal with the merger-ringdown matter effect improves the measurability of. by a factor of similar to 3 over using just the merger-ringdown matter effect alone. However, incorporating correlations between all the waveform parameters then decreases the measurability of. by a factor of similar to 3. The uncertainty in. increases with the mass ratio, but decreases as the black hole spin increases. Overall, a single Advanced LIGO detector can only marginally measure. for mass ratios Q = 2-5, black hole spins J(BH)/M-BH(2) = -0.5-0.75, and neutron star masses M-NS = 1.2M(circle dot)-1.45M(circle dot) at an optimally oriented distance of 100 Mpc. For the proposed Einstein Telescope, however, the uncertainty in. is an order of magnitude smaller.}}, DOI = {{10.1103/PhysRevD.89.043009}}, Article-Number = {{043009}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Brady, Patrick/0000-0002-4611-9387 Kyutoku, Koutarou/0000-0003-3179-5216}}, Unique-ID = {{ISI:000332170900001}}, } @article{ ISI:000332170600001, Author = {Yagi, Kent}, Title = {{Multipole Love relations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2014}}, Volume = {{89}}, Number = {{4}}, Month = {{FEB 20}}, Abstract = {{Gravitational-wave observations in the near future may allow us to measure tidal deformabilities of neutron stars, which leads us to the understanding of physics at nuclear density. In principle, the gravitational waveform depends on various tidal parameters, which correlate strongly. Therefore, it would be useful if one can express such tidal parameters with a single parameter. Here, we report on universal relations among various lth (dimensionless) electric, magnetic, and shape tidal deformabilities in neutron stars and quark stars that do not depend sensitively on the equation of state. Such relations allow us to break the degeneracy among the tidal parameters. In this paper, we focus on gravitational waves from nonspinning neutron-star binary inspirals. We first derive the leading contribution of the lth electric and l = 2 magnetic tidal deformabilities to the gravitational-wave phase, which enters at 2l + 1 and 6 post-Newtonian orders relative to the leading Newtonian one, respectively. We then calculate the useful number of gravitational-wave cycles and show that not only the l = 2 but also l = 3 electric tidal deformabilities are important for parameter estimation with third-generation gravitational-wave detectors such as LIGO III and Einstein Telescope. Although the correlation between the l = 2 and l = 3 electric tidal deformabilities deteriorate the measurement accuracy of the former deformability parameter, one can increase its measurement accuracy significantly by using the universal relation. We provide a fitting formula for the LIGO III noise curve in the appendixes.}}, DOI = {{10.1103/PhysRevD.89.043011}}, Article-Number = {{043011}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000332170600001}}, } @inproceedings{ ISI:000346122600051, Author = {Kroker, Stefanie and Nawrodt, Ronny and ET Sci Team}, Book-Group-Author = {{IEEE}}, Title = {{The Einstein Telescope}}, Booktitle = {{2014 IEEE INTERNATIONAL WORKSHOP ON METROLOGY FOR AEROSPACE (METROAEROSPACE)}}, Year = {{2014}}, Pages = {{288-292}}, Note = {{IEEE International Workshop on Metrology for Aerospace (MetroAeroSpace), Benevento, ITALY, MAY 29-30, 2014}}, Organization = {{IEEE; IEEE Instrumentat \& Measurement Soc; AESS}}, Abstract = {{Interferometric gravitational wave detectors are amongst the most sensitive instruments ever built. They are hunting for tiny oscillations in space-time originating from cosmic events such as inspiraling objects or supernova explosions. These detectors are based on Michelson-like interferometers reaching sensitivities for lengths changes of better than 10(-18) m/root Hz. Currently, a second generation of gravitational wave detectors is under construction reducing relevant noise sources throughout their detection band by one order of magnitude. First steps towards a third generation detector - having two orders of magnitude larger sensitivity compared to the first generation - have been made. This gravitational wave observatory - the Einstein Telescope - is a European-wide effort leading to a sophisticated design including an optimum site selection. We present the status of these activities and give an overview of the state of the art technologies needed to realize such an instrument.}}, ISBN = {{978-1-4799-2069-3}}, ResearcherID-Numbers = {{Kroker, Stefanie/V-3419-2017}}, ORCID-Numbers = {{Kroker, Stefanie/0000-0002-7584-7359}}, Unique-ID = {{ISI:000346122600051}}, } @inproceedings{ ISI:000346122600095, Author = {Kroker, Stefanie and Kley, Ernst-Bernhard}, Book-Group-Author = {{IEEE}}, Title = {{Thermal noise of silicon based grating reflectors for high-precision metrology}}, Booktitle = {{2014 IEEE INTERNATIONAL WORKSHOP ON METROLOGY FOR AEROSPACE (METROAEROSPACE)}}, Year = {{2014}}, Pages = {{523-527}}, Note = {{IEEE International Workshop on Metrology for Aerospace (MetroAeroSpace), Benevento, ITALY, MAY 29-30, 2014}}, Organization = {{IEEE; IEEE Instrumentat \& Measurement Soc; AESS}}, Abstract = {{The sensitivity of many experiments in the field of high-precision optical metrology is severely limited by coating thermal noise of the optical components, for example cavity mirrors. These components are commonly based on alternating layer pairs of amorphous materials. Particularly, for cryogenic applications highly reflective silicon gratings can be a promising low-noise alternative to these layer stacks. In this contribution we present a method to evaluate thermal noise of such micro-structured surfaces. For the example of the Einstein Telescope low-frequency detector it is found that coating thermal noise can be reduced up to one order of magnitude by using monolithic silicon gratings instead of conventional multilayer mirrors.}}, ISBN = {{978-1-4799-2069-3}}, ResearcherID-Numbers = {{Kroker, Stefanie/Q-8871-2016 Kroker, Stefanie/V-3419-2017}}, ORCID-Numbers = {{Kroker, Stefanie/0000-0002-7584-7359 Kroker, Stefanie/0000-0002-7584-7359}}, Unique-ID = {{ISI:000346122600095}}, } @inproceedings{ ISI:000335317500010, Author = {Van den Broeck, C.}, Editor = {{Sathyaprakash, BS and Singh, TP}}, Title = {{Astrophysics, cosmology, and fundamental physics with compact binary coalescence and the Einstein Telescope}}, Booktitle = {{VISHWA MIMANSA: AN INTERPRETATIVE EXPOSITION OF THE UNIVERSE. PROCEEDINGS OF THE 7TH INTERNATIONAL CONFERENCE ON GRAVITATION AND COSMOLOGY}}, Series = {{Journal of Physics Conference Series}}, Year = {{2014}}, Volume = {{484}}, Note = {{7th International Conference on Gravitation and Cosmology (ICGC), INDIA, DEC 14-19, 2011}}, Organization = {{Inter Univ Ctr Astronomy \& Astrophys; Assoc Friends Astronomy; SINP, Ctr AstroParticle Phys; Dept Sci, Technol \& Environm; Foundat Quest Inst; Harish Chandra Res Inst; Infosys Sci Fdn; Inst Math Sci; TATA Inst Fundamental Res, Int Ctr Theoret Sci; Indian Assoc Gen Relat \& Gravitat}}, Abstract = {{The second-generation interferometric gravitational wave detectors, currently under construction are expected to make their first detections within this decade. This will firmly establish gravitational wave physics as an empirical science, and will open up a new era in astrophysics, cosmology, and fundamental physics. Already with the first detections, we will be able to, among other things, establish the nature of short-hard gamma ray bursts, definitively confirm the existence of black holes, measure the Hubble constant in a completely independent way, and for the first time gain access to the genuinely strong-field dynamics of gravity. Hence, it is time to consider the longer-term future of this new field. The Einstein Telescope ( ET) is a concrete conceptual proposal for a third-generation gravitational wave observatory, which will be similar to 10 times more sensitive in strain than the second-generation detectors. This will give access to sources at cosmological distances, with a correspondingly higher detection rate. We have given an overview of the science case for ET, with a focus on what can be learned from signals emitted by coalescing compact binaries. Third-generation observatories will allow us to map the coalescence rate out to redshifts z similar to 3, determine the mass functions of neutron stars and black holes, and perform precision measurements of the neutron star equation of state. ET will enable us to study the large-scale structure and evolution of the Universe without recourse to a cosmic distance ladder. Finally, we have discussed how it will allow for high-precision measurements of strong-field, dynamical gravity.}}, DOI = {{10.1088/1742-6596/484/1/012008}}, Article-Number = {{012008}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, Unique-ID = {{ISI:000335317500010}}, } @article{ ISI:000328260900004, Author = {Cerda-Duran, Pablo and DeBrye, Nicolas and Aloy, Miguel A. and Font, Jose A. and Obergaulinger, Martin}, Title = {{GRAVITATIONAL WAVE SIGNATURES IN BLACK HOLE FORMING CORE COLLAPSE}}, Journal = {{ASTROPHYSICAL JOURNAL LETTERS}}, Year = {{2013}}, Volume = {{779}}, Number = {{2}}, Month = {{DEC 20}}, Abstract = {{We present general relativistic numerical simulations of collapsing stellar cores. Our initial model consists of a low metallicity rapidly-rotating progenitor which is evolved in axisymmetry with the latest version of our general relativistic code CoCoNuT, which allows for black hole formation and includes the effects of a microphysical equation of state (LS220) and a neutrino leakage scheme to account for radiative losses. The motivation of our study is to analyze in detail the emission of gravitational waves in the collapsar scenario of long gamma-ray bursts. Our simulations show that the phase during which the proto-neutron star (PNS) survives before ultimately collapsing to a black hole is particularly optimal for gravitational wave emission. The high-amplitude waves last for several seconds and show a remarkable quasi-periodicity associated with the violent PNS dynamics, namely during the episodes of convection and the subsequent nonlinear development of the standing-accretion shock instability (SASI). By analyzing the spectrogram of our simulations we are able to identify the frequencies associated with the presence of g-modes and with the SASI motions at the PNS surface. We note that the gravitational waves emitted reach large enough amplitudes to be detected with third-generation detectors such as the Einstein Telescope within a Virgo Cluster volume at rates less than or similar to 0.1 yr(-1).}}, DOI = {{10.1088/2041-8205/779/2/L18}}, Article-Number = {{L18}}, ISSN = {{2041-8205}}, EISSN = {{2041-8213}}, ResearcherID-Numbers = {{Font, Jose/K-5198-2014 Cerda-Duran, Pablo/D-7857-2015 Aloy, Miguel-Angel/K-9941-2014}}, ORCID-Numbers = {{Font, Jose/0000-0001-6650-2634 Cerda-Duran, Pablo/0000-0003-4293-340X Aloy, Miguel-Angel/0000-0002-5552-7681}}, Unique-ID = {{ISI:000328260900004}}, } @article{ ISI:000327877400003, Author = {Evangelista, Edgard F. D. and De Araujo, Jose C. N.}, Title = {{A NEW METHOD TO CALCULATE THE STOCHASTIC BACKGROUND OF GRAVITATIONAL WAVES GENERATED BY COMPACT BINARIES}}, Journal = {{MODERN PHYSICS LETTERS A}}, Year = {{2013}}, Volume = {{28}}, Number = {{38}}, Month = {{DEC 14}}, Abstract = {{In the study of gravitational waves (GWs), the stochastic background generated by compact binary systems are among the most important kinds of signals. The reason for such an importance has to do with their probable detection by the interferometric detectors {[}such as the Advanced LEGO (ALIGO) and Einstein `Telescope (ET)] in the near future. In this paper we are concerned with, in particular, the stochastic background of GWs generated by double neutron star (DNS) systems in circular orbits during their periodic and quasi-periodic phases. Our aim here is to describe a new method to calculate such spectra, which is based on an analogy with a problem of Statistical Mechanics. Besides, an important characteristic of our method is to consider the time evolution of the orbital parameters.}}, DOI = {{10.1142/S0217732313501745}}, Article-Number = {{1350174}}, ISSN = {{0217-7323}}, EISSN = {{1793-6632}}, ResearcherID-Numbers = {{Evangelista, Edgard F D/M-2670-2016 de Araujo, Jose C N/C-5181-2013}}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289}}, Unique-ID = {{ISI:000327877400003}}, } @article{ ISI:000328602900008, Author = {Lin, Lap-Ming}, Title = {{Torsional oscillations of crystalline color-superconducting hybrid stars: Possible sources for Advanced LIGO?}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{88}}, Number = {{12}}, Month = {{DEC 3}}, Abstract = {{Deconfined quark matter may exist in a crystalline color-superconducting phase in the interiors of compact stars. In this paper, we study the torsional oscillations of compact stars featuring a crystalline color-superconducting quark-matter core in general relativity. Depending on the size of the crystalline core and the value of the gap parameter Delta, we find that the frequencies of the torsional oscillation modes can range from a few hundred hertz to a few kilohertz for our canonical 1.4M(circle dot) compact star models. We have also studied the prospect for detecting the gravitational-wave signals emitted from these modes in a pulsar glitch event. Assuming that at least 10\% of the energy released in a Vela glitch can be channeled to the oscillation modes, we find that the Einstein Telescope should be able to detect these signals in quite general situations. Furthermore, if the size of the crystalline core is comparable to the stellar radius and the gap parameter is relatively small at Delta similar to 5 MeV, the signal-to-noise ratio for Advanced LIGO could reach similar to 10 for a Vela glitch. Our optimistic results suggest that we might already be able to probe the nature of crystalline color-superconducting quark matter with the second-generation gravitational-wave detectors when they come online in the next few years.}}, DOI = {{10.1103/PhysRevD.88.124002}}, Article-Number = {{124002}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000328602900008}}, } @article{ ISI:000327387900010, Author = {Maselli, Andrea and Gualtieri, Leonardo and Ferrari, Valeria}, Title = {{Constraining the equation of state of nuclear matter with gravitational wave observations: Tidal deformability and tidal disruption}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{88}}, Number = {{10}}, Month = {{NOV 26}}, Abstract = {{We study how to extract information on the neutron star equation of state from the gravitational wave signal emitted during the coalescence of a binary system composed of two neutron stars or a neutron star and a black hole. We use post-Newtonian templates which include the tidal deformability parameter and, when tidal disruption occurs before merger, a frequency cutoff. Assuming that this signal is detected by Advanced LIGO/Virgo or the Einstein Telescope, we evaluate the uncertainties on these parameters using different data-analysis strategies based on the Fisher matrix approach and on recently obtained analytical fits of the relevant quantities. We find that the tidal deformability is more effective than the stellar compactness to discriminate among different possible equations of state.}}, DOI = {{10.1103/PhysRevD.88.104040}}, Article-Number = {{104040}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Gualtieri, Leonardo/F-2612-2012 }}, ORCID-Numbers = {{Gualtieri, Leonardo/0000-0002-1097-3266 Maselli, Andrea/0000-0001-8515-8525}}, Unique-ID = {{ISI:000327387900010}}, } @article{ ISI:000326979500022, Author = {Piorkowska, Aleksandra and Biesiada, Marek and Zhu, Zong-Hong}, Title = {{Strong gravitational lensing of gravitational waves in Einstein Telescope}}, Journal = {{JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS}}, Year = {{2013}}, Number = {{10}}, Month = {{OCT}}, Abstract = {{Gravitational wave experiments have entered a new stage which gets us closer to the opening a new observational window on the Universe. In particular, the Einstein Telescope (ET) is designed to have a fantastic sensitivity that will provide with tens or hundreds of thousand NS-NS inspiral events per year up to the redshift z = 2. Some of such events should be gravitationally lensed by intervening galaxies. We explore the prospects of observing gravitationally lensed inspiral NS-NS events in the Einstein telescope. Being conservative we consider the lens population of elliptical galaxies. It turns out that depending on the local insipral rate ET should detect from one per decade detection in the pessimistic case to a tens of detections per year for the most optimistic case. The detection of gravitationally lensed source in gravitational wave detectors would be an invaluable source of information concerning cosmography, complementary to standard ones (like supernovae or BAO) independent of the local cosmic distance ladder calibrations.}}, DOI = {{10.1088/1475-7516/2013/10/022}}, Article-Number = {{022}}, ISSN = {{1475-7516}}, ResearcherID-Numbers = {{Biesiada, Marek/ABC-3364-2020}}, ORCID-Numbers = {{Biesiada, Marek/0000-0003-1308-7304}}, Unique-ID = {{ISI:000326979500022}}, } @article{ ISI:000324233700006, Author = {Foucart, Francois and Buchman, Luisa and Duez, Matthew D. and Grudich, Michael and Kidder, Lawrence E. and MacDonald, Ilana and Mroue, Abdul and Pfeiffer, Harald P. and Scheel, Mark A. and Szilagyi, Bela}, Title = {{First direct comparison of nondisrupting neutron star-black hole and binary black hole merger simulations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{88}}, Number = {{6}}, Month = {{SEP 9}}, Abstract = {{We present the first direct comparison of numerical simulations of neutron star-black hole and black hole-black hole mergers in full general relativity. We focus on a configuration with nonspinning objects and within the most likely range of mass ratio for neutron star-black hole systems (q = 6). In this region of the parameter space, the neutron star is not tidally disrupted prior to merger, and we show that the two types of mergers appear remarkably similar. The effect of the presence of a neutron star on the gravitational wave signal is not only undetectable by the next generation of gravitational wave detectors, but also too small to be measured in the numerical simulations: even the plunge, merger and ringdown signals appear in perfect agreement for both types of binaries. The characteristics of the post-merger remnants are equally similar, with the masses of the final black holes agreeing within delta M-BH < 5 X 10(-4) M-BH and their dimensionless spins within delta chi(BH) < 10(-3). The rate of periastron advance in the mixed binary agrees with previously published binary black hole results, and we use the inspiral waveforms to place constraints on the accuracy of our numerical simulations independent of algorithmic choices made for each type of binary. Overall, our results indicate that nondisrupting neutron star-black hole mergers are exceptionally well modeled by black hole-black hole mergers, and that given the absence of mass ejection, accretion disk formation, or differences in the gravitational wave signals, only electromagnetic precursors could prove the presence of a neutron star in low-spin systems of total mass similar to 10M(circle dot), at least until the advent of gravitational wave detectors with a sensitivity comparable to that of the proposed Einstein Telescope.}}, DOI = {{10.1103/PhysRevD.88.064017}}, Article-Number = {{064017}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Buchman, Luisa/AAC-8251-2019 }}, ORCID-Numbers = {{Pfeiffer, Harald/0000-0001-9288-519X Foucart, Francois/0000-0003-4617-4738}}, Unique-ID = {{ISI:000324233700006}}, } @article{ ISI:000318972600009, Author = {Nawrodt, R. and Schwarz, C. and Kroker, S. and Martin, I. W. and Bassiri, R. and Brueckner, F. and Cunningham, L. and Hammond, G. D. and Heinert, D. and Hough, J. and Kaesebier, T. and Kley, E-B and Neubert, R. and Reid, S. and Rowan, S. and Seidel, P. and Tuennermann, A.}, Title = {{Investigation of mechanical losses of thin silicon flexures at low temperatures}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2013}}, Volume = {{30}}, Number = {{11}}, Month = {{JUN 7}}, Abstract = {{Studies of the mechanical loss of silicon flexures in a temperature region from 5 to 300 K are presented, where the flexures have been prepared by different fabrication techniques of interest for the construction of suspension elements of future interferometric gravitational wave detectors. A lowest mechanical loss of 3 x 10(-8) was observed for a 130 mu m thick flexure at around 10 K. While the mechanical loss follows the thermo-elastic predictions down to 50 K, at lower temperatures the observed loss is found to be a function of surface roughness. This surface loss is of interest for all applications using silicon-based oscillators at low temperatures. The extraction of a surface loss parameter using results from our measurements and those of other authors is presented and the relevance for future gravitational wave detector suspensions is discussed. A surface loss parameter alpha(s) = 0.5 pm was obtained. This reveals that the surface loss of silicon is significantly lower than the surface loss of fused silica.}}, DOI = {{10.1088/0264-9381/30/11/115008}}, Article-Number = {{115008}}, ISSN = {{0264-9381}}, ResearcherID-Numbers = {{Kroker, Stefanie/V-3419-2017 Martin, Iain/V-1198-2018 Tunnermann, Andreas/K-6453-2016 Kroker, Stefanie/Q-8871-2016 Martin, Iain/A-2445-2010 }}, ORCID-Numbers = {{Kroker, Stefanie/0000-0002-7584-7359 Martin, Iain/0000-0001-7300-9151 Kroker, Stefanie/0000-0002-7584-7359 Bassiri, Riccardo/0000-0001-8171-6833 Hammond, Giles/0000-0002-1414-3622}}, Unique-ID = {{ISI:000318972600009}}, } @article{ ISI:000319284300001, Author = {Gerosa, Davide and Kesden, Michael and Berti, Emanuele and O'Shaughnessy, Richard and Sperhake, Ulrich}, Title = {{Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{87}}, Number = {{10}}, Month = {{MAY 22}}, Abstract = {{We study the influence of astrophysical formation scenarios on the precessional dynamics of spinning black-hole binaries by the time they enter the observational window of second- and third-generation gravitational-wave detectors, such as Advanced LIGO/Virgo, LIGO-India, KAGRA, and the Einstein Telescope. Under the plausible assumption that tidal interactions are efficient at aligning the spins of few-solar mass black-hole progenitors with the orbital angular momentum, we find that black-hole spins should be expected to preferentially lie in a plane when they become detectable by gravitational-wave interferometers. This ``resonant plane{''} is identified by the conditions Delta Phi = 0 degrees or Delta Phi = +/- 180 degrees, where Delta Phi is the angle between the components of the black-hole spins in the plane orthogonal to the orbital angular momentum. If the angles Delta Phi can be accurately measured for a large sample of gravitational-wave detections, their distribution will constrain models of compact binary formation. In particular, it will tell us whether tidal interactions are efficient and whether a mechanism such as mass transfer, stellar winds, or supernovae can induce a mass-ratio reversal (so that the heavier black hole is produced by the initially lighter stellar progenitor). Therefore, our model offers a concrete observational link between gravitational-wave measurements and astrophysics. We also hope that it will stimulate further studies of precessional dynamics, gravitational-wave template placement, and parameter estimation for binaries locked in the resonant plane.}}, DOI = {{10.1103/PhysRevD.87.104028}}, Article-Number = {{104028}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{O'Shaughnessy, Richard/AAA-3625-2021 Berti, Emanuele/C-9331-2016 Berti, Emanuele/AAI-1513-2019 Gerosa, Davide/K-4625-2017 }}, ORCID-Numbers = {{O'Shaughnessy, Richard/0000-0001-5832-8517 Berti, Emanuele/0000-0003-0751-5130 Gerosa, Davide/0000-0002-0933-3579 Kesden, Michael/0000-0002-5987-1471}}, Unique-ID = {{ISI:000319284300001}}, } @article{ ISI:000319059500006, Author = {Wang, Mengyao and Bond, Charlotte and Brown, Daniel and Brueckner, Frank and Carbone, Ludovico and Palmer, Rebecca and Freise, Andreas}, Title = {{Realistic polarizing Sagnac topology with DC readout for the Einstein Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{87}}, Number = {{9}}, Month = {{MAY 14}}, Abstract = {{The Einstein Telescope (ET) is a proposed future gravitational wave detector. Its design is original, using a triangular orientation of three detectors and a xylophone configuration, splitting each detector into one high-frequency and one low-frequency system. In other aspects the current design retains the dual-recycled Michelson interferometer typical of current detectors, such as Advanced LIGO. In this paper, we investigate the feasibility of replacing the low-frequency part of the ET detectors with a Sagnac interferometer. We show that a Sagnac interferometer, using realistic optical parameters based on the ET design, could provide a similar level of radiation pressure noise suppression without the need for a signal recycling mirror and the extensive filter cavities. We consider the practical issues of a realistic, power-recycled Sagnac, using linear arm cavities and polarizing optics. In particular, we investigate the effects of nonperfect polarizing optics and propose a new method for the generation of a local oscillator field similar to the DC readout scheme of current detectors.}}, DOI = {{10.1103/PhysRevD.87.096008}}, Article-Number = {{096008}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Brown, Daniel/0000-0001-7851-3939 Freise, Andreas/0000-0001-6586-9901}}, Unique-ID = {{ISI:000319059500006}}, } @article{ ISI:000318343600090, Author = {Zhu, Xing-Jiang and Howell, Eric J. and Blair, David G. and Zhu, Zong-Hong}, Title = {{On the gravitational wave background from compact binary coalescences in the band of ground-based interferometers}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2013}}, Volume = {{431}}, Number = {{1}}, Pages = {{882-899}}, Month = {{MAY}}, Abstract = {{This paper reports a comprehensive study on the gravitational wave (GW) background from compact binary coalescences. We consider in our calculations newly available observation-based neutron star and black hole mass distributions and complete analytical waveforms that include post-Newtonian amplitude corrections. Our results show that: (i) post-Newtonian effects cause a small reduction in the GW background signal; (ii) below 100 Hz the background depends primarily on the local coalescence rate r(0) and the average chirp mass and is independent of the chirp mass distribution; (iii) the effects of cosmic star formation rates and delay times between the formation and merger of binaries are linear below 100 Hz and can be represented by a single parameter within a factor of similar to 2; (iv) a simple power-law model of the energy density parameter Omega(GW)(f) similar to f(2/3) up to 50-100 Hz is sufficient to be used as a search template for ground-based interferometers. In terms of detection prospects of this background signal, we show that: (i) detection (a signal-to-noise ratio of 3) within one year of observation by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors (H1-L1) requires a coalescence rate of r(0) = 3 (0.2) Mpc(-3) Myr(-1) for binary neutron stars (binary black holes); (ii) this limit on r(0) could be reduced threefold for two co-located and co-aligned detectors, whereas the currently proposed worldwide network of advanced instruments gives only similar to 30 per cent improvement in detectability; (iii) the improved sensitivity of the planned Einstein Telescope allows not only confident detection of the background but also the high-frequency components of the spectrum to be measured, possibly enabling rate evolutionary histories and mass distributions to be probed. Finally, we show that sub-threshold binary neutron star merger events produce a strong foreground, which could be an issue for future terrestrial stochastic searches of primordial GWs.}}, DOI = {{10.1093/mnras/stt207}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Zhu, Xingjiang/E-1501-2016 Howell, Eric/H-5072-2014 }}, ORCID-Numbers = {{Zhu, Xingjiang/0000-0001-7049-6468 Howell, Eric/0000-0001-7891-2817 Ju, Li/0000-0002-7951-4295 Blair, David/0000-0002-1501-2405}}, Unique-ID = {{ISI:000318343600090}}, } @article{ ISI:000317191400005, Author = {Camera, Stefano and Nishizawa, Atsushi}, Title = {{Beyond Concordance Cosmology with Magnification of Gravitational-Wave Standard Sirens}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2013}}, Volume = {{110}}, Number = {{15}}, Month = {{APR 8}}, Abstract = {{We show how future gravitational-wave detectors would be able to discriminate between the concordance Lambda cold dark matter cosmological model and up-to-date competing alternatives, e. g., dynamical dark energy (DE) models or modified gravity (MG) theories. Our method consists of using the weak-lensing magnification effect that affects a standard-siren signal because of its traveling through the Universe's large scale structure. As a demonstration, we present constraints on DE and MG from proposed gravitational-wave detectors, namely Einstein Telescope and DECI-Hertz Interferometer Gravitational-Wave Observatory and Big-Bang Observer. DOI: 10.1103/PhysRevLett.110.151103}}, DOI = {{10.1103/PhysRevLett.110.151103}}, Article-Number = {{151103}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Camera, Stefano/AAG-7753-2020 Camera, Stefano/N-2456-2013 }}, ORCID-Numbers = {{Camera, Stefano/0000-0003-3399-3574 Camera, Stefano/0000-0003-3399-3574 Nishizawa, Atsushi/0000-0003-3562-0990}}, Unique-ID = {{ISI:000317191400005}}, } @article{ ISI:000316227500025, Author = {Sathyaprakash, B. and Mantovani, M.}, Title = {{Scientific objectives of Einstein telescope (vol 29, 124013, 2012)}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2013}}, Volume = {{30}}, Number = {{7}}, Month = {{APR 7}}, DOI = {{10.1088/0264-9381/30/7/079501}}, Article-Number = {{079501}}, ISSN = {{0264-9381}}, ResearcherID-Numbers = {{Kokkotas, Kostas D/B-7878-2010 Schnabel, Roman/V-7759-2019 Sopuerta, Carlos F./L-3835-2014 Seoane, Pau Amaro/U-8229-2017 Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Kokkotas, Kostas D/0000-0001-6048-2919 Sopuerta, Carlos F./0000-0002-1779-4447 Del Pozzo, Walter/0000-0003-3978-2030 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000316227500025}}, } @article{ ISI:000317623300003, Author = {Punturo, Michele and Somiya, Kentaro}, Title = {{UNDERGROUND GRAVITATIONAL WAVE OBSERVATORIES: KAGRA AND ET}}, Journal = {{INTERNATIONAL JOURNAL OF MODERN PHYSICS D}}, Year = {{2013}}, Volume = {{22}}, Number = {{5}}, Month = {{APR}}, Abstract = {{Future gravitational wave observatories will be realized underground in order to reduce external disturbances, such as seismic, Newtonian and environmental noises. The Japanese gravitational wave telescope KAGRA is under construction at the Kamioka site and the Einstein Telescope gravitational wave observatory is under study in Europe; the common aspects, the differences and the expected performances of these innovative machines are investigated.}}, DOI = {{10.1142/S0218271813300103}}, Article-Number = {{1330010}}, ISSN = {{0218-2718}}, EISSN = {{1793-6594}}, ResearcherID-Numbers = {{Punturo, Michele/I-3995-2012 Somiya, Kentaro/ABE-2215-2020}}, ORCID-Numbers = {{Punturo, Michele/0000-0001-8722-4485 Somiya, Kentaro/0000-0003-2601-2264}}, Unique-ID = {{ISI:000317623300003}}, } @article{ ISI:000315739200001, Author = {Lasky, Paul D. and Bennett, Mark F. and Melatos, Andrew}, Title = {{Stochastic gravitational wave background from hydrodynamic turbulence in differentially rotating neutron stars}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2013}}, Volume = {{87}}, Number = {{6}}, Month = {{MAR 7}}, Abstract = {{Hydrodynamic turbulence driven by crust-core differential rotation imposes a fundamental noise floor on gravitational wave observations of neutron stars. The gravitational wave emission peaks at the Kolmogorov decoherence frequency which, for reasonable values of the crust-core shear, Delta Omega, occurs near the most sensitive part of the frequency band for ground-based, long-baseline interferometers. We calculate the energy density spectrum of the stochastic gravitational wave background from a cosmological population of turbulent neutron stars generalizing previous calculations for individual sources. The spectrum resembles a piecewise power law, Omega(gw)(v) = Omega(alpha)v(alpha), with alpha = -1 and 7 above and below the decoherence frequency respectively, and its normalization scales as Omega(alpha) proportional to (Delta Omega)(7). Nondetection of a stochastic signal by Initial LIGO implies an upper limit on Delta Omega and hence by implication on the internal relaxation time scale for the crust and core to come into corotation, tau(d) = Delta Omega/(Omega) over dot, where (Omega) over dot is the observed electromagnetic spin-down rate, with tau(d) less than or similar to 10(7) yr for accreting millisecond pulsars and tau(d) less than or similar to 10(5) yr for radio-loud pulsars. Target limits on tau(d) are also estimated for future detectors, namely Advanced LIGO and the Einstein Telescope, and are found to be astrophysically interesting. DOI: 10.1103/PhysRevD.87.063004}}, DOI = {{10.1103/PhysRevD.87.063004}}, Article-Number = {{063004}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Lasky, Paul/0000-0003-3763-1386 Melatos, Andrew/0000-0003-4642-141X Bennett, Mark/0000-0002-3561-6804}}, Unique-ID = {{ISI:000315739200001}}, } @inproceedings{ ISI:000327218800011, Author = {Passamonti, A. and Gaertig, E. and Kokkotas, K. D.}, Book-Group-Author = {{IOP}}, Title = {{The evolution of the f-mode instability and gravitational wave detection prospectives}}, Booktitle = {{NEB 15 - RECENT DEVELOPMENTS IN GRAVITY}}, Series = {{Journal of Physics Conference Series}}, Year = {{2013}}, Volume = {{453}}, Note = {{Conference on Recent Developments in Gravity, NEB15, Technol Inst Crete, Chania, GREECE, JUN 20-23, 2012}}, Abstract = {{We study the dynamical evolution of the gravitational-wave driven instability of the f-mode in rapidly rotating relativistic stars with a polytropic equation of state. We use linear perturbation theory to describe the evolution of the mode amplitude and follow the trajectory of a newborn neutron star through its instability window. An unstable f-mode with a saturation energy of about 10(-6) M(circle dot)c(2) may generate a gravitational-wave signal which can be detected by the Einstein Telescope detector from the Virgo cluster. The effects of the magnetic field on the evolution and the detectability of the gravitational radiation are relevant when its strength is higher than 10(12) G, while an unstable r-mode becomes dominant it reaches the maximum saturation value allowed by non-linear mode couplings. From the thermal evolution we find also that the heat generated by shear viscosity during the saturation phase completely balances the neutrinos' cooling and prevents the star from entering the regime of mutual friction. The evolution time of the instability is therefore longer and the star loses significantly larger amounts of angular momentum via gravitational waves.}}, DOI = {{10.1088/1742-6596/453/1/012011}}, Article-Number = {{012011}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, ResearcherID-Numbers = {{Passamonti, Andrea/H-7644-2015 Kokkotas, Kostas D/B-7878-2010 }}, ORCID-Numbers = {{Passamonti, Andrea/0000-0002-7457-4926 Kokkotas, Kostas D/0000-0001-6048-2919 Gaertig, Erich/0000-0003-1728-6466}}, Unique-ID = {{ISI:000327218800011}}, } @article{ ISI:000311808400003, Author = {Regimbau, Tania and Dent, Thomas and Del Pozzo, Walter and Giampanis, Stefanos and Li, Tjonnie G. F. and Robinson, Craig and Van den Broeck, Chris and Meacher, Duncan and Rodriguez, Carl and Sathyaprakash, B. S. and Wojcik, Katarzyna}, Title = {{Mock data challenge for the Einstein Gravitational-Wave Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{86}}, Number = {{12}}, Month = {{DEC 3}}, Abstract = {{The Einstein Telescope (ET) is conceived to be a third generation gravitational-wave (GW) observatory. Its amplitude sensitivity would be a factor 10 better than advanced LIGO and Virgo and it could also extend the low-frequency sensitivity down to 1-3 Hz, compared to the 10-20 Hz of advanced detectors. Such an observatory will have the potential to observe a variety of different GW sources, including compact binary systems at cosmological distances. ET's expected reach for binary neutron star (BNS) coalescences is out to redshift z similar or equal to 2 and the rate of detectable BNS coalescences could be as high as one every few tens or hundreds of seconds, each lasting up to several days. With such a signal-rich environment, a key question in data analysis is whether overlapping signals can be discriminated. In this paper we simulate the GW signals from a cosmological population of BNS and ask the following questions: Does this population create a confusion background that limits ET's ability to detect foreground sources? How efficient are current algorithms in discriminating overlapping BNS signals? Is it possible to discern the presence of a population of signals in the data by cross correlating data from different detectors in the ET observatory? We find that algorithms currently used to analyze LIGO and Virgo data are already powerful enough to detect the sources expected in ET, but new algorithms are required to fully exploit ET data.}}, DOI = {{10.1103/PhysRevD.86.122001}}, Article-Number = {{122001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Van Den Broeck, Chris/R-7871-2018 Dent, Thomas/AAB-3674-2019 Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Van Den Broeck, Chris/0000-0001-6800-4006 Del Pozzo, Walter/0000-0003-3978-2030 Li, Tjonnie Guang Feng/0000-0003-4297-7365 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000311808400003}}, } @article{ ISI:000311279300007, Author = {Tapai, Marton and Keresztes, Zoltan and Gergely, Laszlo Arpad}, Title = {{Spin-dominated waveforms for unequal mass compact binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{86}}, Number = {{10}}, Month = {{NOV 19}}, Abstract = {{We derive spin-dominated waveforms (SDW) for binary systems composed of spinning black holes with unequal masses (less than 1: 30). Such systems could be formed by an astrophysical black hole with a smaller black hole or a neutron star companion; and typically arise for supermassive black hole encounters. SDW characterize the last stages of the inspiral, when the larger spin dominates over the orbital angular momentum (while the spin of the smaller companion can be neglected). They emerge as a double expansion in the post-Newtonian parameter epsilon and the ratio xi of the orbital angular momentum and dominant spin. The SDW amplitudes are presented to (epsilon(3/2), xi) orders, while the phase of the gravitational waves to (epsilon(2), xi) orders (omitting the highest order mixed terms). To this accuracy the amplitude includes the (leading order) spin-orbit contributions, while the phase the (leading order) spin-orbit, self-spin and mass quadrupole-monopole contributions. While the SDW hold for any mass ratio smaller than 1: 30, lower bounds for the mass ratios are derived from the best sensitivity frequency range expected for Advanced LIGO (giving 1: 140), the Einstein Telescope (7 x 10(-4)), the LAGRANGE (7 x 10(-7)) and LISA missions (7 x 10(-9)), respectively.}}, DOI = {{10.1103/PhysRevD.86.104045}}, Article-Number = {{104045}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Tapai, Marton/X-8850-2018 Keresztes, Zoltan/T-4900-2019 Gergely, Laszlo Arpad/X-7693-2018 Keresztes, Zoltan/X-8914-2018}}, ORCID-Numbers = {{Tapai, Marton/0000-0002-5354-5683 Gergely, Laszlo Arpad/0000-0003-3146-6201 Keresztes, Zoltan/0000-0002-2258-5981}}, Unique-ID = {{ISI:000311279300007}}, } @article{ ISI:000311143200006, Author = {Bernuzzi, Sebastiano and Nagar, Alessandro and Zenginoglu, Anil}, Title = {{Horizon-absorption effects in coalescing black-hole binaries: An effective-one-body study of the nonspinning case}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{86}}, Number = {{10}}, Month = {{NOV 15}}, Abstract = {{We study the horizon absorption of gravitational waves in coalescing, circularized, nonspinning black-hole binaries. The horizon-absorbed fluxes of a binary with a large mass ratio (q = 1000) obtained by numerical perturbative simulations are compared with an analytical, effective-one-body (EOB) resummed expression recently proposed. The perturbative method employs an analytical, linear in the mass ratio, EOB-resummed radiation reaction, and the Regge-Wheeler-Zerilli formalism for wave extraction. Hyperboloidal layers are employed for the numerical solution of the Regge-Wheeler-Zerilli equations to accurately compute horizon fluxes up to the late plunge phase. The horizon fluxes from perturbative simulations and the EOB-resummed expression agree at the level of a few percent down to the late plunge. An upgrade of the EOB model for nonspinning binaries that includes horizon absorption of angular momentum as an additional term in the resummed radiation reaction is then discussed. The effect of this term on the waveform phasing for binaries with mass ratios spanning 1-1000 is investigated. We confirm that for comparable and intermediate-mass-ratio binaries horizon absorption is practically negligible for detection with advanced LIGO and the Einstein Telescope (faithfulness >= 0.997).}}, DOI = {{10.1103/PhysRevD.86.104038}}, Article-Number = {{104038}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Zenginoglu, Anil/AAE-3968-2019 }}, ORCID-Numbers = {{Zenginoglu, Anil/0000-0001-7896-6268}}, Unique-ID = {{ISI:000311143200006}}, } @article{ ISI:000310064400011, Author = {Miranda, Oswaldo D.}, Title = {{Stochastic backgrounds of gravitational waves from cosmological sources - the role of dark energy}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2012}}, Volume = {{426}}, Number = {{4}}, Pages = {{2758-2771}}, Month = {{NOV}}, Abstract = {{In this work we investigate the detectability of the gravitational stochastic background produced by cosmological sources in scenarios of structure formation. The calculation is performed in the framework of hierarchical structure formation using a PressSchechter-like formalism. The model considers the coalescences of three kinds of binary systems, namely double neutron stars (NSNS), the neutron starblack hole (NSBH) binaries and the black holeblack hole (BHBH) systems. We also included in the model the core-collapse supernovae leaving black holes as compact remnants. In particular, we use two different dark energy scenarios, specifically cosmological constant (?) and Chaplygin gas, in order to verify their influence on the cosmic star formation rate, the coalescence rates and the gravitational wave backgrounds. We calculate the gravitational wave signals separately for each kind of source and also determine their collective contribution for the stochastic background of gravitational waves. Concerning the compact binary systems, we verify that these sources produce stochastic backgrounds with signal-to-noise ratio (S/N) values similar to 1.5 (similar to 0.90) for NSNS, similar to 0.50 (similar to 0.30) for NSBH, similar to 0.20 (similar to 0.10) for BHBH and similar to 0.14 (similar to 0.07) for core-collapse supernovae for a pair of advanced LIGO detectors in the cosmological-constant (Chaplygin gas) cosmology. Particularly, the sensitivity of the future third-generation detectors such as the Einstein Telescope (ET), in the triangular configuration, could increase the present S/N values by a high factor (similar to 3001000) when compared to the S/N calculated for advanced LIGO detectors. As an example, the collective contribution of these sources can produce S/N similar to 3.3 (similar to 1.8) for the ? (Chaplygin gas) cosmology for a pair of advanced LIGO interferometers and within the frequency range similar to 10?Hz1.5?kHz. Considering ET we have S/N similar to 2200 (similar to 1300) for the ? (Chaplygin gas) cosmology. Thus, the third-generation gravitational wave detectors could be used to reconstruct the history of star formation in the Universe and to contribute for the characterization of the dark energy, for example, identifying if there is evidence for the evolution of the dark energy equation-of-state parameter w(a).}}, DOI = {{10.1111/j.1365-2966.2012.21887.x}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Miranda, Oswaldo/C-4748-2012}}, ORCID-Numbers = {{Miranda, Oswaldo/0000-0002-0109-2483}}, Unique-ID = {{ISI:000310064400011}}, } @article{ ISI:000308292300001, Author = {Bauswein, A. and Janka, H. -T. and Hebeler, K. and Schwenk, A.}, Title = {{Equation-of-state dependence of the gravitational-wave signal from the ring-down phase of neutron-star mergers}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{86}}, Number = {{6}}, Month = {{SEP 4}}, Abstract = {{Neutron star (NS) merger simulations are conducted for 38 representative microphysical descriptions of high-density matter in order to explore the equation-of-state (EoS) dependence of the postmerger ringdown phase. The formation of a deformed, oscillating, differentially rotating very massive NS is the typical outcome of the coalescence of two stars with 1.35M(circle dot) for most candidate EoSs. The oscillations of this object imprint a pronounced peak in the gravitational wave (GW) spectra, which is used to characterize the emission for a given model. The peak frequency of this postmerger GW signal correlates very well with the radii of nonrotating NSs, and thus allows us to constrain the high-density EoS by a GW detection. In the case of 1. 35-1.35M(circle dot) mergers the peak frequency scales particularly well with the radius of an NS with 1.6M(circle dot), where the maximum deviation from this correlation is only 60 m for fully microphysical EoSs which are compatible with NS observations. Combined with the uncertainty in the determination of the peak frequency it appears likely that a GW detection can measure the radius of a 1.6M(circle dot) NS with an accuracy of about 100-200 m. We also uncover relations of the peak frequency with the radii of nonrotating NSs with 1.35M(circle dot) or 1.8M(circle dot), with the radius or the central energy density of the maximum-mass Tolman-Oppenheimer-Volkoff configuration, and with the pressure or sound speed at a fiducial rest mass density of about twice the nuclear saturation density. Furthermore, it is found that a determination of the dominant postmerger GW frequency can provide an upper limit for the maximum mass of nonrotating NSs. The effect of variations of the binary setup are investigated and corresponding functional dependences between the peak frequency and radii of nonrotating NSs are derived. With higher total binary masses, correlations are tighter for radii of nonrotating NSs with higher masses. The prospects for a detection of the postmerger GW signal and a determination of the dominant GW frequency are estimated to be in the range of 0.015-1.2 events per year with the upcoming Advanced Laser Interferometer Gravitational Wave Observatory detector.}}, DOI = {{10.1103/PhysRevD.86.063001}}, Article-Number = {{063001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Schwenk, Achim/0000-0001-8027-4076}}, Unique-ID = {{ISI:000308292300001}}, } @article{ ISI:000307790900003, Author = {Glampedakis, K. and Jones, D. I. and Samuelsson, L.}, Title = {{Gravitational Waves from Color-Magnetic ``Mountains{''} in Neutron Stars}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2012}}, Volume = {{109}}, Number = {{8}}, Month = {{AUG 22}}, Abstract = {{Neutron stars may harbor the true ground state of matter in the form of strange quark matter. If present, this type of matter is expected to be a color superconductor, a consequence of quark pairing with respect to the color and flavor degrees of freedom. The stellar magnetic field threading the quark core becomes a color-magnetic admixture and, in the event that superconductivity is of type II, leads to the formation of color-magnetic vortices. In this Letter, we show that the volume-averaged color-magnetic vortex tension force should naturally lead to a significant degree of nonaxisymmetry in systems such as radio pulsars. We show that gravitational radiation from such color-magnetic ``mountains{''} in young pulsars, such as the Crab and Vela, could be observable by the future Einstein Telescope, thus, becoming a probe of paired quark matter in neutron stars. The detectability threshold can be pushed up toward the sensitivity level of Advanced LIGO if we invoke an interior magnetic field about a factor ten stronger than the surface polar field.}}, DOI = {{10.1103/PhysRevLett.109.081103}}, Article-Number = {{081103}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ORCID-Numbers = {{Jones, David/0000-0002-0117-7567}}, Unique-ID = {{ISI:000307790900003}}, } @article{ ISI:000308406500067, Author = {Hosain, M. A. and Sirr, A. and Ju, L. and Blair, D. G.}, Title = {{Novel Euler-LaCoste linkage as a very low frequency vertical vibration isolator}}, Journal = {{REVIEW OF SCIENTIFIC INSTRUMENTS}}, Year = {{2012}}, Volume = {{83}}, Number = {{8}}, Month = {{AUG}}, Abstract = {{LaCoste linkage vibration isolators have shown excellent performance for ultra-low frequency vertical vibration isolation. However, such isolators depend on the use of conventional pre-stressed coil springs, which suffer from creep. Here, we show that compressional Euler springs can be configured to create a stable tension unit for use in a LaCoste structure. In a proof of concept experiment, we demonstrate a vertical resonance frequency of 0.15 Hz in an Euler-LaCoste configuration with 200 mm height. The system enables the use of very low creep maraging steel as spring elements to eliminate the creep while minimising spring mass and reducing the effect of parasitic resonances. Larger scale systems with optimized Euler spring boundary conditions should achieve performance suitable for applications on third generation gravitational wave detectors such as the proposed Einstein telescope. (C) 2012 American Institute of Physics.{[}http://dx.doi.org/10.1063/1.4745505]}}, DOI = {{10.1063/1.4745505}}, Article-Number = {{085108}}, ISSN = {{0034-6748}}, EISSN = {{1089-7623}}, ResearcherID-Numbers = {{Ju, Li/C-2623-2013 }}, ORCID-Numbers = {{Blair, David/0000-0002-1501-2405 Ju, Li/0000-0002-7951-4295}}, Unique-ID = {{ISI:000308406500067}}, } @article{ ISI:000306944700028, Author = {Komma, J. and Schwarz, C. and Hofmann, G. and Heinert, D. and Nawrodt, R.}, Title = {{Thermo-optic coefficient of silicon at 1550nm and cryogenic temperatures}}, Journal = {{APPLIED PHYSICS LETTERS}}, Year = {{2012}}, Volume = {{101}}, Number = {{4}}, Month = {{JUL 23}}, Abstract = {{The thermo-optic coefficient dn/dT of silicon was measured at 1550nm in the wide temperature range from 5K to 300 K. For this purpose an interferometric measurement scheme was applied using the silicon sample as a Fabry-Perot etalon. The high resolution of this setup revealed a thermo-optic coefficient as low as 10(-8) K-1 at 5K. The presented results show an excellent agreement with former measurements above 30K including a value of dn/dT = 1.8 x 10(-4) K-1 at 300K. (C) 2012 American Institute of Physics. {[}http://dx.doi.org/10.1063/1.4738989]}}, DOI = {{10.1063/1.4738989}}, Article-Number = {{041905}}, ISSN = {{0003-6951}}, Unique-ID = {{ISI:000306944700028}}, } @article{ ISI:000305810600015, Author = {Ali, Asad and Christensen, Nelson and Meyer, Renate and Roever, Christian}, Title = {{Bayesian inference on EMRI signals using low frequency approximations}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2012}}, Volume = {{29}}, Number = {{14}}, Month = {{JUL 21}}, Abstract = {{Extreme mass ratio inspirals (EMRIs) are thought to be one of the most exciting gravitational wave sources to be detected with LISA. Due to their complicated nature and weak amplitudes the detection and parameter estimation of such sources is a challenging task. In this paper we present a statistical methodology based on Bayesian inference in which the estimation of parameters is carried out by advanced Markov chain Monte Carlo (MCMC) algorithms such as parallel tempering MCMC. We analysed high and medium mass EMRI systems that fall well inside the low frequency range of LISA. In the context of the Mock LISA Data Challenges, our investigation and results are also the first instance in which a fully Markovian algorithm is applied for EMRI searches. Results show that our algorithm worked well in recovering EMRI signals from different (simulated) LISA data sets having single and multiple EMRI sources and holds great promise for posterior computation under more realistic conditions. The search and estimation methods presented in this paper are general in their nature, and can be applied in any other scenario such as AdLIGO, AdVIRGO and Einstein Telescope with their respective response functions.}}, DOI = {{10.1088/0264-9381/29/14/145014}}, Article-Number = {{145014}}, ISSN = {{0264-9381}}, ResearcherID-Numbers = {{Christensen, Nelson/AAH-9184-2019 Rover, Christian/H-4892-2019}}, ORCID-Numbers = {{Christensen, Nelson/0000-0002-6870-4202 Rover, Christian/0000-0002-6911-698X}}, Unique-ID = {{ISI:000305810600015}}, } @article{ ISI:000305937500004, Author = {Taylor, Stephen R. and Gair, Jonathan R.}, Title = {{Cosmology with the lights off: Standard sirens in the Einstein Telescope era}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{86}}, Number = {{2}}, Month = {{JUL 3}}, Abstract = {{We explore the prospects for constraining cosmology using gravitational-wave (GW) observations of neutron-star binaries by the proposed Einstein Telescope (ET), exploiting the narrowness of the neutron-star mass function. This builds on our previous work in the context of advanced-era GW detectors. Double neutron-star (DNS) binaries are expected to be one of the first sources detected after ``first-light{''} of Advanced LIGO. DNS systems are expected to be detected at a rate of a few tens per year in the advanced era, but the proposed ET could catalog tens, if not hundreds, of thousands per year. Combining the measured source redshift distributions with GW-network distance determinations will permit not only the precision measurement of background cosmological parameters, but will provide an insight into the astrophysical properties of these DNS systems. Of particular interest will be to probe the distribution of delay times between DNS-binary creation and subsequent merger, as well as the evolution of the star-formation rate density within ET's detection horizon. Keeping H-0, Omega(m,0) and Omega(Lambda,0) fixed and investigating the precision with which the dark-energy equation-of-state parameters could be recovered, we found that with 10(5) detected DNS binaries, we could constrain these parameters to an accuracy similar to forecasted constraints from future CMB + BAO + SNIa measurements. Furthermore, modeling the merger delay-time distribution as a power-law (proportional to t(proportional to)) and the star-formation rate density as a parametrized version of the Porciani and Madau SF2 model, we find that the associated astrophysical parameters are constrained to within similar to 10\%. All parameter precisions scaled as 1/root N, where N is the number of cataloged detections. We also investigated how parameter precisions varied with the intrinsic underlying properties of the Universe and with the distance reach of the network (which is affected, for instance, by the low-frequency cutoff of the detector). We also consider various sources of distance-measurement errors in the third-generation era and how these can be folded into the analysis.}}, DOI = {{10.1103/PhysRevD.86.023502}}, Article-Number = {{023502}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Taylor, Stephen/0000-0003-0264-1453}}, Unique-ID = {{ISI:000305937500004}}, } @article{ ISI:000305681900009, Author = {Gossan, S. and Veitch, J. and Sathyaprakash, B. S.}, Title = {{Bayesian model selection for testing the no-hair theorem with black hole ringdowns}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{85}}, Number = {{12}}, Month = {{JUN 26}}, Abstract = {{In this paper we examine the extent to which black hole quasinormal modes (QNMs) could be used to test the no-hair theorem with future ground-and space-based gravitational-wave detectors. We model departures from general relativity (GR) by introducing extra parameters which change the mode frequencies or decay times from their values in GR. With the aid of Bayesian model selection, we assess the extent to which the presence of such a parameter could be inferred, and its value estimated. We find that it is harder to measure the departure of the mode decay times from their GR values than it is with the mode frequencies. The Einstein Telescope (ET, a third generation ground-based detector) could detect departures of as little as 8\% in the frequency of the dominant QNM mode of a 500M(circle dot) black hole, out to a maximum range of similar or equal to 6 Gpc (z similar or equal to 0.91). The New Gravitational Observatory (NGO, an ESA space mission to detect gravitational waves) can detect departures of similar to 0.6\% in a 10(8)M(circle dot) black hole to a luminosity distance of 50 Gpc (z similar or equal to 5.1), and departures of similar to 10\% in a 10(6)M(circle dot) black hole to a luminosity distance of similar or equal to 6 Gpc. In this exploratory work we have made a specific choice of source position (overhead), orientation (inclination angle of pi/3) and mass ratio of progenitor binary (m(1)/m(2) = 2). A more exhaustive Monte Carlo simulation that incorporates progenitor black hole spins and a hierarchical model for the growth of massive black holes is needed to evaluate a more realistic picture of the possibility of ET and NGO to carry out such tests.}}, DOI = {{10.1103/PhysRevD.85.124056}}, Article-Number = {{124056}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Veitch, John/0000-0002-6508-0713 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000305681900009}}, } @article{ ISI:000305810400007, Author = {Hild, S.}, Title = {{Beyond the second generation of laser-interferometric gravitational wave observatories}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2012}}, Volume = {{29}}, Number = {{12, SI}}, Month = {{JUN 21}}, Note = {{9th Edoardo Amaldi Conference on Gravitational Waves (Amaldi)/Meeting on Numerical Relativity - Data Analysis (NRDA), Cardiff, WALES, JUL 10-15, 2011}}, Organization = {{IUPAP}}, Abstract = {{This paper gives an overview of potential upgrades of second-generation gravitational wave detectors and the required key technologies to improve the limiting noise sources. In addition, the baseline design of the Einstein telescope, a European third-generation gravitational wave observatory, is briefly discussed.}}, DOI = {{10.1088/0264-9381/29/12/124006}}, Article-Number = {{124006}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Hild, Stefan/A-3864-2010}}, ORCID-Numbers = {{Hild, Stefan/0000-0001-9221-6009}}, Unique-ID = {{ISI:000305810400007}}, } @article{ ISI:000305810400014, Author = {Sathyaprakash, B. and Abernathy, M. and Acernese, F. and Ajith, P. and Allen, B. and Amaro-Seoane, P. and Andersson, N. and Aoudia, S. and Arun, K. and Astone, P. and Krishnan, B. and Barack, L. and Barone, F. and Barr, B. and Barsuglia, M. and Bassan, M. and Bassiri, R. and Beker, M. and Beveridge, N. and Bizouard, M. and Bond, C. and Bose, S. and Bosi, L. and Braccini, S. and Bradaschia, C. and Britzger, M. and Brueckner, F. and Bulik, T. and Bulten, H. J. and Burmeister, O. and Calloni, E. and Campsie, P. and Carbone, L. and Cella, G. and Chalkley, E. and Chassande-Mottin, E. and Chelkowski, S. and Chincarini, A. and Di Cintio, A. and Clark, J. and Coccia, E. and Colacino, C. N. and Colas, J. and Colla, A. and Corsi, A. and Cumming, A. and Cunningham, L. and Cuoco, E. and Danilishin, S. and Danzmann, K. and Daw, E. and De Salvo, R. and Del Pozzo, W. and Dent, T. and De Rosa, R. and Di Fiore, L. and Emilio, M. Di Paolo and Di Virgilio, A. and Dietz, A. and Doets, M. and Dueck, J. and Edwards, M. and Fafone, V. and Fairhurst, S. and Falferi, P. and Favata, M. and Ferrari, V. and Ferrini, F. and Fidecaro, F. and Flaminio, R. and Franc, J. and Frasconi, F. and Freise, A. and Friedrich, D. and Fulda, P. and Gair, J. and Galimberti, M. and Gemme, G. and Genin, E. and Gennai, A. and Giazotto, A. and Glampedakis, K. and Gossan, S. and Gouaty, R. and Graef, C. and Graham, W. and Granata, M. and Grote, H. and Guidi, G. and Hallam, J. and Hammond, G. and Hannam, M. and Harms, J. and Haughian, K. and Hawke, I. and Heinert, D. and Hendry, M. and Heng, I. and Hennes, E. and Hild, S. and Hough, J. and Huet, D. and Husa, S. and Huttner, S. and Iyer, B. and Jones, D. I. and Jones, G. and Kamaretsos, I. and Mishra, C. Kant and Kawazoe, F. and Khalili, F. and Kley, B. and Kokeyama, K. and Kokkotas, K. and Kroker, S. and Kumar, R. and Kuroda, K. and Lagrange, B. and Lastzka, N. and Li, T. G. F. and Lorenzini, M. and Losurdo, G. and Lueck, H. and Majorana, E. and Malvezzi, V. and Mandel, I. and Mandic, V. and Marka, S. and Marin, F. and Marion, F. and Marque, J. and Martin, I. and Mc Leod, D. and Mckechan, D. and Mehmet, M. and Michel, C. and Minenkov, Y. and Morgado, N. and Morgia, A. and Mosca, S. and Moscatelli, L. and Mours, B. and Mueller-Ebhardt, H. and Murray, P. and Naticchioni, L. and Nawrodt, R. and Nelson, J. and Shaughnessy, R. O' and Ott, C. D. and Palomba, C. and Paoli, A. and Parguez, G. and Pasqualetti, A. and Passaquieti, R. and Passuello, D. and Perciballi, M. and Piergiovanni, F. and Pinard, L. and Pitkin, M. and Plastino, W. and Plissi, M. and Poggiani, R. and Popolizio, P. and Porter, E. and Prato, M. and Prodi, G. and Punturo, M. and Puppo, P. and Rabeling, D. and Racz, I. and Rapagnani, P. and Re, V. and Read, J. and Regimbau, T. and Rehbein, H. and Reid, S. and Ricci, F. and Richard, F. and Robinson, C. and Rocchi, A. and Romano, R. and Rowan, S. and Ruediger, A. and Samblowski, A. and Santamaria, L. and Sassolas, B. and Schilling, R. and Schmidt, P. and Schnabel, R. and Schutz, B. and Schwarz, C. and Scott, J. and Seidel, P. and Sintes, A. M. and Somiya, K. and Sopuerta, C. F. and Sorazu, B. and Speirits, F. and Storchi, L. and Strain, K. and Strigin, S. and Sutton, P. and Tarabrin, S. and Taylor, B. and Thuerin, A. and Tokmakov, K. and Tonelli, M. and Tournefier, H. and Vaccarone, R. and Vahlbruch, H. and van den Brand, J. F. J. and Van den Broeck, C. and van der Putten, S. and van Veggel, M. and Vecchio, A. and Veitch, J. and Vetrano, F. and Vicere, A. and Vyatchanin, S. and Wessels, P. and Willke, B. and Winkler, W. and Woan, G. and Woodcraft, A. and Yamamoto, K.}, Title = {{Scientific objectives of Einstein Telescope}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2012}}, Volume = {{29}}, Number = {{12, SI}}, Month = {{JUN 21}}, Note = {{9th Edoardo Amaldi Conference on Gravitational Waves (Amaldi)/Meeting on Numerical Relativity - Data Analysis (NRDA), Cardiff, WALES, JUL 10-15, 2011}}, Organization = {{IUPAP}}, Abstract = {{The advanced interferometer network will herald a new era in observational astronomy. There is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from 1 Hz to 10 kHz, with sensitivity a factor 10 better in amplitude. Such detectors will be able to probe a range of topics in nuclear physics, astronomy, cosmology and fundamental physics, providing insights into many unsolved problems in these areas.}}, DOI = {{10.1088/0264-9381/29/12/124013}}, Article-Number = {{124013}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Bassan, Massimo/J-1652-2012 Hallam, Jonathan Mark/AAI-9469-2020 Schnabel, Roman/V-7759-2019 Marin, Francesco/I-7492-2013 Cuoco, Elena/O-4680-2019 Gemme, Gianluca/C-7233-2008 di virgilio, angela/AAA-4814-2019 Dent, Thomas/AAB-3674-2019 Sopuerta, Carlos F./L-3835-2014 Vicere', Andrea/J-1742-2012 Ott, Christian/G-2651-2011 Harms, Jan/O-7967-2019 Kokkotas, Kostas D/B-7878-2010 Martin, Iain/A-2445-2010 di virgilio, angela/E-9078-2015 Naticchioni, Luca/AAB-7775-2019 Willke, Benno/U-8992-2017 Graef, Christian/J-3167-2015 Bassan, Massimo/AAD-8716-2019 Poggiani, Rosa/P-8801-2018 Pitkin, Matthew/I-3802-2013 Falferi, Paolo/C-3439-2015 CHASSANDE-MOTTIN, Eric/ABC-2478-2020 Schutz, Bernard F/B-1504-2010 Rapagnani, Piero/T-2050-2019 Re, Virginia/F-6403-2013 Hild, Stefan/A-3864-2010 Vyatchanin, Sergey P/J-2238-2012 Strigin, Sergey E/I-8337-2012 Nelson, John/H-7215-2014 Martin, Iain/V-1198-2018 Prodi, Giovanni Andrea/B-4398-2010 Santamaria, Lucia/G-1297-2017 di cintio, arianna/AAI-1502-2019 Losurdo, Giovanni/K-1241-2014 Sintes, Alicia M/AAF-4791-2019 Kroker, Stefanie/V-3419-2017 Storchi, Loriano/K-3557-2018 Lueck, Harald/F-7100-2011 Somiya, Kentaro/ABE-2215-2020 Vecchio, Alberto/F-8310-2015 Husa, Sascha/AAB-6992-2019 Rocchi, Alessio/O-9499-2015 mosca, simona/I-7116-2012 Harms, Jan/J-4359-2012 Santamaria, Lucia/A-7269-2012 Danilishin, Stefan/K-7262-2012 Van Den Broeck, Chris/R-7871-2018 Acernese, Fausto/AAX-5705-2020 O'Shaughnessy, Richard/AAA-3625-2021 Chincarini, Andrea/J-9998-2018 Cuoco, Elena Dr./I-8789-2012 Bulik, Tomasz/AAJ-6742-2020 Prato, Mirko/AAD-9075-2019 Punturo, Michele/I-3995-2012 Colla, Alberto/J-4694-2012 Rapagnani, Piero/J-4783-2012 Cella, Giancarlo/A-9946-2012 Frasconi, Franco/K-1068-2016 Lorenzini, Matteo/AAC-6035-2021 Seoane, Pau Amaro/U-8229-2017 Fidecaro, Francesco/H-9581-2017 calloni, enrico/K-5852-2019 Prato, Mirko/D-8531-2012 Puppo, Paola/J-4250-2012 Allen, Bruce/K-2327-2012 Iyer, Bala R./E-2894-2012 Khalili, Farit Ya/D-8113-2012 Barr, Bryan/G-3348-2019 Sorazu, Borja/H-6966-2018 Sathyaprakash, Bangalore/M-1235-2014 Passaquieti, Roberto/U-3083-2017 Strain, Kenneth/D-5236-2011}}, ORCID-Numbers = {{Bassan, Massimo/0000-0001-6512-8003 Hallam, Jonathan Mark/0000-0002-7087-0461 Marin, Francesco/0000-0001-8227-124X Cuoco, Elena/0000-0002-6528-3449 Gemme, Gianluca/0000-0002-1127-7406 Sopuerta, Carlos F./0000-0002-1779-4447 Vicere', Andrea/0000-0003-0624-6231 Ott, Christian/0000-0003-4993-2055 Harms, Jan/0000-0002-7332-9806 Kokkotas, Kostas D/0000-0001-6048-2919 di virgilio, angela/0000-0002-2237-7533 Naticchioni, Luca/0000-0003-2918-0730 Willke, Benno/0000-0003-0524-2925 Graef, Christian/0000-0002-4535-2603 Pitkin, Matthew/0000-0003-4548-526X Falferi, Paolo/0000-0002-1929-4710 CHASSANDE-MOTTIN, Eric/0000-0003-3768-9908 Rapagnani, Piero/0000-0002-1865-6126 Hild, Stefan/0000-0001-9221-6009 Nelson, John/0000-0002-6928-617X Martin, Iain/0000-0001-7300-9151 Prodi, Giovanni Andrea/0000-0001-5256-915X Santamaria, Lucia/0000-0002-5986-0449 Losurdo, Giovanni/0000-0003-0452-746X Kroker, Stefanie/0000-0002-7584-7359 Storchi, Loriano/0000-0001-5021-7759 Lueck, Harald/0000-0001-9350-4846 Somiya, Kentaro/0000-0003-2601-2264 Vecchio, Alberto/0000-0002-6254-1617 Husa, Sascha/0000-0002-0445-1971 Rocchi, Alessio/0000-0002-1382-9016 mosca, simona/0000-0001-7869-8275 Harms, Jan/0000-0002-7332-9806 Danilishin, Stefan/0000-0001-7758-7493 Van Den Broeck, Chris/0000-0001-6800-4006 Acernese, Fausto/0000-0003-3103-3473 O'Shaughnessy, Richard/0000-0001-5832-8517 Cuoco, Elena Dr./0000-0002-6528-3449 Prato, Mirko/0000-0002-2188-8059 Punturo, Michele/0000-0001-8722-4485 Rapagnani, Piero/0000-0002-1865-6126 Cella, Giancarlo/0000-0002-0752-0338 Frasconi, Franco/0000-0003-4204-6587 Lorenzini, Matteo/0000-0002-2765-7905 Fidecaro, Francesco/0000-0002-6189-3311 Prato, Mirko/0000-0002-2188-8059 Puppo, Paola/0000-0003-4677-5015 Allen, Bruce/0000-0003-4285-6256 Iyer, Bala R./0000-0002-4141-5179 Barr, Bryan/0000-0002-5232-2736 Sorazu, Borja/0000-0002-6178-3198 Schutz, Bernard/0000-0001-9487-6983 van den Brand, Johannes/0000-0003-4434-5353 Hawke, Ian/0000-0003-4805-0309 Scott, Jamie/0000-0001-6701-6515 Di Paolo Emilio, Maurizio/0000-0002-9558-3610 Krishnan, Badri/0000-0003-3015-234X Poggiani, Rosa/0000-0002-9968-2464 Guidi, Gianluca/0000-0002-3061-9870 Barone, Fabrizio/0000-0002-8069-8490 calloni, enrico/0000-0003-4819-3297 Sathyaprakash, Bangalore/0000-0003-3845-7586 Coccia, Eugenio/0000-0002-6669-5787 Romano, Rocco/0000-0002-0485-6936 Bassiri, Riccardo/0000-0001-8171-6833 Palomba, Cristiano/0000-0002-4450-9883 Sintes, Alicia M/0000-0001-9050-7515 Yamamoto, Kazuhiro/0000-0001-5647-6735 Woan, Graham/0000-0003-0381-0394 Hammond, Giles/0000-0002-1414-3622 Mandel, Ilya/0000-0002-6134-8946 Schmidt, Patricia/0000-0003-1542-1791 Ricci, Fulvio/0000-0001-5475-4447 Fairhurst, Stephen/0000-0001-8480-1961 Chincarini, Andrea/0000-0003-4094-9942 Granata, Massimo/0000-0003-3275-1186 Del Pozzo, Walter/0000-0003-3978-2030 Amaro Seoane, Pau/0000-0003-3993-3249 Freise, Andreas/0000-0001-6586-9901 Daw, Edward/0000-0002-3780-5430 Passaquieti, Roberto/0000-0003-4753-9428 Plastino, Wolfango/0000-0002-5737-6346 Mishra, Chandra Kant/0000-0002-8115-8728 Vetrano, Flavio/0000-0002-7523-4296 Piergiovanni, Francesco/0000-0001-8063-828X Bulik, Tomasz/0000-0003-2045-4803 Majorana, Ettore/0000-0002-2383-3692 Tokmakov, Kirill/0000-0002-2808-6593 Speirits, Fiona/0000-0002-6460-5231 Veitch, John/0000-0002-6508-0713 Strain, Kenneth/0000-0002-2066-5355}}, Unique-ID = {{ISI:000305810400014}}, } @article{ ISI:000304246100037, Author = {Passamonti, Andrea and Glampedakis, Kostas}, Title = {{Non-linear viscous damping and gravitational wave detectability of the f-mode instability in neutron stars}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2012}}, Volume = {{422}}, Number = {{4}}, Pages = {{3327-3338}}, Month = {{JUN}}, Abstract = {{We study the damping of the gravitational radiation-driven f-mode instability in rotating neutron stars by non-linear bulk viscosity in the so-called suprathermal regime. In this regime the dissipative action of bulk viscosity is known to be enhanced as a result of non-linear contributions with respect to the oscillation amplitude. Our analysis of the f-mode instability is based on a time-domain code that evolves linear perturbations of rapidly rotating polytropic neutron star models. The extracted mode frequency and eigenfunctions are subsequently used in standard energy integrals for the gravitational wave growth and viscous damping. We find that non-linear bulk viscosity has a moderate impact on the size of the f-mode instability window, becoming an important factor and saturating the modes growth at a relatively large oscillation amplitude. We show similarly that non-linear bulk viscosity leads to a rather high saturation amplitude even for the r-mode instability. In addition, we show that the action of bulk viscosity can be significantly mitigated by the presence of superfluidity in neutron star matter. Apart from revising the f-modes instability window we provide results on the modes gravitational wave detectability. Considering an f-mode-unstable neutron star located in the Virgo cluster and assuming a mode amplitude at the level allowed by bulk viscosity, we find that the emitted gravitational wave signal could be detectable by advanced ground-based detectors such as Advanced LIGO/Virgo and the Einstein Telescope.}}, DOI = {{10.1111/j.1365-2966.2012.20849.x}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Passamonti, Andrea/H-7644-2015}}, ORCID-Numbers = {{Passamonti, Andrea/0000-0002-7457-4926}}, Unique-ID = {{ISI:000304246100037}}, } @article{ ISI:000304390900120, Author = {Kowalska, I. and Bulik, T. and Belczynski, K.}, Title = {{Gravitational wave background from Population III binaries}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2012}}, Volume = {{541}}, Month = {{MAY}}, Abstract = {{Context. Current star formation models imply that the binary fraction of Population III stars is non-zero. The evolution of these binaries must have led to the formation of compact object binaries. Aims. We estimate the gravitational wave background originating in these binaries and discuss its observability. Methods. The properties of the Population III binaries are investigated using a binary population synthesis code. We numerically model the background and take into account the evolution of eccentric binaries. Results. The gravitational wave background from Population III binaries dominates the spectrum below 100 Hz. If the binary fraction is larger than 10(-2), the background will be detectable by Einstein Telescope (ET), Laser Interferometer Space Antenna (LISA), and DECi-Hertz Interferometer Gravitational wave Observatory (DECIGO). Conclusions. The gravitational wave background from Population III binaries will dominate the spectrum below 100 Hz. The instruments LISA, ET, and DECIGO should either see it easily or, in the case of non-detection, provide very strong constraints on the properties of the Population III stars.}}, DOI = {{10.1051/0004-6361/201118604}}, Article-Number = {{A120}}, ISSN = {{0004-6361}}, EISSN = {{1432-0746}}, ResearcherID-Numbers = {{Bulik, Tomasz/AAJ-6742-2020 }}, ORCID-Numbers = {{Bulik, Tomasz/0000-0003-2045-4803 Kowalska-Leszczynska, Izabela/0000-0002-6569-3800}}, Unique-ID = {{ISI:000304390900120}}, } @article{ ISI:000302175500091, Author = {Fryer, Chris L. and Belczynski, Krzysztof and Wiktorowicz, Grzegorz and Dominik, Michal and Kalogera, Vicky and Holz, Daniel E.}, Title = {{COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2012}}, Volume = {{749}}, Number = {{1}}, Month = {{APR 10}}, Abstract = {{The mass distribution of neutron stars and stellar-mass black holes provides vital clues into the nature of stellar core collapse and the physical engine responsible for supernova explosions. A number of supernova engines have been proposed: neutrino- or oscillation-driven explosions enhanced by early (developing in 10-50 ms) and late-time (developing in 200 ms) convection as well as magnetic field engines (in black hole accretion disks or neutron stars). Using our current understanding of supernova engines, we derive mass distributions of stellar compact remnants. We provide analytic prescriptions for both single-star models (as a function of initial star mass) and for binary-star models-prescriptions for compact object masses for major population synthesis codes. These prescriptions have implications for a range of observations: X-ray binary populations, supernova explosion energies, and gravitational wave sources. We show that advanced gravitational radiation detectors (like LIGO/VIRGO or the Einstein Telescope) will be able to further test the supernova explosion engine models once double black hole inspirals are detected.}}, DOI = {{10.1088/0004-637X/749/1/91}}, Article-Number = {{91}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ORCID-Numbers = {{Wiktorowicz, Grzegorz/0000-0001-6106-0515 Holz, Daniel/0000-0002-0175-5064}}, Unique-ID = {{ISI:000302175500091}}, } @article{ ISI:000301977700013, Author = {Arun, K. G.}, Title = {{Generic bounds on dipolar gravitational radiation from inspiralling compact binaries}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2012}}, Volume = {{29}}, Number = {{7}}, Month = {{APR 7}}, Abstract = {{Various alternative theories of gravity predict dipolar gravitational radiation in addition to quadrupolar radiation. We show that gravitational wave (GW) observations of inspiralling compact binaries can put interesting constraints on the strengths of the dipole modes of GW polarizations. We put forward a physically motivated gravitational waveform for dipole modes, in the Fourier domain, in terms of two parameters: one which captures the relative amplitude of the dipole mode with respect to the quadrupole mode (alpha) and the other a dipole term in the phase (beta). We then use this two-parameter representation to discuss typical bounds on their values using GW measurements. We obtain the expected bounds on the amplitude parameter alpha and the phase parameter beta for advanced LIGO (AdvLIGO) and Einstein telescope (ET) noise power spectral densities using Fisher information matrix. AdvLIGO and ET may at best bound alpha to an accuracy of similar to 10(-2) and similar to 10(-3) and beta to an accuracy of similar to 10(-5) and similar to 10(-6).}}, DOI = {{10.1088/0264-9381/29/7/075011}}, Article-Number = {{075011}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, Unique-ID = {{ISI:000301977700013}}, } @article{ ISI:000302983700001, Author = {Rakhubovsky, Andrey A. and Vyatchanin, Sergey P.}, Title = {{Sensitivity of laser gravitational-wave detectors with stable double-pumped optical spring}}, Journal = {{PHYSICS LETTERS A}}, Year = {{2012}}, Volume = {{376}}, Number = {{17}}, Pages = {{1405-1411}}, Month = {{MAR 26}}, Abstract = {{We analyze the sensitivity of gravitational-wave antenna with stable double optical spring created by two independent pumps. We investigate regime of three close eigen frequencies (roots of characteristic equation) which appears to provide more wide frequency band in which sensitivity of antenna can beat Standard Quantum Limit (SQL) than previously considered regime with two close eigen frequencies. We take into account optical losses and show that they do not degrade sensitivity significantly. We also demonstrate possible application of considered regime to Einstein Telescope. (c) 2012 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.physleta.2012.03.030}}, ISSN = {{0375-9601}}, EISSN = {{1873-2429}}, ResearcherID-Numbers = {{Vyatchanin, Sergey P/J-2238-2012 Rakhubovsky, Andrey/E-1306-2012}}, ORCID-Numbers = {{Rakhubovsky, Andrey/0000-0001-8643-670X}}, Unique-ID = {{ISI:000302983700001}}, } @article{ ISI:000303155000009, Author = {Strigin, S. E.}, Title = {{The Effect of Parametric Oscillatory Instability in a Fabry-Perot Cavity of the Einstein Telescope}}, Journal = {{OPTICS AND SPECTROSCOPY}}, Year = {{2012}}, Volume = {{112}}, Number = {{3}}, Pages = {{373-376}}, Month = {{MAR}}, Abstract = {{The nonlinear effect of a parametric oscillatory instability in a Fabry-Perot cavity of the Einstein Telescope is investigated. Unstable combinations of elastic and optical modes are calculated for two possible configurations of the third-generation gravitational-wave detector. The results are compared with those for the LIGO gravitational-wave interferometer. DOI: 10.1134/S0030400X12030198}}, DOI = {{10.1134/S0030400X12030198}}, ISSN = {{0030-400X}}, EISSN = {{1562-6911}}, ResearcherID-Numbers = {{Strigin, Sergey E/I-8337-2012}}, Unique-ID = {{ISI:000303155000009}}, } @article{ ISI:000300938700005, Author = {Regimbau, Tania and Giampanis, Stefanos and Siemens, Xavier and Mandic, Vuk}, Title = {{Stochastic background from cosmic (super)strings: Popcorn-like and (Gaussian) continuous regimes}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{85}}, Number = {{6}}, Month = {{MAR 1}}, Abstract = {{In the era of the next generation of gravitational wave experiments a stochastic background from cusps of cosmic (super) strings is expected to be probed and, if not detected, to be significantly constrained. A popcornlike background can be, for part of the parameter space, as pronounced as the (Gaussian) continuous contribution from unresolved sources that overlap in frequency and time. We study both contributions from unresolved cosmic string cusps over a range of frequencies relevant to ground based interferometers, such as the LIGO/Virgo second generation and Einstein Telescope third generation detectors, the space antenna LISA, and pulsar timing arrays. We compute the sensitivity (at the 2 sigma level) in the parameter space for the LIGO/Virgo second generation detector, the Einstein Telescope detector, LISA, and pulsar timing arrays. We conclude that the popcorn regime is complementary to the continuous background. Its detection could therefore enhance confidence in a stochastic background detection and possibly help determine fundamental string parameters such as the string tension and the reconnection probability.}}, DOI = {{10.1103/PhysRevD.85.066001}}, Article-Number = {{066001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000300938700005}}, } @article{ ISI:000300836100002, Author = {Lackey, Benjamin D. and Kyutoku, Koutarou and Shibata, Masaru and Brady, Patrick R. and Friedman, John L.}, Title = {{Extracting equation of state parameters from black hole-neutron star mergers: Nonspinning black holes}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2012}}, Volume = {{85}}, Number = {{4}}, Month = {{FEB 28}}, Abstract = {{The late inspiral, merger, and ringdown of a black hole-neutron star (BHNS) system can provide information about the neutron-star equation of state (EOS). Candidate EOSs can be approximated by a parametrized piecewise-polytropic EOS above nuclear density, matched to a fixed low-density EOS; and we report results from a large set of BHNS inspiral simulations that systematically vary two parameters. To within the accuracy of the simulations, we find that, apart from the neutron-star mass, a single physical parameter Lambda, describing its deformability, can be extracted from the late inspiral, merger, and ringdown waveform. This parameter is related to the radius, mass, and l = 2 Love number, k(2), of the neutron star by Lambda = 2k(2)R(5)/3M(NS)(5), and it is the same parameter that determines the departure from point-particle dynamics during the early inspiral. Observations of gravitational waves from BHNS inspiral thus restrict the EOS to a surface of constant Lambda in the parameter space, thickened by the measurement error. Using various configurations of a single Advanced LIGO detector, we find that Lambda(1/5) or equivalently R can be extracted to 10-50\% accuracy from single events for mass ratios of Q = 2 and 3 at a distance of 100 Mpc, while with the proposed Einstein Telescope, EOS parameters can be extracted to accuracy an order of magnitude better.}}, DOI = {{10.1103/PhysRevD.85.044061}}, Article-Number = {{044061}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Brady, Patrick/0000-0002-4611-9387 Kyutoku, Koutarou/0000-0003-3179-5216}}, Unique-ID = {{ISI:000300836100002}}, } @inproceedings{ ISI:000307754800047, Author = {Kamaretsos, Ioannis}, Editor = {{Hannam, M and Sutton, P and Hild, S and VanDenBroeck, C}}, Title = {{From black holes to their progenitors: A full population study in measuring black hole binary parameters from ringdown signals}}, Booktitle = {{9TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES (AMALDI 9) AND THE 2011 NUMERICAL RELATIVITY - DATA ANALYSIS MEETING (NRDA 2011)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2012}}, Volume = {{363}}, Note = {{9th Edoardo Amaldi Conference on Gravitational Waves (Amaldi)/Meeting on Numerical Relativity - Data Analysis (NRDA), Cardiff, WALES, JUL 10-15, 2011}}, Organization = {{IUPAP}}, Abstract = {{A perturbed black hole emits gravitational radiation, usually termed the ringdown signal, whose frequency and time-constant depends on the mass and spin of the black hole. I investigate the case of a binary black hole merger resulting from two initially non-spinning black holes of various mass ratios, in quasi-circular orbits. The observed ringdown signal will be determined, among other things, by the black hole's spin-axis orientation with respect to Earth, its sky position and polarization angle - parameters which can take any values in a particular observation. I have carried out a statistical analysis of the effect of these variables, focusing on detection and measurement of the multimode ringdown signals using the reformulated European LISA mission, Next Gravitational-Wave Observatory, NGO, the third generation ground-based observatory, Einstein Telescope and the advanced era detector, aLIGO. To the extent possible I have discussed the effect of these results on plausible event rates, as well as astrophysical implications concerning the formation and growth of supermassive and intermediate mass black holes.}}, DOI = {{10.1088/1742-6596/363/1/012047}}, Article-Number = {{012047}}, ISSN = {{1742-6588}}, Unique-ID = {{ISI:000307754800047}}, } @article{ ISI:000314808600004, Author = {Vyatchanin, S. P. and Strigin, S. E.}, Title = {{Parametric oscillatory instability in gravitational wave laser detectors}}, Journal = {{PHYSICS-USPEKHI}}, Year = {{2012}}, Volume = {{55}}, Number = {{11}}, Pages = {{1115-1123}}, Abstract = {{The nonlinear effect of parametric oscillatory instability in the gravitational wave laser detector (antenna) is considered as a factor that considerably reduces the sensitivity of the device. It is shown that in an antenna with a circulating power above a certain threshold value there occurs excitation of Stokes optical modes in the Fabry-Perot resonators and of test mass elastic modes. Parametric oscillatory instability in gravitational wave interferometers of the second (LIGO, Virgo, LCGT, GEO-600) and third (ET - Einstein Telescope) generation with different types of pump is examined. The effect discussed has been observed not only in gravitational wave laser interferometers, but also many times in other opto-mechanical systems. All current methods for suppressing parametric oscillatory instability in gravitational wave interferometers are also discussed, both passive and active.}}, DOI = {{10.3367/UFNe.0182.201211e.1195}}, ISSN = {{1063-7869}}, EISSN = {{1468-4780}}, ResearcherID-Numbers = {{Strigin, Sergey E/I-8337-2012}}, Unique-ID = {{ISI:000314808600004}}, } @inproceedings{ ISI:000307754800056, Author = {Yagi, Kent and Nishizawa, Atsushi and Yoo, Chul-Moon}, Editor = {{Hannam, M and Sutton, P and Hild, S and VanDenBroeck, C}}, Title = {{Probing the Inhomogeneous Universe with Gravitational Wave Cosmology}}, Booktitle = {{9TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES (AMALDI 9) AND THE 2011 NUMERICAL RELATIVITY - DATA ANALYSIS MEETING (NRDA 2011)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2012}}, Volume = {{363}}, Note = {{9th Edoardo Amaldi Conference on Gravitational Waves (Amaldi)/Meeting on Numerical Relativity - Data Analysis (NRDA), Cardiff, WALES, JUL 10-15, 2011}}, Organization = {{IUPAP}}, Abstract = {{If we assume that we live in the center of a spherical inhomogeneous universe, we can explain the apparent accelerating expansion of the universe without introducing the unknown dark energy or modifying gravitational theory. Direct measurement of the cosmic acceleration can be a powerful tool in distinguishing Lambda CDM and the inhomogeneous models. If Lambda CDM is the correct model, we have shown that DECIGO/BBO has sufficient ability to detect the positive redshift drift of the source by observing gravitational waves from neutron star binaries for 5-10 years. This enables us to rule out any Lemaitre-Tolman-Bondi (LTB) void model with monotonically increasing density profile. Furthermore, by detecting the positive redshift drift at z similar to 0, we can even rule out generic LTB models unless we allow unrealistically steep density gradient at z similar to 0. We also show that the measurement accuracy is slightly improved when we consider the joint search of DECIGO/BBO and the third generation Einstein Telescope. This test can be performed with GW observations alone without any reference to electromagnetic observations.}}, DOI = {{10.1088/1742-6596/363/1/012056}}, Article-Number = {{012056}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, ORCID-Numbers = {{Nishizawa, Atsushi/0000-0003-3562-0990}}, Unique-ID = {{ISI:000307754800056}}, } @inproceedings{ ISI:000307754800046, Author = {Filloux, Ch. and Pacheco, J. A. de Freitas and Durier, F. and de Araujo, J. C. N.}, Editor = {{Hannam, M and Sutton, P and Hild, S and VanDenBroeck, C}}, Title = {{Gravitational ringdown signal from coalescences of SMBH binaries - detection rates for LISA and ET}}, Booktitle = {{9TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES (AMALDI 9) AND THE 2011 NUMERICAL RELATIVITY - DATA ANALYSIS MEETING (NRDA 2011)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2012}}, Volume = {{363}}, Note = {{9th Edoardo Amaldi Conference on Gravitational Waves (Amaldi)/Meeting on Numerical Relativity - Data Analysis (NRDA), Cardiff, WALES, JUL 10-15, 2011}}, Organization = {{IUPAP}}, Abstract = {{The coalescence history of massive black holes is derived from cosmological simulations, in which their evolution and that of the host galaxies are followed in a consistent way. With the coalescence rate per comoving volume and per mass interval derived from the simulations we estimate the expected detection rate distribution of ``ring-down{''} gravitational wave signals along frequencies accessible by LISA and Einstein Telescope (ET). For LISA, a total detection rate of about 15 yr(-1) is predicted for events having a signal-to-noise ratio equal to 10. For ET, one event each 14 months down to one event each 4 years is expected with a signal-to-noise ratio of 5. The detection of these gravitational signals and their distribution in frequency would be in the future an important tool able to discriminate among different scenarios for the origin of supermassive black holes.}}, DOI = {{10.1088/1742-6596/363/1/012046}}, Article-Number = {{012046}}, ISSN = {{1742-6588}}, EISSN = {{1742-6596}}, ResearcherID-Numbers = {{de Araujo, Jose C N/C-5181-2013}}, ORCID-Numbers = {{de Araujo, Jose C N/0000-0003-4418-4289}}, Unique-ID = {{ISI:000307754800046}}, } @article{ ISI:000298649600005, Author = {Marassi, S. and Schneider, R. and Corvino, G. and Ferrari, V. and Portegies Zwart, S.}, Title = {{Imprint of the merger and ring-down on the gravitational wave background from black hole binaries coalescence}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{84}}, Number = {{12}}, Month = {{DEC 20}}, Abstract = {{We compute the gravitational wave background (GWB) generated by a cosmological population of black hole-black hole (BH-BH) binaries using hybrid waveforms recently produced by numerical simulations of (BH-BH) coalescence, which include the inspiral, merger, and ring-down contributions. A large sample of binary systems is simulated using the population synthesis code SeBa, and we extract fundamental statistical information on (BH-BH) physical parameters (primary and secondary BH masses, orbital separations and eccentricities, formation, and merger time scales). We then derive the binary birth and merger rates using the theoretical cosmic star formation history obtained from a numerical study which reproduces the available observational data at redshifts z < 8. We evaluate the contributions of the inspiral, merger, and ring-down signals to the GWB, and discuss how these depend on the parameters which critically affect the number of coalescing (BH-BH) systems. We find that Advanced LIGO/Virgo have a chance to detect the GWB signal from the inspiral phase with a (S/N) = 10 only for the most optimistic model, which predicts the highest local merger rate of 0: 85 Mpc(-3) Myr(-1). Third generation detectors, such as the Einstein Telescope (ET), could reveal the GWB from the inspiral phase predicted by any of the considered models. In addition, ET could sample the merger phase of the evolution at least for models which predict local merger rates between {[}0.053-0.85] Mpc(-3) Myr(-1), which are more than a factor 2 lower than the upper limit inferred from the analysis of the LIGO S5 run {[}J. Abadie et al., Phys. Rev. D 83, 122005 (2011)]. The frequency dependence and amplitude of the GWB generated during the coalescence is very sensitive to the adopted core mass threshold for BH formation. This opens up the possibility to better understand the final stages of the evolution of massive stellar binaries using observational constraints on the associated gravitational wave emission.}}, DOI = {{10.1103/PhysRevD.84.124037}}, Article-Number = {{124037}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Corvino, Giovanni/D-5918-2011 Schneider, Raffaella/E-4216-2017 }}, ORCID-Numbers = {{Schneider, Raffaella/0000-0001-9317-2888 Marassi, Stefania/0000-0001-9018-4867}}, Unique-ID = {{ISI:000298649600005}}, } @article{ ISI:000297702400092, Author = {Mehmet, Moritz and Ast, Stefan and Eberle, Tobias and Steinlechner, Sebastian and Vahlbruch, Henning and Schnabel, Roman}, Title = {{Squeezed light at 1550 nm with a quantum noise reduction of 12.3 dB}}, Journal = {{OPTICS EXPRESS}}, Year = {{2011}}, Volume = {{19}}, Number = {{25}}, Pages = {{25763-25772}}, Month = {{DEC 5}}, Abstract = {{Continuous-wave squeezed states of light at the wavelength of 1550 nm have recently been demonstrated, but so far the obtained factors of noise suppression still lag behind today's best squeezing values demonstrated at 1064 nm. Here we report on the realization of a half-monolithic nonlinear resonator based on periodically-poled potassium titanyl phosphate which enabled the direct detection of up to 12.3 dB of squeezing at 5 MHz. Squeezing was observed down to a frequency of 2 kHz which is well within the detection band of gravitational wave interferometers. Our results suggest that a long-term stable 1550 nm squeezed light source can be realized with strong squeezing covering the entire detection band of a 3rd generation gravitational-wave detector such as the Einstein Telescope. (C) 2011 Optical Society of America}}, DOI = {{10.1364/OE.19.025763}}, ISSN = {{1094-4087}}, ResearcherID-Numbers = {{Schnabel, Roman/V-7759-2019 Steinlechner, Sebastian S/D-5781-2013 Ast, Stefan/R-4514-2017}}, ORCID-Numbers = {{Steinlechner, Sebastian S/0000-0003-4710-8548 Ast, Stefan/0000-0003-4531-273X}}, Unique-ID = {{ISI:000297702400092}}, } @article{ ISI:000296997100007, Author = {Gurkovsky, Alexey G. and Heinert, Daniel and Hild, Stefan and Nawrodt, Ronny and Somiya, Kentaro and Vyatchanin, Sergey P. and Wittel, Holger}, Title = {{Reducing thermal noise in future gravitational wave detectors by employing Khalili etalons}}, Journal = {{PHYSICS LETTERS A}}, Year = {{2011}}, Volume = {{375}}, Number = {{46}}, Pages = {{4147-4157}}, Month = {{NOV 7}}, Abstract = {{Reduction of thermal noise in dielectric mirror coatings is a key issue for the sensitivity improvement in the second and third generation interferometric gravitational wave detectors. Replacing an end mirror of the interferometer by an anti-resonant cavity (a so-called Khalili cavity) has been proposed to realize the reduction of the overall thermal noise level. In this article we show that the use of a Khalili etalon, which requires less hardware than a Khalili cavity, yields still a significant reduction of thermal noise. We identify the optimum distribution of coating layers on the front and rear surfaces of the etalon and compare the total noise budget with a conventional mirror. In addition we briefly discuss advantages and disadvantages of the Khalili etalon compared with the Khalili cavity in terms of technical aspects, such as interferometric length control and thermal lensing. (C) 2011 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.physleta.2011.07.063}}, ISSN = {{0375-9601}}, EISSN = {{1873-2429}}, ResearcherID-Numbers = {{Hild, Stefan/A-3864-2010 Vyatchanin, Sergey P/J-2238-2012 Nawrodt, Ronny/J-5155-2014 Somiya, Kentaro/ABE-2215-2020}}, ORCID-Numbers = {{Hild, Stefan/0000-0001-9221-6009 Somiya, Kentaro/0000-0003-2601-2264}}, Unique-ID = {{ISI:000296997100007}}, } @article{ ISI:000296913600002, Author = {Bond, Charlotte and Fulda, Paul and Carbone, Ludovico and Kokeyama, Keiko and Freise, Andreas}, Title = {{Higher order Laguerre-Gauss mode degeneracy in realistic, high finesse cavities}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{84}}, Number = {{10}}, Month = {{NOV 4}}, Abstract = {{Higher order Laguerre-Gauss (LG) beams have been proposed for use in future gravitational wave detectors, such as upgrades to the Advanced LIGO detectors and the Einstein Telescope, for their potential to reduce the effects of the thermal noise of the test masses. This paper details the theoretical analysis and simulation work carried out to investigate the behavior of LG beams in realistic optical setups, in particular, the coupling between different LG modes in a linear cavity. We present a new analytical approximation to compute the coupling between modes, using Zernike polynomials to describe mirror surface distortions. We apply this method in a study of the behavior of the LG(33) mode within realistic arm cavities, using measured mirror surface maps from the Advanced LIGO project. We show mode distortions that can be expected to arise due to the degeneracy of higher order spatial modes within such cavities and relate this to the theoretical analysis. Finally, we identify the mirror distortions which cause significant coupling from the LG(33) mode into other order 9 modes and derive requirements for the mirror surfaces.}}, DOI = {{10.1103/PhysRevD.84.102002}}, Article-Number = {{102002}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Freise, Andreas/F-8892-2011 }}, ORCID-Numbers = {{Freise, Andreas/0000-0001-6586-9901}}, Unique-ID = {{ISI:000296913600002}}, } @article{ ISI:000297045700063, Author = {Stergioulas, Nikolaos and Bauswein, Andreas and Zagkouris, Kimon and Janka, Hans-Thomas}, Title = {{Gravitational waves and non-axisymmetric oscillation modes in mergers of compact object binaries}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2011}}, Volume = {{418}}, Number = {{1}}, Pages = {{427-436}}, Month = {{NOV}}, Abstract = {{We study the excitation of non-axisymmetric modes in the post-merger phase of binary compact object mergers and the associated gravitational wave emission. Our analysis is based on general-relativistic simulations, in the spatial conformal flatness approximation, using smoothed particle hydrodynamics for the evolution of matter, and we use a set of equal- and unequal-mass models, described by two non-zero-temperature hadronic equations of state and by one strange star equation of state. Through Fourier transforms of the evolution of matter variables, we can identify a number of oscillation modes, as well as several non-linear components (combination frequencies). We focus on the dominant m= 2 mode, which forms a triplet with two non-linear components that are the result of coupling to the quasi-radial mode. A corresponding triplet of frequencies is identified in the gravitational wave spectrum, when the individual masses of the compact objects are in the most likely range of 1.21.35 M?. We can thus associate, through direct analysis of the dynamics of the fluid, a specific frequency peak in the gravitational wave spectrum with the non-linear component resulting from the difference between the m= 2 mode and the quasi-radial mode. Once such observation becomes available, both the m= 2 and quasi-radial mode frequencies could be extracted, allowing for the application of gravitational wave asteroseismology to the post-merger remnant and leading to tight constraints on the equation of state of high-density matter.}}, DOI = {{10.1111/j.1365-2966.2011.19493.x}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Stergioulas, Nikolaos/AAF-1202-2020}}, ORCID-Numbers = {{Stergioulas, Nikolaos/0000-0002-5490-5302}}, Unique-ID = {{ISI:000297045700063}}, } @article{ ISI:000295124300017, Author = {Abernathy, M. R. and Reid, S. and Chalkley, E. and Bassiri, R. and Martin, I. W. and Evans, K. and Fejer, M. M. and Gretarsson, A. and Harry, G. M. and Hough, J. and MacLaren, I. and Markosyan, A. and Murray, P. and Nawrodt, R. and Penn, S. and Route, R. and Rowan, S. and Seidel, P.}, Title = {{Cryogenic mechanical loss measurements of heat-treated hafnium dioxide}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2011}}, Volume = {{28}}, Number = {{19}}, Month = {{OCT 7}}, Abstract = {{Low mechanical loss, high index-of-refraction thin-film coating materials are of particular interest to the gravitational wave detection community, where reduced mirror coating thermal noise in gravitational wave detectors is desirable. Current studies are focused on understanding the loss of amorphous metal oxides such as SiO(2), Ta(2)O(5) and HfO(2). Here, we report recent measurements of the temperature dependence of the mechanical loss of ion-beam sputtered hafnium dioxide (HfO(2)) coatings that have undergone heat treatment. The results indicate that, even when partially crystallized, these coatings have lower loss than amorphous Ta(2)O(5) films below similar to 100 K and that their loss exhibits some features which are heat-treatment dependent in the temperature range of similar to 100-200 K, with higher heat treatment yielding lower mechanical loss. The potential for using silica doping of hafnia coatings to prevent crystallization is discussed.}}, DOI = {{10.1088/0264-9381/28/19/195017}}, Article-Number = {{195017}}, ISSN = {{0264-9381}}, ResearcherID-Numbers = {{Abernathy, Matthew/G-1113-2011 Martin, Iain/A-2445-2010 Fejer, Martin/AAH-3883-2020 MacLaren, Ian/C-1773-2010 Martin, Iain/V-1198-2018 }}, ORCID-Numbers = {{MacLaren, Ian/0000-0002-5334-3010 Martin, Iain/0000-0001-7300-9151 Bassiri, Riccardo/0000-0001-8171-6833}}, Unique-ID = {{ISI:000295124300017}}, } @article{ ISI:000296523900005, Author = {Rosado, Pablo A.}, Title = {{Gravitational wave background from binary systems}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{84}}, Number = {{8}}, Month = {{OCT 3}}, Abstract = {{Basic aspects of the background of gravitational waves and its mathematical characterization are reviewed. The spectral energy density parameter Omega(f), commonly used as a quantifier of the background, is derived for an ensemble of many identical sources emitting at different times and locations. For such an ensemble, Omega(f) is generalized to account for the duration of the signals and of the observation, so that one can distinguish the resolvable and unresolvable parts of the background. The unresolvable part, often called confusion noise or stochastic background, is made by signals that cannot be either individually identified or subtracted out of the data. To account for the resolvability of the background, the overlap function is introduced. This function is a generalization of the duty cycle, which has been commonly used in the literature, in some cases leading to incorrect results. The spectra produced by binary systems (stellar binaries and massive black hole binaries) are presented over the frequencies of all existing and planned detectors. A semi-analytical formula for Omega(f) is derived in the case of stellar binaries (containing white dwarfs, neutron stars or stellar-mass black holes). Besides a realistic expectation of the level of background, upper and lower limits are given, to account for the uncertainties in some astrophysical parameters such as binary coalescence rates. One interesting result concerns all current and planned ground-based detectors (including the Einstein Telescope). In their frequency range, the background of binaries is resolvable and only sporadically present. In other words, there is no stochastic background of binaries for ground-based detectors.}}, DOI = {{10.1103/PhysRevD.84.084004}}, Article-Number = {{084004}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000296523900005}}, } @article{ ISI:000295044600011, Author = {Thuering, Andre and Schnabel, Roman}, Title = {{Critical Kerr nonlinear optical cavity in the presence of internal loss and driving noise}}, Journal = {{PHYSICAL REVIEW A}}, Year = {{2011}}, Volume = {{84}}, Number = {{3}}, Month = {{SEP 20}}, Abstract = {{We theoretically analyze the noise transformation of a high-power continuous-wave light field that is reflected off a critical Kerr nonlinear cavity (KNLC). Our investigations are based on a rigorous treatment in the time domain. Thereby, realistic conditions of a specific experimental environment including optical intracavity loss and strong classical driving noise can be modeled for any KNLC. We show that, even in the presence of optical loss and driving noise, considerable squeezing levels can be achieved. We find that the achievable squeezing levels are not limited by the driving noise but solely by the amount of optical loss. Amplitude-quadrature squeezing of the reflected mean field is obtained if the KNLC's operating point is chosen properly. Consistently, a KNLC can provide a passive purely optical reduction of laser-power noise as experimentally demonstrated in Khalaidovski et al. {[}Phys. Rev. A 80, 053801 (2009)]. We apply our model to this experiment and find good agreement with measured noise spectra.}}, DOI = {{10.1103/PhysRevA.84.033839}}, Article-Number = {{033839}}, ISSN = {{1050-2947}}, EISSN = {{1094-1622}}, ResearcherID-Numbers = {{Schnabel, Roman/V-7759-2019}}, Unique-ID = {{ISI:000295044600011}}, } @article{ ISI:000293756300067, Author = {Pitkin, Matthew}, Title = {{Prospects of observing continuous gravitational waves from known pulsars}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2011}}, Volume = {{415}}, Number = {{2}}, Pages = {{1849-1863}}, Month = {{AUG}}, Abstract = {{Several past searches for gravitational waves from a selection of known pulsars have been performed with data from the science runs of the Laser Interferometer Gravitational-Wave Observatory (LIGO) gravitational wave detectors. So far these have led to no detection, but upper limits on the gravitational wave amplitudes have been set. Here we study our intrinsic ability to detect, and estimate the gravitational wave amplitude for non-accreting pulsars. Using spin-down limits on emission as a guide we examine amplitudes that would be required to observe known pulsars with future detectors (Advanced LIGO, Advanced Virgo and the Einstein Telescope), assuming that they are triaxial stars emitting at precisely twice the known rotation frequency. Maximum allowed amplitudes depend on the stars' equation of state (e. g. a normal neutron star, a quark star, a hybrid star) and the theoretical mass quadrupoles that they can sustain. We study what range of quadrupoles, and therefore equation of state (EoS), would be consistent with being able to detect these sources. For globular cluster pulsars, with spin-downs masked by accelerations within the cluster, we examine what spin-down values gravitational wave observations would be able to set. For all pulsars we also alternatively examine what internal magnetic fields they would need to sustain observable ellipticities.}}, DOI = {{10.1111/j.1365-2966.2011.18818.x}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Pitkin, Matthew/I-3802-2013}}, ORCID-Numbers = {{Pitkin, Matthew/0000-0003-4548-526X}}, Unique-ID = {{ISI:000293756300067}}, } @article{ ISI:000291789300005, Author = {Falferi, Paolo}, Title = {{Testing the intrinsic noise of a coil-magnet actuator for cryogenic gravitational wave interferometers}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2011}}, Volume = {{28}}, Number = {{14}}, Month = {{JUL 21}}, Abstract = {{The third generation gravitational wave interferometers that will operate underground and at cryogenic temperatures will need a complex and sophisticated control system to satisfy the requirements on the alignment and position of its optics and keep the detector at its working point. The force actuators of the control systems of the present interferometers are for the most part coil-magnet actuators. To check the possibility of using these actuators also at low temperature we have tested the magnetization and the magnetization noise of an SmCo magnet at 4.2 K. The magnetization loss, measured with a fluxgate magnetometer, is 7\%. The magnetization noise has been measured with a superconducting quantum interference device magnetometer. The application of dc and ac (0.1 Hz) magnetic fields of an amplitude comparable to that needed to produce on the magnet a force large enough for the control system does not change the measured noise. The equivalent maximum force noise produced by the actuator as a result of the magnetization noise of the magnet has been evaluated. Its effect on the sensitivity of a third generation interferometer (Einstein Telescope) is negligible with respect to the most relevant fundamental noise contributions.}}, DOI = {{10.1088/0264-9381/28/14/145005}}, Article-Number = {{145005}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Falferi, Paolo/C-3439-2015}}, ORCID-Numbers = {{Falferi, Paolo/0000-0002-1929-4710}}, Unique-ID = {{ISI:000291789300005}}, } @article{ ISI:000292104500004, Author = {King, Ritchie S.}, Title = {{The Einstein Telescope}}, Journal = {{IEEE SPECTRUM}}, Year = {{2011}}, Volume = {{48}}, Number = {{7}}, Pages = {{14}}, Month = {{JUL}}, ISSN = {{0018-9235}}, Unique-ID = {{ISI:000292104500004}}, } @article{ ISI:000291620500012, Author = {Banks, Michael}, Title = {{Plans for Einstein Telescope unveiled}}, Journal = {{PHYSICS WORLD}}, Year = {{2011}}, Volume = {{24}}, Number = {{6}}, Pages = {{13}}, Month = {{JUN}}, ISSN = {{0953-8585}}, Unique-ID = {{ISI:000291620500012}}, } @article{ ISI:000289677700014, Author = {Hild, S. and Abernathy, M. and Acernese, F. and Amaro-Seoane, P. and Andersson, N. and Arun, K. and Barone, F. and Barr, B. and Barsuglia, M. and Beker, M. and Beveridge, N. and Birindelli, S. and Bose, S. and Bosi, L. and Braccini, S. and Bradaschia, C. and Bulik, T. and Calloni, E. and Cella, G. and Mottin, E. Chassande and Chelkowski, S. and Chincarini, A. and Clark, J. and Coccia, E. and Colacino, C. and Colas, J. and Cumming, A. and Cunningham, L. and Cuoco, E. and Danilishin, S. and Danzmann, K. and De Salvo, R. and Dent, T. and De Rosa, R. and Di Fiore, L. and Di Virgilio, A. and Doets, M. and Fafone, V. and Falferi, P. and Flaminio, R. and Franc, J. and Frasconi, F. and Freise, A. and Friedrich, D. and Fulda, P. and Gair, J. and Gemme, G. and Genin, E. and Gennai, A. and Giazotto, A. and Glampedakis, K. and Graef, C. and Granata, M. and Grote, H. and Guidi, G. and Gurkovsky, A. and Hammond, G. and Hannam, M. and Harms, J. and Heinert, D. and Hendry, M. and Heng, I. and Hennes, E. and Hough, J. and Husa, S. and Huttner, S. and Jones, G. and Khalili, F. and Kokeyama, K. and Kokkotas, K. and Krishnan, B. and Li, T. G. F. and Lorenzini, M. and Lueck, H. and Majorana, E. and Mandel, I. and Mandic, V. and Mantovani, M. and Martin, I. and Michel, C. and Minenkov, Y. and Morgado, N. and Mosca, S. and Mours, B. and Mueller-Ebhardt, H. and Murray, P. and Nawrodt, R. and Nelson, J. and Oshaughnessy, R. and Ott, C. D. and Palomba, C. and Paoli, A. and Parguez, G. and Pasqualetti, A. and Passaquieti, R. and Passuello, D. and Pinard, L. and Plastino, W. and Poggiani, R. and Popolizio, P. and Prato, M. and Punturo, M. and Puppo, P. and Rabeling, D. and Rapagnani, P. and Read, J. and Regimbau, T. and Rehbein, H. and Reid, S. and Ricci, F. and Richard, F. and Rocchi, A. and Rowan, S. and Ruediger, A. and Santamaria, L. and Sassolas, B. and Sathyaprakash, B. and Schnabel, R. and Schwarz, C. and Seidel, P. and Sintes, A. and Somiya, K. and Speirits, F. and Strain, K. and Strigin, S. and Sutton, P. and Tarabrin, S. and Thuering, A. and van den Brand, J. and van Veggel, M. and van den Broeck, C. and Vecchio, A. and Veitch, J. and Vetrano, F. and Vicere, A. and Vyatchanin, S. and Willke, B. and Woan, G. and Yamamoto, K.}, Title = {{Sensitivity studies for third-generation gravitational wave observatories}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2011}}, Volume = {{28}}, Number = {{9}}, Month = {{MAY 7}}, Note = {{8th International Laser Interferometric Space Antenna (LISA) Symposium, Stanford, CA, JUN 28-JUL 02, 2010}}, Abstract = {{Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.}}, DOI = {{10.1088/0264-9381/28/9/094013}}, Article-Number = {{094013}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Frasconi, Franco/K-1068-2016 Freise, Andreas/F-8892-2011 Acernese, Fausto/E-4989-2010 Bulik, Tomasz/AAJ-6742-2020 Prato, Mirko/D-8531-2012 di virgilio, angela/E-9078-2015 Vicere', Andrea/J-1742-2012 Cella, Giancarlo/A-9946-2012 Puppo, Paola/J-4250-2012 Husa, Sascha/AAB-6992-2019 Vecchio, Alberto/F-8310-2015 Vyatchanin, Sergey P/J-2238-2012 Somiya, Kentaro/ABE-2215-2020 Santamaria, Lucia/A-7269-2012 Willke, Benno/U-8992-2017 Hild, Stefan/A-3864-2010 Ott, Christian/G-2651-2011 Santamaria, Lucia/G-1297-2017 Martin, Iain/A-2445-2010 Van Den Broeck, Chris/R-7871-2018 Harms, Jan/O-7967-2019 Seoane, Pau Amaro/U-8229-2017 Danilishin, Stefan/K-7262-2012 Harms, Jan/J-4359-2012 Barr, Bryan/G-3348-2019 Acernese, Fausto/AAX-5705-2020 Graef, Christian/J-3167-2015 Falferi, Paolo/C-3439-2015 O'Shaughnessy, Richard/AAA-3625-2021 Rapagnani, Piero/J-4783-2012 di virgilio, angela/AAA-4814-2019 Hammond, Giles/A-8168-2012 calloni, enrico/K-5852-2019 Gemme, Gianluca/C-7233-2008 Poggiani, Rosa/P-8801-2018 Schnabel, Roman/V-7759-2019 Cuoco, Elena Dr./I-8789-2012 Kokkotas, Kostas D/B-7878-2010 Lueck, Harald/F-7100-2011 Dent, Thomas/AAB-3674-2019 Rocchi, Alessio/O-9499-2015 Prato, Mirko/AAD-9075-2019 Abernathy, Matthew/G-1113-2011 Chincarini, Andrea/J-9998-2018 Sintes, Alicia M/AAF-4791-2019 Rapagnani, Piero/T-2050-2019 mosca, simona/I-7116-2012 Punturo, Michele/I-3995-2012 Lorenzini, Matteo/AAC-6035-2021 Khalili, Farit Ya/D-8113-2012 Cuoco, Elena/O-4680-2019 Strigin, Sergey E/I-8337-2012 Martin, Iain/V-1198-2018 Passaquieti, Roberto/U-3083-2017 Sathyaprakash, Bangalore/M-1235-2014 Strain, Kenneth/D-5236-2011 }}, ORCID-Numbers = {{Frasconi, Franco/0000-0003-4204-6587 Acernese, Fausto/0000-0003-3103-3473 Prato, Mirko/0000-0002-2188-8059 di virgilio, angela/0000-0002-2237-7533 Vicere', Andrea/0000-0003-0624-6231 Cella, Giancarlo/0000-0002-0752-0338 Puppo, Paola/0000-0003-4677-5015 Husa, Sascha/0000-0002-0445-1971 Vecchio, Alberto/0000-0002-6254-1617 Somiya, Kentaro/0000-0003-2601-2264 Willke, Benno/0000-0003-0524-2925 Hild, Stefan/0000-0001-9221-6009 Ott, Christian/0000-0003-4993-2055 Santamaria, Lucia/0000-0002-5986-0449 Van Den Broeck, Chris/0000-0001-6800-4006 Harms, Jan/0000-0002-7332-9806 Danilishin, Stefan/0000-0001-7758-7493 Harms, Jan/0000-0002-7332-9806 Barr, Bryan/0000-0002-5232-2736 Acernese, Fausto/0000-0003-3103-3473 Graef, Christian/0000-0002-4535-2603 Falferi, Paolo/0000-0002-1929-4710 O'Shaughnessy, Richard/0000-0001-5832-8517 Rapagnani, Piero/0000-0002-1865-6126 Gemme, Gianluca/0000-0002-1127-7406 Cuoco, Elena Dr./0000-0002-6528-3449 Kokkotas, Kostas D/0000-0001-6048-2919 Lueck, Harald/0000-0001-9350-4846 Rocchi, Alessio/0000-0002-1382-9016 Prato, Mirko/0000-0002-2188-8059 Rapagnani, Piero/0000-0002-1865-6126 mosca, simona/0000-0001-7869-8275 Punturo, Michele/0000-0001-8722-4485 Lorenzini, Matteo/0000-0002-2765-7905 Cuoco, Elena/0000-0002-6528-3449 Martin, Iain/0000-0001-7300-9151 Passaquieti, Roberto/0000-0003-4753-9428 Hammond, Giles/0000-0002-1414-3622 Vetrano, Flavio/0000-0002-7523-4296 Guidi, Gianluca/0000-0002-3061-9870 Mandel, Ilya/0000-0002-6134-8946 Majorana, Ettore/0000-0002-2383-3692 Chincarini, Andrea/0000-0003-4094-9942 Veitch, John/0000-0002-6508-0713 Amaro Seoane, Pau/0000-0003-3993-3249 Coccia, Eugenio/0000-0002-6669-5787 Palomba, Cristiano/0000-0002-4450-9883 mantovani, maddalena/0000-0002-4424-5726 Plastino, Wolfango/0000-0002-5737-6346 Krishnan, Badri/0000-0003-3015-234X Poggiani, Rosa/0000-0002-9968-2464 Yamamoto, Kazuhiro/0000-0001-5647-6735 Sathyaprakash, Bangalore/0000-0003-3845-7586 Speirits, Fiona/0000-0002-6460-5231 Bulik, Tomasz/0000-0003-2045-4803 Granata, Massimo/0000-0003-3275-1186 van den Brand, Johannes/0000-0003-4434-5353 Ricci, Fulvio/0000-0001-5475-4447 Freise, Andreas/0000-0001-6586-9901 Di Fiore, Luciano/0000-0001-6296-1526 Sintes, Alicia M/0000-0001-9050-7515 calloni, enrico/0000-0003-4819-3297 Woan, Graham/0000-0003-0381-0394 Barone, Fabrizio/0000-0002-8069-8490 Strain, Kenneth/0000-0002-2066-5355 Genin, Eric/0000-0001-6948-032X}}, Unique-ID = {{ISI:000289677700014}}, } @article{ ISI:000289520300001, Author = {Kashiyama, Kazumi and Ioka, Kunihito}, Title = {{Magnetar asteroseismology with long-term gravitational waves}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{83}}, Number = {{8}}, Month = {{APR 13}}, Abstract = {{Magnetic flares and induced oscillations of magnetars (supermagnetized neutron stars) are promising sources of gravitational waves (GWs). We suggest that the GW emission, if any, would last longer than the observed x-ray quasiperiodic oscillations (X-QPOs), calling for longer-term GW analyses lasting a day to months, compared to current searches' durations. Like the pulsar timing, the oscillation frequency would also evolve with time because of the decay or reconfiguration of the magnetic field, which is crucial for the GW detection. With the observed GW frequency and its time-derivatives, we can probe the interior magnetic field strength of similar to 10(16) G and its evolution to open a new GW asteroseismology with the next generation interferometers like the advanced laser interferometer gravitational wave observatory, the advanced Virgo gravitational wave detector at the European Gravitational Observatory, the Large-scale cryogenic gravitational wave telescope, and the Einstein telescope.}}, DOI = {{10.1103/PhysRevD.83.081302}}, Article-Number = {{081302}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Kashiyama, Kazumi/AAW-2077-2020 }}, ORCID-Numbers = {{Kashiyama, Kazumi/0000-0003-4299-8799 Ioka, Kunihito/0000-0002-3517-1956}}, Unique-ID = {{ISI:000289520300001}}, } @article{ ISI:000287484100085, Author = {Kowalska, I. and Bulik, T. and Belczynski, K. and Dominik, M. and Gondek-Rosinska, D.}, Title = {{The eccentricity distribution of compact binaries}}, Journal = {{ASTRONOMY \& ASTROPHYSICS}}, Year = {{2011}}, Volume = {{527}}, Month = {{MAR}}, Abstract = {{Context. The current gravitational wave detectors have reached their operational sensitivity and are nearing detection of compact object binaries. In the coming years, we expect that the Advanced LIGO/VIRGO will start taking data. At the same time, there are plans for third generation ground-based detectors such as the Einstein Telescope, and space detectors such as DECIGO. Aims. We discuss the eccentricity distribution of inspiral compact object binaries during they inspiral phase. We analyze the expected distributions of eccentricities at three frequencies that are characteristic of three future detectors: Advanced LIGO/VIRGO (30 Hz), Einstein Telescope (3 Hz), and DECIGO (0.3 Hz). Methods. We use the StarTrack binary population code to investigate the properties of the population of compact binaries in formation. We evolve their orbits until the point that they enter a given detector sensitivity window and analyze the eccentricity distribution at that time. Results. We find that the eccentricities of BH-BH and BH-NS binaries are quite small when entering the Advanced LIGO/VIRGO detector window for all considered models of binary evolution. Even in the case of the DECIGO detector, the typical eccentricities of BH-BH binaries are below 10(-4), and the BH-NS eccentricities are smaller than 10(-3). Some fraction of NS-NS binaries may have significant eccentricities. Within the range of considered models, we found that a fraction of between 0.2\% and 2\% NS-NS binaries will have an eccentricity above 0.01 for the Advanced LIGO/VIRGO detectors. For the ET detector, this fraction is between 0.4\% and 4\%, and for the DECIGO detector it lies between 2\% and 27\%.}}, DOI = {{10.1051/0004-6361/201015777}}, Article-Number = {{A70}}, ISSN = {{0004-6361}}, EISSN = {{1432-0746}}, ResearcherID-Numbers = {{Bulik, Tomasz/AAJ-6742-2020 }}, ORCID-Numbers = {{Rosinska, Dorota/0000-0002-3681-9304 Kowalska-Leszczynska, Izabela/0000-0002-6569-3800 Bulik, Tomasz/0000-0003-2045-4803}}, Unique-ID = {{ISI:000287484100085}}, } @article{ ISI:000287859200026, Author = {Marassi, Stefania and Ciolfi, Riccardo and Schneider, Raffaella and Stella, Luigi and Ferrari, Valeria}, Title = {{Stochastic background of gravitational waves emitted by magnetars}}, Journal = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}}, Year = {{2011}}, Volume = {{411}}, Number = {{4}}, Pages = {{2549-2557}}, Month = {{MAR}}, Abstract = {{Two classes of high-energy sources in our galaxy are believed to host magnetars, i.e. neutron stars whose emission results from the dissipation of their magnetic field. The extremely high magnetic field of magnetars distorts their shape, and causes the emission of a conspicuous gravitational wave signal if rotation is fast and takes place around a different axis than the symmetry axis of the magnetic distortion. Based on a numerical model of the cosmic star formation history, we derive the cosmological background of gravitational waves produced by magnetars, when they are very young and fast spinning. We adopt different models for the configuration and strength of the internal magnetic field (which determines the distortion) as well as different values of the external dipole field strength (which governs the spin evolution of magnetars over a wide range of parameters). We find that the expected gravitational wave background differs considerably from one model to another. The strongest signals are generated for magnetars with very intense toroidal internal fields (similar to 10(16) G range) and external dipole fields of similar to 10(14), as envisaged in models aimed at explaining the properties of the 2004 December giant flare from SGR 1806-20. Such signals should be easily detectable with third-generation ground-based interferometers such as the Einstein Telescope.}}, DOI = {{10.1111/j.1365-2966.2010.17861.x}}, ISSN = {{0035-8711}}, EISSN = {{1365-2966}}, ResearcherID-Numbers = {{Schneider, Raffaella/E-4216-2017 Ciolfi, Riccardo/P-4462-2016 }}, ORCID-Numbers = {{Schneider, Raffaella/0000-0001-9317-2888 Ciolfi, Riccardo/0000-0003-3140-8933 Marassi, Stefania/0000-0001-9018-4867 Stella, Luigi/0000-0002-0018-1687}}, Unique-ID = {{ISI:000287859200026}}, } @article{ ISI:000287194900002, Author = {Huerta, E. A. and Gair, Jonathan R.}, Title = {{Intermediate-mass-ratio inspirals in the Einstein Telescope. II. Parameter estimation errors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{83}}, Number = {{4}}, Month = {{FEB 10}}, Abstract = {{We explore the precision with which the Einstein Telescope will be able to measure the parameters of intermediate-mass-ratio inspirals, i.e., the inspirals of stellar mass compact objects into intermediate-mass black holes (IMBHs). We calculate the parameter estimation errors using the Fisher Matrix formalism and present results of Monte Carlo simulations of these errors over choices for the extrinsic parameters of the source. These results are obtained using two different models for the gravitational waveform which were introduced in paper I of this series. These two waveform models include the inspiral, merger, and ringdown phases in a consistent way. One of the models, based on the transition scheme of Ori and Thorne {[}A. Ori and K. S. Thorne, Phys. Rev. D 62, 124022 (2000).], is valid for IMBHs of arbitrary spin; whereas, the second model, based on the effective-one-body approach, has been developed to cross-check our results in the nonspinning limit. In paper I of this series, we demonstrated the excellent agreement in both phase and amplitude between these two models for nonspinning black holes, and that their predictions for signal-to-noise ratios are consistent to within 10\%. We now use these waveform models to estimate parameter estimation errors for binary systems with masses 1: 4M(circle dot) + 100M(circle dot), 10M(circle dot) + 100M(circle dot), 1.4M(circle dot) + 500M(circle dot), and 10M(circle dot) + 500M(circle dot) and various choices for the spin of the central IMBH. Assuming a detector network of three Einstein Telescopes, the analysis shows that for a 10M(circle dot) compact object inspiralling into a 100M(circle dot) IMBH with spin q = 0.3, detected with a signal-to-noise ratio of 30, we should be able to determine the compact object and IMBH masses, and the IMBH spin magnitude to fractional accuracies of similar to 10(-3), similar to 10(-3.5), and similar to 10(-3), respectively. We also expect to determine the location of the source in the sky and the luminosity distance to within similar to 0.003 steradians and similar to 10\%, respectively. We also compute results for several different possible configurations of the detector network to assess how the precision of parameter determination depends on the network configuration.}}, DOI = {{10.1103/PhysRevD.83.044021}}, Article-Number = {{044021}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Huerta, Eliu/J-5426-2014}}, Unique-ID = {{ISI:000287194900002}}, } @article{ ISI:000287194900001, Author = {Huerta, E. A. and Gair, Jonathan R.}, Title = {{Intermediate-mass-ratio inspirals in the Einstein Telescope. I. Signal-to-noise ratio calculations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{83}}, Number = {{4}}, Month = {{FEB 10}}, Abstract = {{The Einstein Telescope (ET) is a proposed third-generation ground-based interferometric gravitational wave detector, for which the target is a sensitivity that is a factor of 10 better than Advanced LIGO and a frequency range that extends down to similar to 1 Hz. Such a third-generation interferometer will provide opportunities to test Einstein's theory of relativity in the strong field and will realize precision gravitational wave astronomy with a thousandfold increase in the expected number of events over the advanced ground-based detectors. A design study for ET is currently underway, so it is timely to assess the science that could be done with such an instrument. This paper is the first in a series that will carry out a detailed study of intermediate-mass-ratio inspirals (IMRIs) for ET. In the context of ET, an IMRI is the inspiral of a neutron star or stellar-mass black hole into an intermediate mass black hole (IMBH). In this paper we focus on the development of IMRI waveform models for circular and equatorial inspirals. We consider two approximations for the waveforms, which both incorporate the inspiral, merger, and ringdown phases in a consistent way. One approximation, valid for IMBHs of arbitrary spin, uses the transition model of Ori and Thorne {[}A. Ori and K. S. Thorne, Phys. Rev. D 62, 124022 (2000).] to describe the merger, and this is then matched smoothly onto a ringdown waveform. The second approximation uses the effective one body approach to model the merger phase of the waveform and is valid for nonspinning IMBHs. In this paper, we use both waveform models to compute signal-to-noise ratios for IMRI sources detectable by ET. At a redshift of z = 1, we find typical signal-to-noise ratios for IMRI systems with masses 1: 4M(circle dot) + 100M(circle dot), 10M(circle dot) + 100M(circle dot), 1.4M(circle dot) + 500M(circle dot) and 10M(circle dot) + 500M(circle dot) of similar to 10-25, similar to 40-80, similar to 3-15, and similar to 10-60, respectively. We also find that the two models make predictions for nonspinning inspirals that are consistent to about 10\%.}}, DOI = {{10.1103/PhysRevD.83.044020}}, Article-Number = {{044020}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Huerta, Eliu/J-5426-2014 }}, ORCID-Numbers = {{Huerta, Eliu/0000-0002-9682-3604}}, Unique-ID = {{ISI:000287194900001}}, } @article{ ISI:000286984900002, Author = {Giacomazzo, Bruno and Rezzolla, Luciano and Baiotti, Luca}, Title = {{Accurate evolutions of inspiralling and magnetized neutron stars: Equal-mass binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{83}}, Number = {{4}}, Month = {{FEB 4}}, Abstract = {{By performing new, long and numerically accurate general-relativistic simulations of magnetized, equal-mass neutron-star binaries, we investigate the role that realistic magnetic fields may have in the evolution of these systems. In particular, we study the evolution of the magnetic fields and show that they can influence the survival of the hypermassive neutron star produced at the merger by accelerating its collapse to a black hole. We also provide evidence that, even if purely poloidal initially, the magnetic fields produced in the tori surrounding the black hole have toroidal and poloidal components of equivalent strength. When estimating the possibility that magnetic fields could have an impact on the gravitational-wave signals emitted by these systems either during the inspiral or after the merger, we conclude that for realistic magnetic-field strengths B <= 10(12) G such effects could be detected, but only marginally, by detectors such as advanced LIGO or advanced Virgo. However, magnetically induced modifications could become detectable in the case of small-mass binaries and with the development of gravitational-wave detectors, such as the Einstein Telescope, with much higher sensitivities at frequencies larger than approximate to 2 kHz.}}, DOI = {{10.1103/PhysRevD.83.044014}}, Article-Number = {{044014}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Giacomazzo, Bruno/I-8088-2012 Baiotti, Luca/N-1791-2019}}, ORCID-Numbers = {{Giacomazzo, Bruno/0000-0002-6947-4023 }}, Unique-ID = {{ISI:000286984900002}}, } @article{ ISI:000286619500013, Author = {Puppo, Paola and Ricci, Fulvio}, Title = {{Cryogenics and Einstein Telescope}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{657-669}}, Month = {{FEB}}, Abstract = {{The dominant noises which limit the present sensitivity of the gravitational wave detectors are the thermal noise of the suspended mirrors and the shot noise. For the third generation of gravitational wave detectors as the Einstein Telescope (ET), the reduction of the shot noise implies to increase the power stored in the detector at 1 MW level and, at the same time, to compensate the huge optic distortion due to induced thermal lensing. At low temperature it is possible to reduce both these effects. However, lowering the temperature of the test masses without injecting vibration noise from the cooling system is a technological challenge. We review here the thermal noise impact on the ultimate ET sensitivity limit and we discuss possible cryogenic configurations to cool the mirror.}}, DOI = {{10.1007/s10714-010-1037-x}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ResearcherID-Numbers = {{Puppo, Paola/J-4250-2012 }}, ORCID-Numbers = {{Puppo, Paola/0000-0003-4677-5015 Ricci, Fulvio/0000-0001-5475-4447}}, Unique-ID = {{ISI:000286619500013}}, } @article{ ISI:000286619500008, Author = {Bosi, Leone and Porter, Edward K.}, Title = {{Data analysis challenges for the Einstein Telescope}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{519-535}}, Month = {{FEB}}, Abstract = {{The Einstein Telescope is a proposed third generation gravitational wave detector that will operate in the region of 1 Hz to a few kHz. As well as the inspiral of compact binaries composed of neutron stars or black holes, the lower frequency cut-off of the detector will open the window to a number of new sources. These will include the end stage of inspirals, plus merger and ringdown of intermediate mass black holes, where the masses of the component bodies are on the order of a few hundred solar masses. There is also the possibility of observing intermediate mass ratio inspirals, where a stellar mass compact object inspirals into a black hole which is a few hundred to a few thousand times more massive. In this article, we investigate some of the data analysis challenges for the Einstein Telescope such as the effects of increased source number, the need for more accurate waveform models and the some of the computational issues that a data analysis strategy might face.}}, DOI = {{10.1007/s10714-010-1084-3}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, Unique-ID = {{ISI:000286619500008}}, } @article{ ISI:000286619500002, Author = {Punturo, Michele and Lueck, Harald}, Title = {{Toward a third generation of gravitational wave observatories}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{363-385}}, Month = {{FEB}}, Abstract = {{Large gravitational wave interferometric detectors, like Virgo and LIGO, demonstrated the capability to reach their design sensitivity, but to transform these machines into an effective observational instrument for gravitational wave astronomy a large improvement in sensitivity is required. Advanced detectors in the near future and third generation observatories in slightly more than one decade will open the possibility to perform gravitational wave astronomical observations from the Earth. An overview of the technological progress needed to realize a third generation observatory, like the Einstein Telescope (ET), and a possible evolution scenario are discussed in this paper.}}, DOI = {{10.1007/s10714-010-1010-8}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ResearcherID-Numbers = {{Punturo, Michele/I-3995-2012 Lueck, Harald/F-7100-2011}}, ORCID-Numbers = {{Punturo, Michele/0000-0001-8722-4485 Lueck, Harald/0000-0001-9350-4846}}, Unique-ID = {{ISI:000286619500002}}, } @article{ ISI:000286619500004, Author = {Andersson, N. and Ferrari, V. and Jones, D. I. and Kokkotas, K. D. and Krishnan, B. and Read, J. S. and Rezzolla, L. and Zink, B.}, Title = {{Gravitational waves from neutron stars: promises and challenges}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{409-436}}, Month = {{FEB}}, Abstract = {{We discuss different ways that neutron stars can generate gravitational waves, describe recent improvements in modelling the relevant scenarios in the context of improving detector sensitivity, and show how observations are beginning to test our understanding of fundamental physics. The main purpose of the discussion is to establish promising science goals for third-generation ground-based detectors, like the Einstein Telescope, and identify the various challenges that need to be met if we want to use gravitational-wave data to probe neutron star physics.}}, DOI = {{10.1007/s10714-010-1059-4}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ResearcherID-Numbers = {{Kokkotas, Kostas D/B-7878-2010 }}, ORCID-Numbers = {{Kokkotas, Kostas D/0000-0001-6048-2919 Read, Jocelyn/0000-0002-3923-1055 Krishnan, Badri/0000-0003-3015-234X Jones, David/0000-0002-0117-7567 Andersson, Nils/0000-0001-8550-3843}}, Unique-ID = {{ISI:000286619500004}}, } @article{ ISI:000286619500005, Author = {Chassande-Mottin, Eric and Hendry, Martin and Sutton, Patrick J. and Marka, Szabolcs}, Title = {{Multimessenger astronomy with the Einstein Telescope}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{437-464}}, Month = {{FEB}}, Abstract = {{Gravitational waves (GWs) are expected to play a crucial role in the development of multimessenger astrophysics. The combination of GW observations with other astrophysical triggers, such as from gamma-ray and X-ray satellites, optical/radio telescopes, and neutrino detectors allows us to decipher science that would otherwise be inaccessible. In this paper, we provide a broad review from the multimessenger perspective of the science reach offered by the third generation interferometric GW detectors and by the Einstein Telescope (ET) in particular. We focus on cosmic transients, and base our estimates on the results obtained by ET's predecessors GEO, LIGO, and Virgo.}}, DOI = {{10.1007/s10714-010-1019-z}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ResearcherID-Numbers = {{CHASSANDE-MOTTIN, Eric/ABC-2478-2020}}, ORCID-Numbers = {{CHASSANDE-MOTTIN, Eric/0000-0003-3768-9908}}, Unique-ID = {{ISI:000286619500005}}, } @article{ ISI:000286619500006, Author = {Hannam, Mark and Hawke, Ian}, Title = {{Numerical relativity simulations in the era of the Einstein Telescope}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{465-483}}, Month = {{FEB}}, Abstract = {{Numerical-relativity (NR) simulations of compact binaries are expected to be an invaluable tool in gravitational-wave astronomy. The sensitivity of future detectors such as the Einstein Telescope (ET) will place much higher demands on NR simulations than first- and second-generation ground-based detectors. We discuss the issues facing compact-object simulations over the next decade, with an emphasis on estimating where the accuracy and parameter space coverage will be sufficient for ET and where significant work is needed.}}, DOI = {{10.1007/s10714-010-1008-2}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ORCID-Numbers = {{Hawke, Ian/0000-0003-4805-0309}}, Unique-ID = {{ISI:000286619500006}}, } @article{ ISI:000286619500007, Author = {Gair, Jonathan R. and Mandel, Ilya and Miller, M. Coleman and Volonteri, Marta}, Title = {{Exploring intermediate and massive black-hole binaries with the Einstein Telescope}}, Journal = {{GENERAL RELATIVITY AND GRAVITATION}}, Year = {{2011}}, Volume = {{43}}, Number = {{2}}, Pages = {{485-518}}, Month = {{FEB}}, Abstract = {{We discuss the capability of a third-generation ground-based detector such as the Einstein Telescope (ET) to enhance our astrophysical knowledge through detections of gravitational waves emitted by binaries including intermediate-mass and massive black holes. The design target for such instruments calls for improved sensitivity at low frequencies, specifically in the similar to 1-10 Hz range. This will allow the detection of gravitational waves generated in binary systems containing black holes of intermediate mass, similar to 100-10000 M-circle dot. We primarily discuss two different source types-mergers between two intermediate mass black holes (IMBHs) of comparable mass, and intermediate-mass-ratio inspirals (IMRIs) of smaller compact objects with mass similar to 1-10 M-circle dot into IMBHs. IMBHs may form via two channels: (i) in dark matter halos at high redshift through direct collapse or the collapse of very massive metal-poor Population III stars, or (ii) via runaway stellar collisions in globular clusters. In this paper, we will discuss both formation channels, and both classes of merger in each case. We review existing rate estimates where these exist in the literature, and provide some new calculations for the approximate numbers of events that will be seen by a detector like the Einstein Telescope. These results indicate that the ET may see a few to a few thousand comparable-mass IMBH mergers and as many as several hundred IMRI events per year. These observations will significantly enhance our understanding of galactic black-hole growth, of the existence and properties of IMBHs and of the astrophysics of globular clusters. We finish our review with a discussion of some more speculative sources of gravitational waves for the ET, including hypermassive white dwarfs and eccentric stellar-mass compact-object binaries.}}, DOI = {{10.1007/s10714-010-1104-3}}, ISSN = {{0001-7701}}, EISSN = {{1572-9532}}, ORCID-Numbers = {{Mandel, Ilya/0000-0002-6134-8946 Miller, Cole/0000-0002-2666-728X}}, Unique-ID = {{ISI:000286619500007}}, } @article{ ISI:000286772800001, Author = {Zhao, W. and Van den Broeck, C. and Baskaran, D. and Li, T. G. F.}, Title = {{Determination of dark energy by the Einstein Telescope: Comparing with CMB, BAO, and SNIa observations}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2011}}, Volume = {{83}}, Number = {{2}}, Month = {{JAN 11}}, Abstract = {{A design study is currently in progress for a third-generation gravitational-wave (GW) detector called the Einstein Telescope (ET). An important kind of source for ET will be the inspiral and merger of binary neutron stars up to z similar to 2. If binary neutron star mergers are the progenitors of short-hard gamma -ray bursts, then some fraction of them will be seen both electromagnetically and through GW, so that the luminosity distance and the redshift of the source can be determined separately. An important property of these ``standard sirens{''} is that they are self-calibrating: the luminosity distance can be inferred directly from the GW signal, with no need for a cosmic distance ladder. Thus, standard sirens will provide a powerful independent check of the Lambda CDM model. In previous work, estimates were made of how well ET would be able to measure a subset of the cosmological parameters (such as the dark energy parameter w(0)) it will have access to, assuming that the others had been determined to great accuracy by alternative means. Here we perform a more careful analysis by explicitly using the potential Planck cosmic microwave background data as prior information for these other parameters. We find that ET will be able to constrain w(0) and w(a) with accuracies Delta w(0) = 0.099 and Delta w(a) = 0.302, respectively. These results are compared with projected accuracies for the JDEM baryon acoustic oscillations project and the SNAP type Ia supernovae observations.}}, DOI = {{10.1103/PhysRevD.83.023005}}, Article-Number = {{023005}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Van Den Broeck, Chris/R-7871-2018 }}, ORCID-Numbers = {{Van Den Broeck, Chris/0000-0001-6800-4006 Zhao, Wen/0000-0002-1330-2329}}, Unique-ID = {{ISI:000286772800001}}, } @article{ ISI:000293358600001, Author = {Pitkin, Matthew and Reid, Stuart and Rowan, Sheila and Hough, Jim}, Title = {{Gravitational Wave Detection by Interferometry (Ground and Space)}}, Journal = {{LIVING REVIEWS IN RELATIVITY}}, Year = {{2011}}, Volume = {{14}}, Abstract = {{Significant progress has been made in recent years on the development of gravitational-wave detectors. Sources such as coalescing compact binary systems, neutron stars in low-mass X-ray binaries, stellar collapses and pulsars are all possible candidates for detection. The most promising design of gravitational-wave detector uses test masses a long distance apart and freely suspended as pendulums on Earth or in drag-free spacecraft. The main theme of this review is a discussion of the mechanical and optical principles used in the various long baseline systems in operation around the world - LIGO (USA), Virgo (Italy/France), TAMA300 and LCGT (Japan), and GEO600 (Germany/U.K.) - and in LISA, a proposed space-borne interferometer. A review of recent science runs from the current generation of ground-based detectors will be discussed, in addition to highlighting the astrophysical results gained thus far. Looking to the future, the major upgrades to LIGO (Advanced LIGO), Virgo (Advanced Virgo), LCGT and GEO600 (GEO-HF) will be completed over the coming years, which will create a network of detectors with the significantly improved sensitivity required to detect gravitational waves. Beyond this, the concept and design of possible future ``third generation{''} gravitational-wave detectors, such as the Einstein Telescope (ET), will be discussed.}}, DOI = {{10.12942/lrr-2011-5}}, Article-Number = {{5}}, ISSN = {{2367-3613}}, EISSN = {{1433-8351}}, ResearcherID-Numbers = {{Pitkin, Matthew/I-3802-2013}}, ORCID-Numbers = {{Pitkin, Matthew/0000-0003-4548-526X}}, Unique-ID = {{ISI:000293358600001}}, } @article{ ISI:000208475400001, Author = {Keppel, D. and Ajith, P.}, Title = {{Constraining the mass of the graviton using coalescing black-hole binaries}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2010}}, Volume = {{82}}, Number = {{12}}, Month = {{DEC 9}}, Abstract = {{We study how well the mass of the graviton can be constrained from gravitational-wave (GW) observations of coalescing binary black holes. Whereas the previous investigations employed post-Newtonian (PN) templates describing only the inspiral part of the signal, the recent progress in analytical and numerical relativity has provided analytical waveform templates coherently describing the inspiral-merger-ringdown (IMR) signals. We show that a search for binary black holes employing IMR templates will be able to constrain the mass of the graviton much more accurately (similar to an order of magnitude) than a search employing PN templates. The best expected bound from GW observatories (lambda(g) > 7.8 x 10(13) km from Advanced LIGO, lambda(g) > 7.1 x 10(14) km from Einstein Telescope, and lambda(g) > 5.9 x 10(17) km from LISA) are several orders of magnitude better than the best available model-independent bound (lambda(g) > 2.8 x 10(12) km, from solar system tests).}}, DOI = {{10.1103/PhysRevD.82.122001}}, Article-Number = {{122001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000208475400001}}, } @article{ ISI:000284211200014, Author = {Harms, J. and Acernese, F. and Barone, F. and Bartos, I. and Beker, M. and van den Brand, J. F. J. and Christensen, N. and Coughlin, M. and DeSalvo, R. and Dorsher, S. and Heise, J. and Kandhasamy, S. and Mandic, V. and Marka, S. and Mueller, G. and Naticchioni, L. and O'Keefe, T. and Rabeling, D. S. and Sajeva, A. and Trancynger, T. and Wand, V.}, Title = {{Characterization of the seismic environment at the Sanford Underground Laboratory, South Dakota}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2010}}, Volume = {{27}}, Number = {{22}}, Month = {{NOV 21}}, Abstract = {{An array of seismometers is being developed at the Sanford Underground Laboratory, the former Homestake mine, in South Dakota to study the properties of underground seismic fields and Newtonian noise, and to investigate the possible advantages of constructing a third-generation gravitational-wave detector underground. Seismic data were analyzed to characterize seismic noise and disturbances. External databases were used to identify sources of seismic waves: ocean-wave data to identify sources of oceanic microseisms and surface wind-speed data to investigate correlations with seismic motion as a function of depth. In addition, sources of events contributing to the spectrum at higher frequencies are characterized by studying the variation of event rates over the course of a day. Long-term observations of spectral variations provide further insight into the nature of seismic sources. Seismic spectra at three different depths are compared, establishing the 4100 ft level as a world-class low seismic-noise environment.}}, DOI = {{10.1088/0264-9381/27/22/225011}}, Article-Number = {{225011}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Acernese, Fausto/AAX-5705-2020 Naticchioni, Luca/AAB-7775-2019 Bartos, Imre/A-2592-2017 Christensen, Nelson/AAH-9184-2019 Harms, Jan/J-4359-2012 Acernese, Fausto/E-4989-2010 Lueck, Harald/F-7100-2011 Harms, Jan/O-7967-2019 Bartos, Imre/AAD-6024-2019 Sajeva, Angelo/H-7303-2019 }}, ORCID-Numbers = {{Acernese, Fausto/0000-0003-3103-3473 Naticchioni, Luca/0000-0003-2918-0730 Christensen, Nelson/0000-0002-6870-4202 Harms, Jan/0000-0002-7332-9806 Acernese, Fausto/0000-0003-3103-3473 Lueck, Harald/0000-0001-9350-4846 Harms, Jan/0000-0002-7332-9806 Sajeva, Angelo/0000-0002-4772-2874 van den Brand, Johannes/0000-0003-4434-5353 O'Keefe, Thomas/0000-0003-1439-8569 Barone, Fabrizio/0000-0002-8069-8490}}, Unique-ID = {{ISI:000284211200014}}, } @article{ ISI:000284211200023, Author = {Martin, I. W. and Bassiri, R. and Nawrodt, R. and Fejer, M. M. and Gretarsson, A. and Gustafson, E. and Harry, G. and Hough, J. and MacLaren, I. and Penn, S. and Reid, S. and Route, R. and Rowan, S. and Schwarz, C. and Seidel, P. and Scott, J. and Woodcraft, A. L.}, Title = {{Effect of heat treatment on mechanical dissipation in Ta2O5 coatings}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2010}}, Volume = {{27}}, Number = {{22}}, Month = {{NOV 21}}, Abstract = {{Thermal noise arising from mechanical dissipation in dielectric reflective coatings is expected to critically limit the sensitivity of precision measurement systems such as high-resolution optical spectroscopy, optical frequency standards and future generations of interferometric gravitational wave detectors. We present measurements of the effect of post-deposition heat treatment on the temperature dependence of the mechanical dissipation in ion-beam sputtered tantalum pentoxide between 11 K and 300 K. We find that the temperature dependence of the dissipation is strongly dependent on the temperature at which the heat treatment was carried out, and we have identified three dissipation peaks occurring at different heat treatment temperatures. At temperatures below 200 K, the magnitude of the loss was found to increase with higher heat treatment temperatures, indicating that heat treatment is a significant factor in determining the level of coating thermal noise.}}, DOI = {{10.1088/0264-9381/27/22/225020}}, Article-Number = {{225020}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Martin, Iain/A-2445-2010 MacLaren, Ian/C-1773-2010 Fejer, Martin/AAH-3883-2020 Martin, Iain/V-1198-2018 }}, ORCID-Numbers = {{MacLaren, Ian/0000-0002-5334-3010 Martin, Iain/0000-0001-7300-9151 Bassiri, Riccardo/0000-0001-8171-6833 Scott, Jamie/0000-0001-6701-6515}}, Unique-ID = {{ISI:000284211200023}}, } @article{ ISI:000283059500011, Author = {Sathyaprakash, B. S. and Schutz, B. F. and Van den Broeck, C.}, Title = {{Cosmography with the Einstein Telescope}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2010}}, Volume = {{27}}, Number = {{21}}, Month = {{NOV 21}}, Abstract = {{The Einstein Telescope, a third-generation gravitational-wave detector under a design study, could detect millions of binary neutron star inspirals each year. A small fraction of these events might be observed as gamma-ray bursts, helping to measure both the luminosity distance D-L to and redshift z of the source. By fitting these measured values of D-L and z to a cosmological model, it would be possible to infer the dark energy equation of state to within 1.5\% without the need to correct for errors in D-L caused by weak lensing. This compares favourably with 0.3-10\% accuracy that can be achieved with the Laser Interferometer Space Antenna (where weak lensing will need to be dealt with) as well as with dedicated dark energy missions that have been proposed, where 3.5-11\% uncertainty is expected.}}, DOI = {{10.1088/0264-9381/27/21/215006}}, Article-Number = {{215006}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Van Den Broeck, Chris/R-7871-2018 Schutz, Bernard F/B-1504-2010 Sathyaprakash, Bangalore/M-1235-2014 }}, ORCID-Numbers = {{Van Den Broeck, Chris/0000-0001-6800-4006 Sathyaprakash, Bangalore/0000-0003-3845-7586 Schutz, Bernard/0000-0001-9487-6983}}, Unique-ID = {{ISI:000283059500011}}, } @article{ ISI:000284075400018, Author = {Amaro-Seoane, Pau and Santamaria, Lucia}, Title = {{DETECTION OF IMBHs WITH GROUND-BASED GRAVITATIONAL WAVE OBSERVATORIES: A BIOGRAPHY OF A BINARY OF BLACK HOLES, FROM BIRTH TO DEATH}}, Journal = {{ASTROPHYSICAL JOURNAL}}, Year = {{2010}}, Volume = {{722}}, Number = {{2}}, Pages = {{1197-1206}}, Month = {{OCT 20}}, Abstract = {{Even though the existence of intermediate-mass black holes (IMBHs; black holes with masses ranging between 10(2) M-circle dot and 10(4) M-circle dot) has not yet been corroborated observationally, these objects are of high interest for astrophysics. Our understanding of the formation and evolution of supermassive black holes, as well as galaxy evolution modeling and cosmography would dramatically change if an IMBH were to be observed. From the point of view of traditional photon-based astronomy, which relies on the monitoring of innermost stellar kinematics, the direct detection of an IMBH seems to be rather far in the future. However, the prospect of the detection and characterization of an IMBH has good chances in lower frequency gravitational-wave (GW) astrophysics using ground-based detectors such as the Laser Interferometer Gravitational-Wave Observatory (LIGO), Virgo, and the future Einstein Telescope (ET). We present an analysis of the signal of a system of a binary of IMBHs based on a waveform model obtained with numerical relativity simulations coupled with post-Newtonian calculations at the highest available order. IMBH binaries with total masses between 200 and 20,000 M-circle dot would produce significant signal-to-noise ratios in Advanced LIGO and Virgo and the ET. We have computed the expected event rate of IMBH binary coalescences for different configurations of the binary, finding interesting values that depend on the spin of the IMBHs. The prospects for IMBH detection and characterization with ground-based GW observatories would not only provide us with a robust test of general relativity, but would also corroborate the existence of these systems. Such detections should allow astrophysicists to probe the stellar environments of IMBHs and their formation processes.}}, DOI = {{10.1088/0004-637X/722/2/1197}}, ISSN = {{0004-637X}}, EISSN = {{1538-4357}}, ResearcherID-Numbers = {{Santamaria, Lucia/G-1297-2017 Seoane, Pau Amaro/U-8229-2017 Santamaria, Lucia/A-7269-2012 }}, ORCID-Numbers = {{Santamaria, Lucia/0000-0002-5986-0449 Amaro Seoane, Pau/0000-0003-3993-3249}}, Unique-ID = {{ISI:000284075400018}}, } @article{ ISI:000282067500003, Author = {Punturo, M. and Abernathy, M. and Acernese, F. and Allen, B. and Andersson, N. and Arun, K. and Barone, F. and Barr, B. and Barsuglia, M. and Beker, M. and Beveridge, N. and Birindelli, S. and Bose, S. and Bosi, L. and Braccini, S. and Bradaschia, C. and Bulik, T. and Calloni, E. and Cella, G. and Mottin, E. Chassande and Chelkowski, S. and Chincarini, A. and Clark, J. and Coccia, E. and Colacino, C. and Colas, J. and Cumming, A. and Cunningham, L. and Cuoco, E. and Danilishin, S. and Danzmann, K. and De Luca, G. and De Salvo, R. and Dent, T. and De Rosa, R. and Di Fiore, L. and Di Virgilio, A. and Doets, M. and Fafone, V. and Falferi, P. and Flaminio, R. and Franc, J. and Frasconi, F. and Freise, A. and Fulda, P. and Gair, J. and Gemme, G. and Gennai, A. and Giazotto, A. and Glampedakis, K. and Granata, M. and Grote, H. and Guidi, G. and Hammond, G. and Hannam, M. and Harms, J. and Heinert, D. and Hendry, M. and Heng, I. and Hennes, E. and Hild, S. and Hough, J. and Husa, S. and Huttner, S. and Jones, G. and Khalili, F. and Kokeyama, K. and Kokkotas, K. and Krishnan, B. and Lorenzini, M. and Lueck, H. and Majorana, E. and Mandel, I. and Mandic, V. and Martin, I. and Michel, C. and Minenkov, Y. and Morgado, N. and Mosca, S. and Mours, B. and Mueller-Ebhardt, H. and Murray, P. and Nawrodt, R. and Nelson, J. and Oshaughnessy, R. and Ott, C. D. and Palomba, C. and Paoli, A. and Parguez, G. and Pasqualetti, A. and Passaquieti, R. and Passuello, D. and Pinard, L. and Poggiani, R. and Popolizio, P. and Prato, M. and Puppo, P. and Rabeling, D. and Rapagnani, P. and Read, J. and Regimbau, T. and Rehbein, H. and Reid, S. and Rezzolla, L. and Ricci, F. and Richard, F. and Rocchi, A. and Rowan, S. and Ruediger, A. and Sassolas, B. and Sathyaprakash, B. and Schnabel, R. and Schwarz, C. and Seidel, P. and Sintes, A. and Somiya, K. and Speirits, F. and Strain, K. and Strigin, S. and Sutton, P. and Tarabrin, S. and Thuering, A. and van den Brand, J. and van Leewen, C. and van Veggel, M. and van den Broeck, C. and Vecchio, A. and Veitch, J. and Vetrano, F. and Vicere, A. and Vyatchanin, S. and Willke, B. and Woan, G. and Plastino, W. and Yamamoto, K.}, Title = {{The Einstein Telescope: a third-generation gravitational wave observatory}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2010}}, Volume = {{27}}, Number = {{19, SI}}, Month = {{OCT 7}}, Note = {{14th Gravitational Waves Data Analysis Workshop (GWDAW), Univ Rome Sapienza, Dept Phys, Rome, ITALY, JAN 26-29, 2010}}, Organization = {{Univ Rome Sapienza; Italian Natl Inst Nucl Phys (INFN); Italian Natl Inst Astrophys (INAF); Univ Rome Tor Vergata; Univ Sannio; E4-Comp Engn s p a}}, Abstract = {{Advanced gravitational wave interferometers, currently under realization, will soon permit the detection of gravitational waves from astronomical sources. To open the era of precision gravitational wave astronomy, a further substantial improvement in sensitivity is required. The future space-based Laser Interferometer Space Antenna and the third-generation ground-based observatory Einstein Telescope (ET) promise to achieve the required sensitivity improvements in frequency ranges. The vastly improved sensitivity of the third generation of gravitational wave observatories could permit detailed measurements of the sources' physical parameters and could complement, in a multi-messenger approach, the observation of signals emitted by cosmological sources obtained through other kinds of telescopes. This paper describes the progress of the ET project which is currently in its design study phase.}}, DOI = {{10.1088/0264-9381/27/19/194002}}, Article-Number = {{194002}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Puppo, Paola/J-4250-2012 Somiya, Kentaro/ABE-2215-2020 Vecchio, Alberto/F-8310-2015 di virgilio, angela/AAA-4814-2019 Chincarini, Andrea/J-9998-2018 Acernese, Fausto/AAX-5705-2020 Cuoco, Elena Dr./I-8789-2012 Rapagnani, Piero/T-2050-2019 calloni, enrico/K-5852-2019 Lueck, Harald/F-7100-2011 Khalili, Farit Ya/D-8113-2012 Vicere', Andrea/J-1742-2012 Strigin, Sergey E/I-8337-2012 Cuoco, Elena/O-4680-2019 Prato, Mirko/AAD-9075-2019 Gemme, Gianluca/C-7233-2008 Freise, Andreas/F-8892-2011 Willke, Benno/U-8992-2017 Danilishin, Stefan/K-7262-2012 Harms, Jan/J-4359-2012 Dent, Thomas/AAB-3674-2019 Martin, Iain/A-2445-2010 Martin, Iain/V-1198-2018 Vyatchanin, Sergey P/J-2238-2012 Lorenzini, Matteo/AAC-6035-2021 O'Shaughnessy, Richard/AAA-3625-2021 Kokkotas, Kostas D/B-7878-2010 Prato, Mirko/D-8531-2012 Poggiani, Rosa/P-8801-2018 Rocchi, Alessio/O-9499-2015 Van Den Broeck, Chris/R-7871-2018 Falferi, Paolo/C-3439-2015 Punturo, Michele/I-3995-2012 Abernathy, Matthew/G-1113-2011 Bulik, Tomasz/AAJ-6742-2020 Hammond, Giles/B-7861-2009 Acernese, Fausto/E-4989-2010 Hild, Stefan/A-3864-2010 Ott, Christian/G-2651-2011 Barr, Bryan/G-3348-2019 Sintes, Alicia M/AAF-4791-2019 mosca, simona/I-7116-2012 Harms, Jan/O-7967-2019 Rapagnani, Piero/J-4783-2012 Frasconi, Franco/K-1068-2016 Husa, Sascha/AAB-6992-2019 Hammond, Giles/A-8168-2012 Allen, Bruce/K-2327-2012 Cella, Giancarlo/A-9946-2012 di virgilio, angela/E-9078-2015 Strain, Kenneth/D-5236-2011 Sathyaprakash, Bangalore/M-1235-2014 Passaquieti, Roberto/U-3083-2017 }}, ORCID-Numbers = {{Puppo, Paola/0000-0003-4677-5015 Somiya, Kentaro/0000-0003-2601-2264 Vecchio, Alberto/0000-0002-6254-1617 Acernese, Fausto/0000-0003-3103-3473 Cuoco, Elena Dr./0000-0002-6528-3449 Rapagnani, Piero/0000-0002-1865-6126 Lueck, Harald/0000-0001-9350-4846 Vicere', Andrea/0000-0003-0624-6231 Cuoco, Elena/0000-0002-6528-3449 Prato, Mirko/0000-0002-2188-8059 Gemme, Gianluca/0000-0002-1127-7406 Willke, Benno/0000-0003-0524-2925 Danilishin, Stefan/0000-0001-7758-7493 Harms, Jan/0000-0002-7332-9806 Martin, Iain/0000-0001-7300-9151 Lorenzini, Matteo/0000-0002-2765-7905 O'Shaughnessy, Richard/0000-0001-5832-8517 Kokkotas, Kostas D/0000-0001-6048-2919 Prato, Mirko/0000-0002-2188-8059 Rocchi, Alessio/0000-0002-1382-9016 Van Den Broeck, Chris/0000-0001-6800-4006 Falferi, Paolo/0000-0002-1929-4710 Punturo, Michele/0000-0001-8722-4485 Acernese, Fausto/0000-0003-3103-3473 Hild, Stefan/0000-0001-9221-6009 Ott, Christian/0000-0003-4993-2055 Barr, Bryan/0000-0002-5232-2736 mosca, simona/0000-0001-7869-8275 Harms, Jan/0000-0002-7332-9806 Rapagnani, Piero/0000-0002-1865-6126 Frasconi, Franco/0000-0003-4204-6587 Husa, Sascha/0000-0002-0445-1971 Allen, Bruce/0000-0003-4285-6256 Cella, Giancarlo/0000-0002-0752-0338 di virgilio, angela/0000-0002-2237-7533 Speirits, Fiona/0000-0002-6460-5231 Plastino, Wolfango/0000-0002-5737-6346 Strain, Kenneth/0000-0002-2066-5355 Palomba, Cristiano/0000-0002-4450-9883 Veitch, John/0000-0002-6508-0713 Guidi, Gianluca/0000-0002-3061-9870 Krishnan, Badri/0000-0003-3015-234X Majorana, Ettore/0000-0002-2383-3692 Granata, Massimo/0000-0003-3275-1186 Bulik, Tomasz/0000-0003-2045-4803 van den Brand, Johannes/0000-0003-4434-5353 Ricci, Fulvio/0000-0001-5475-4447 Mandel, Ilya/0000-0002-6134-8946 Sintes, Alicia M/0000-0001-9050-7515 Sathyaprakash, Bangalore/0000-0003-3845-7586 Woan, Graham/0000-0003-0381-0394 Di Fiore, Luciano/0000-0001-6296-1526 Chincarini, Andrea/0000-0003-4094-9942 Barone, Fabrizio/0000-0002-8069-8490 Coccia, Eugenio/0000-0002-6669-5787 Vetrano, Flavio/0000-0002-7523-4296 Hough, James/0000-0003-3242-3123 Hammond, Giles/0000-0002-1414-3622 Passaquieti, Roberto/0000-0003-4753-9428 Freise, Andreas/0000-0001-6586-9901 Andersson, Nils/0000-0001-8550-3843 Yamamoto, Kazuhiro/0000-0001-5647-6735 calloni, enrico/0000-0003-4819-3297 Poggiani, Rosa/0000-0002-9968-2464}}, Unique-ID = {{ISI:000282067500003}}, } @article{ ISI:000281644400007, Author = {Mishra, Chandra Kant and Arun, K. G. and Iyer, Bala R. and Sathyaprakash, B. S.}, Title = {{Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2010}}, Volume = {{82}}, Number = {{6}}, Month = {{SEP 7}}, Abstract = {{General relativity has very specific predictions for the gravitational waveforms from inspiralling compact binaries obtained using the post-Newtonian (PN) approximation. We investigate the extent to which the measurement of the PN coefficients, possible with the second generation gravitational-wave detectors such as the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) and the third generation gravitational-wave detectors such as the Einstein Telescope (ET), could be used to test post-Newtonian theory and to put bounds on a subclass of parametrized-post-Einstein theories which differ from general relativity in a parametrized sense. We demonstrate this possibility by employing the best inspiralling waveform model for nonspinning compact binaries which is 3.5PN accurate in phase and 3PN in amplitude. Within the class of theories considered, Advanced LIGO can test the theory at 1.5PN and thus the leading tail term. Future observations of stellar mass black hole binaries by ET can test the consistency between the various PN coefficients in the gravitational-wave phasing over the mass range of 11-44M(circle dot). The choice of the lower frequency cutoff is important for testing post-Newtonian theory using the ET. The bias in the test arising from the assumption of nonspinning binaries is indicated.}}, DOI = {{10.1103/PhysRevD.82.064010}}, Article-Number = {{064010}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Iyer, Bala R./E-2894-2012 Sathyaprakash, Bangalore/M-1235-2014}}, ORCID-Numbers = {{Iyer, Bala R./0000-0002-4141-5179 Mishra, Chandra Kant/0000-0002-8115-8728 Sathyaprakash, Bangalore/0000-0003-3845-7586}}, Unique-ID = {{ISI:000281644400007}}, } @article{ ISI:000279941700008, Author = {Postnikov, Sergey and Prakash, Madappa and Lattimer, James M.}, Title = {{Tidal Love numbers of neutron and self-bound quark stars}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2010}}, Volume = {{82}}, Number = {{2}}, Month = {{JUL 15}}, Abstract = {{Gravitational waves from the final stages of inspiraling binary neutron stars are expected to be one of the most important sources for ground-based gravitational wave detectors. The masses of the components are determinable from the orbital and chirp frequencies during the early part of the evolution, and large finite-size (tidal) effects are measurable toward the end of inspiral, but the gravitational wave signal is expected to be very complex at this time. Tidal effects during the early part of the evolution will form a very small correction, but during this phase the signal is relatively clean. The accumulated phase shift due to tidal corrections is characterized by a single quantity related to a star's tidal Love number. The Love number is sensitive, in particular, to the compactness parameter M/R and the star's internal structure, and its determination could provide an important constraint to the neutron star radius. We show that Love numbers of self-bound strange quark matter stars are qualitatively different from those of normal neutron stars. Observations of the tidal signature from coalescing compact binaries could therefore provide an important, and possibly unique, way to distinguish self-bound strange quark stars from normal neutron stars. Tidal signatures from self-bound strange quark stars with masses smaller than 1M(circle dot) are substantially smaller than those of normal stars owing to their smaller radii. Thus tidal signatures of stars less massive than 1M(circle dot) are probably not detectable with Advanced LIGO. For stars with masses in the range 1-2M(circle dot), the anticipated efficiency of the proposed Einstein telescope would be required for the detection of tidal signatures.}}, DOI = {{10.1103/PhysRevD.82.024016}}, Article-Number = {{024016}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Lattimer, James M/L-6242-2017 Prakash, Madappa/D-9820-2016}}, ORCID-Numbers = {{Lattimer, James M/0000-0002-5907-4552 }}, Unique-ID = {{ISI:000279941700008}}, } @article{ ISI:000279161800001, Author = {Hinderer, Tanja and Lackey, Benjamin D. and Lang, Ryan N. and Read, Jocelyn S.}, Title = {{Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2010}}, Volume = {{81}}, Number = {{12}}, Month = {{JUN 23}}, Abstract = {{The early part of the gravitational wave signal of binary neutron-star inspirals can potentially yield robust information on the nuclear equation of state. The influence of a star's internal structure on the waveform is characterized by a single parameter: the tidal deformability lambda, which measures the star's quadrupole deformation in response to the companion's perturbing tidal field. We calculate lambda for a wide range of equations of state and find that the value of lambda spans an order of magnitude for the range of equation of state models considered. An analysis of the feasibility of discriminating between neutron-star equations of state with gravitational wave observations of the early part of the inspiral reveals that the measurement error in lambda increases steeply with the total mass of the binary. Comparing the errors with the expected range of lambda, we find that Advanced LIGO observations of binaries at a distance of 100 Mpc will probe only unusually stiff equations of state, while the proposed Einstein Telescope is likely to see a clean tidal signature.}}, DOI = {{10.1103/PhysRevD.81.123016}}, Article-Number = {{123016}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ORCID-Numbers = {{Read, Jocelyn/0000-0002-3923-1055 Hinderer, Tanja/0000-0002-3394-6105}}, Unique-ID = {{ISI:000279161800001}}, } @article{ ISI:000279081800002, Author = {Eberle, Tobias and Steinlechner, Sebastian and Bauchrowitz, Joeran and Haendchen, Vitus and Vahlbruch, Henning and Mehmet, Moritz and Mueller-Ebhardt, Helge and Schnabel, Roman}, Title = {{Quantum Enhancement of the Zero-Area Sagnac Interferometer Topology for Gravitational Wave Detection}}, Journal = {{PHYSICAL REVIEW LETTERS}}, Year = {{2010}}, Volume = {{104}}, Number = {{25}}, Month = {{JUN 22}}, Abstract = {{Only a few years ago, it was realized that the zero-area Sagnac interferometer topology is able to perform quantum nondemolition measurements of position changes of a mechanical oscillator. Here, we experimentally show that such an interferometer can also be efficiently enhanced by squeezed light. We achieved a nonclassical sensitivity improvement of up to 8.2 dB, limited by optical loss inside our interferometer. Measurements performed directly on our squeezed-light laser output revealed squeezing of 12.7 dB. We show that the sensitivity of a squeezed-light enhanced Sagnac interferometer can surpass the standard quantum limit for a broad spectrum of signal frequencies without the need for filter cavities as required for Michelson interferometers. The Sagnac topology is therefore a powerful option for future gravitational-wave detectors, such as the Einstein Telescope, whose design is currently being studied.}}, DOI = {{10.1103/PhysRevLett.104.251102}}, Article-Number = {{251102}}, ISSN = {{0031-9007}}, EISSN = {{1079-7114}}, ResearcherID-Numbers = {{Gehring, Tobias/A-8596-2016 Schnabel, Roman/V-7759-2019 Steinlechner, Sebastian S/D-5781-2013}}, ORCID-Numbers = {{Gehring, Tobias/0000-0002-4311-2593 Steinlechner, Sebastian S/0000-0003-4710-8548}}, Unique-ID = {{ISI:000279081800002}}, } @article{ ISI:000282154300008, Author = {Punturo, M. and Abernathy, M. and Acernese, F. and Allen, B. and Andersson, N. and Arun, K. and Barone, F. and Barr, B. and Barsuglia, M. and Beker, M. and Beveridge, N. and Birindelli, S. and Bose, S. and Bosi, L. and Braccini, S. and Bradaschia, C. and Bulik, T. and Calloni, E. and Cella, G. and Mottin, E. Chassande and Chelkowski, S. and Chincarini, A. and Clark, J. and Coccia, E. and Colacino, C. and Colas, J. and Cumming, A. and Cunningham, L. and Cuoco, E. and Danilishin, S. and Danzmann, K. and De Luca, G. and De Salvo, R. and Dent, T. and Derosa, R. and Di Fiore, L. and Di Virgilio, A. and Doets, M. and Fafone, V. and Falferi, P. and Flaminio, R. and Franc, J. and Frasconi, F. and Freise, A. and Fulda, P. and Gair, J. and Gemme, G. and Gennai, A. and Giazotto, A. and Glampedakis, K. and Granata, M. and Grote, H. and Guidi, G. and Hammond, G. and Hannam, M. and Harms, J. and Heinert, D. and Hendry, M. and Heng, I. and Hennes, E. and Hild, S. and Hough, J. and Husa, S. and Huttner, S. and Jones, G. and Khalili, F. and Kokeyama, K. and Kokkotas, K. and Krishnan, B. and Lorenzini, M. and Lueck, H. and Majorana, E. and Mandel, I. and Mandic, V. and Martin, I. and Michel, C. and Minenkov, Y. and Morgado, N. and Mosca, S. and Mours, B. and Mueller-Ebhardt, H. and Murray, P. and Nawrodt, R. and Nelson, J. and Oshaughnessy, R. and Ott, C. D. and Palomba, C. and Paoli, A. and Parguez, G. and Pasqualetti, A. and Passaquieti, R. and Passuello, D. and Pinard, L. and Poggiani, R. and Popolizio, P. and Prato, M. and Puppo, P. and Rabeling, D. and Rapagnani, P. and Read, J. and Regimbau, T. and Rehbein, H. and Reid, S. and Rezzolla, L. and Ricci, F. and Richard, F. and Rocchi, A. and Rowan, S. and Ruediger, A. and Sassolas, B. and Sathyaprakash, B. and Schnabel, R. and Schwarz, C. and Seidel, P. and Sintes, A. and Somiya, K. and Speirits, F. and Strain, K. and Strigin, S. and Sutton, P. and Tarabrin, S. and Van den Brand, J. and Van Leewen, C. and Van Veggel, M. and Van den Broeck, C. and Vecchio, A. and Veitch, J. and Vetrano, F. and Vicere, A. and Vyatchanin, S. and Willke, B. and Woan, G. and Plastino, W. and Yamamoto, K.}, Title = {{The third generation of gravitational wave observatories and their science reach}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2010}}, Volume = {{27}}, Number = {{8}}, Month = {{APR 21}}, Note = {{8th Edoardo Amaldi Conference on Gravitational Waves, Columbia Univ, New York, NY, JUN 22-26, 2009}}, Abstract = {{Large gravitational wave interferometric detectors, like Virgo and LIGO, demonstrated the capability to reach their design sensitivity, but to transform these machines into an effective observational instrument for gravitational wave astronomy a large improvement in sensitivity is required. Advanced detectors in the near future and third-generation observatories in more than one decade will open the possibility to perform gravitational wave astronomical observations from the Earth. An overview of the possible science reaches and the technological progress needed to realize a third-generation observatory are discussed in this paper. The status of the project Einstein Telescope (ET), a design study of a third-generation gravitational wave observatory, will be reported.}}, DOI = {{10.1088/0264-9381/27/8/084007}}, Article-Number = {{084007}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Rapagnani, Piero/T-2050-2019 Punturo, Michele/I-3995-2012 Strigin, Sergey E/I-8337-2012 Hammond, Giles/B-7861-2009 Barr, Bryan/G-3348-2019 Hammond, Giles/A-8168-2012 di virgilio, angela/E-9078-2015 Rocchi, Alessio/O-9499-2015 Sintes, Alicia M/AAF-4791-2019 Chincarini, Andrea/J-9998-2018 Schnabel, Roman/V-7759-2019 Harms, Jan/J-4359-2012 Frasconi, Franco/K-1068-2016 Puppo, Paola/J-4250-2012 Acernese, Fausto/AAX-5705-2020 Prato, Mirko/AAD-9075-2019 Martin, Iain/A-2445-2010 Allen, Bruce/K-2327-2012 Prato, Mirko/D-8531-2012 di virgilio, angela/AAA-4814-2019 Hild, Stefan/A-3864-2010 Husa, Sascha/AAB-6992-2019 Harms, Jan/O-7967-2019 Acernese, Fausto/E-4989-2010 Lorenzini, Matteo/AAC-6035-2021 Bulik, Tomasz/AAJ-6742-2020 Lueck, Harald/F-7100-2011 Abernathy, Matthew/G-1113-2011 Ott, Christian/G-2651-2011 Khalili, Farit Ya/D-8113-2012 Kokkotas, Kostas D/B-7878-2010 O'Shaughnessy, Richard/AAA-3625-2021 Cella, Giancarlo/A-9946-2012 Vicere', Andrea/J-1742-2012 Vyatchanin, Sergey P/J-2238-2012 Falferi, Paolo/C-3439-2015 Van Den Broeck, Chris/R-7871-2018 Martin, Iain/V-1198-2018 Willke, Benno/U-8992-2017 Dent, Thomas/AAB-3674-2019 Rapagnani, Piero/J-4783-2012 Gemme, Gianluca/C-7233-2008 Somiya, Kentaro/ABE-2215-2020 calloni, enrico/K-5852-2019 Cuoco, Elena Dr./I-8789-2012 Freise, Andreas/F-8892-2011 Danilishin, Stefan/K-7262-2012 Poggiani, Rosa/P-8801-2018 Vecchio, Alberto/F-8310-2015 Cuoco, Elena/O-4680-2019 Strain, Kenneth/D-5236-2011 mosca, simona/I-7116-2012 Sathyaprakash, Bangalore/M-1235-2014 Passaquieti, Roberto/U-3083-2017 }}, ORCID-Numbers = {{Rapagnani, Piero/0000-0002-1865-6126 Punturo, Michele/0000-0001-8722-4485 Barr, Bryan/0000-0002-5232-2736 di virgilio, angela/0000-0002-2237-7533 Rocchi, Alessio/0000-0002-1382-9016 Harms, Jan/0000-0002-7332-9806 Frasconi, Franco/0000-0003-4204-6587 Puppo, Paola/0000-0003-4677-5015 Acernese, Fausto/0000-0003-3103-3473 Prato, Mirko/0000-0002-2188-8059 Allen, Bruce/0000-0003-4285-6256 Prato, Mirko/0000-0002-2188-8059 Hild, Stefan/0000-0001-9221-6009 Husa, Sascha/0000-0002-0445-1971 Harms, Jan/0000-0002-7332-9806 Acernese, Fausto/0000-0003-3103-3473 Lorenzini, Matteo/0000-0002-2765-7905 Lueck, Harald/0000-0001-9350-4846 Ott, Christian/0000-0003-4993-2055 Kokkotas, Kostas D/0000-0001-6048-2919 O'Shaughnessy, Richard/0000-0001-5832-8517 Cella, Giancarlo/0000-0002-0752-0338 Vicere', Andrea/0000-0003-0624-6231 Falferi, Paolo/0000-0002-1929-4710 Van Den Broeck, Chris/0000-0001-6800-4006 Martin, Iain/0000-0001-7300-9151 Willke, Benno/0000-0003-0524-2925 Rapagnani, Piero/0000-0002-1865-6126 Gemme, Gianluca/0000-0002-1127-7406 Somiya, Kentaro/0000-0003-2601-2264 Cuoco, Elena Dr./0000-0002-6528-3449 Danilishin, Stefan/0000-0001-7758-7493 Vecchio, Alberto/0000-0002-6254-1617 Cuoco, Elena/0000-0002-6528-3449 Strain, Kenneth/0000-0002-2066-5355 Yamamoto, Kazuhiro/0000-0001-5647-6735 calloni, enrico/0000-0003-4819-3297 mosca, simona/0000-0001-7869-8275 Bulik, Tomasz/0000-0003-2045-4803 Palomba, Cristiano/0000-0002-4450-9883 Speirits, Fiona/0000-0002-6460-5231 Ricci, Fulvio/0000-0001-5475-4447 Krishnan, Badri/0000-0003-3015-234X Majorana, Ettore/0000-0002-2383-3692 Chincarini, Andrea/0000-0003-4094-9942 Sathyaprakash, Bangalore/0000-0003-3845-7586 Sintes, Alicia M/0000-0001-9050-7515 Coccia, Eugenio/0000-0002-6669-5787 Guidi, Gianluca/0000-0002-3061-9870 Andersson, Nils/0000-0001-8550-3843 Barone, Fabrizio/0000-0002-8069-8490 Passaquieti, Roberto/0000-0003-4753-9428 Freise, Andreas/0000-0001-6586-9901 Poggiani, Rosa/0000-0002-9968-2464 Hough, James/0000-0003-3242-3123 Hammond, Giles/0000-0002-1414-3622 van den Brand, Johannes/0000-0003-4434-5353 Veitch, John/0000-0002-6508-0713 Mandel, Ilya/0000-0002-6134-8946 Woan, Graham/0000-0003-0381-0394 Vetrano, Flavio/0000-0002-7523-4296 Plastino, Wolfango/0000-0002-5737-6346 Granata, Massimo/0000-0003-3275-1186}}, Unique-ID = {{ISI:000282154300008}}, } @article{ ISI:000276420300008, Author = {Acernese, F. and Antonucci, F. and Aoudia, S. and Arun, K. G. and Astone, P. and Ballardin, G. and Barone, F. and Barsuglie, M. and Bauer, Th. S. and Beker, M. G. and Bigotta, S. and Birindelli, S. and Bitossi, M. and Bizouard, M. A. and Blom, M. and Boccara, C. and Bondu, F. and Bonelli, L. and Bosi, L. and Braccini, S. and Bradaschia, C. and Brillet, A. and Brisson, V. and Budzynski, R. and Bulik, T. and Bulten, H. J. and Buskulic, D. and Cagnoli, G. and Calloni, E. and Campagna, E. and Canuel, B. and Carbognani, F. and Cavalier, F. and Cavalieri, R. and Celia, G. and Cesarini, E. and Chassande-Mottin, E. and Chincarini, A. and Cleva, F. and Coccia, E. and Colacine, C. N. and Colas, J. and Colla, A. and Colombini, M. and Corda, C. and Corsi, A. and Coulon, J-P. and Cuoco, E. and D'Antonio, S. and Dari, A. and Dattilo, V. and Davier, M. and Day, R. and De Rosa, R. and Del Prete, M. and Di Fiore, L. and Di Lieto, A. and Emilio, M. Di Paolo and Di Virgilio, A. and Dietz, A. and Drago, M. and Fafone, V. and Ferrante, I. and Fidecaro, F. and Fiori, I. and Flaminio, R. and Fournier, J-D. and Franc, J. and Frasca, S. and Frasconi, F. and Freise, A. and Gammaitoni, L. and Garufi, F. and Gemme, G. and Genin, E. and Gennai, A. and Giazotto, A. and Granata, M. and Greverie, C. and Guidi, G. and Heitmann, H. and Hello, P. and Hild, S. and Huet, D. and Jaranowski, P. and Kowalska, I. and Krolak, A. and La Penna, P. and Leroy, N. and Letendre, N. and Li, T. G. F. and Lorenzini, M. and Loriette, V. and Losurdo, G. and Mackowski, J-M. and Majorana, E. and Man, N. and Mantovani, M. and Marchesoni, F. and Marion, F. and Marque, J. and Martelli, F. and Masserot, A. and Menzinger, F. and Michel, C. and Milano, L. and Minenkov, Y. and Mohan, M. and Moreau, J. and Morgado, N. and Morgia, A. and Mosca, S. and Moscatelli, V. and Mours, B. and Neri, I. and Nocera, F. and Pagliaroli, G. and Palomba, C. and Paoletti, F. and Pardi, S. and Parisi, M. and Pasqualetti, A. and Passaquieti, R. and Passuello, D. and Persichetti, G. and Pichot, M. and Piergiovanni, F. and Pietka, M. and Pinard, L. and Poggiani, R. and Prato, M. and Prodi, G. A. and Punturo, M. and Puppo, P. and Rabaste, O. and Rabeling, D. S. and Rapagnani, P. and Re, V. and Regimbau, T. and Ricci, F. and Robinet, F. and Rocchi, A. and Rolland, L. and Romano, R. and Rosinska, D. and Ruggi, P. and Salemi, F. and Sassolas, B. and Sentenac, D. and Sturani, R. and Swinkels, B. and Toncelli, A. and Tonelli, M. and Tournefier, E. and Travasso, F. and Trummer, J. and Vajente, G. and van den Brand, J. F. J. and van der Puttee, S. and Vavoulidis, M. and Vedovato, G. and Verkindt, D. and Vetrano, F. and Vicere, A. and Vinet, J-Y. and Vocca, H. and Was, M. and Yvert, M.}, Title = {{Measurements of Superattenuator seismic isolation by Virgo interferometer}}, Journal = {{ASTROPARTICLE PHYSICS}}, Year = {{2010}}, Volume = {{33}}, Number = {{3}}, Pages = {{182-189}}, Month = {{APR}}, Abstract = {{Each mirror of the interferometric gravitational wave antenna Virgo is attached to a Superattenuator, a chain of mechanical filters designed to suppress seismic vibrations, starting from a few Hz The filter chain attenuation has been measured by exciting its suspension point with sinuisodal forces and using the interferometer as sensor. The attenuation, measured at different frequencies, is compliant with the requirements of the next generation antenna Advanced Virgo In the third generation detector Einstein Telescope, the attenuation is sufficient above 3 Hz, independently of the underground site choice. (C) 2010 Elsevier B.V. All rights reserved.}}, DOI = {{10.1016/j.astropartphys.2010.01.006}}, ISSN = {{0927-6505}}, EISSN = {{1873-2852}}, ResearcherID-Numbers = {{Rapagnani, Piero/T-2050-2019 Toncelli, Alessandra/A-5352-2012 Cesarini, Elisabetta/C-4507-2017 Hild, Stefan/A-3864-2010 Corda, Christian/C-1169-2013 Punturo, Michele/I-3995-2012 Freise, Andreas/F-8892-2011 dattilo, vincenzino/N-9732-2015 Bulik, Tomasz/AAJ-6742-2020 Vocca, Helios/J-9579-2016 Krolak, Andrzej/V-3384-2017 Marchesoni, Fabio/A-1920-2008 Chincarini, Andrea/J-9998-2018 Salemi, Francesco/F-6988-2014 CHASSANDE-MOTTIN, Eric/ABC-2478-2020 Prodi, Giovanni Andrea/B-4398-2010 Re, Virginia/F-6403-2013 Acernese, Fausto/AAX-5705-2020 mosca, simona/I-7116-2012 Fidecaro, Francesco/H-9581-2017 Rocchi, Alessio/O-9499-2015 Puppo, Paola/J-4250-2012 Vocca, Helios/F-1444-2010 Garufi, Fabio/K-3263-2015 Frasconi, Franco/K-1068-2016 Lorenzini, Matteo/AAC-6035-2021 Neri, Igor/F-1482-2010 DRAGO, Marco/K-6895-2019 Pagliaroli, Giulia/AAA-7637-2020 Parisi, Maria/D-2817-2013 Bondu, Francois/A-2071-2012 di virgilio, angela/AAA-4814-2019 Ferrante, Isidoro/F-1017-2012 Losurdo, Giovanni/K-1241-2014 Acernese, Fausto/E-4989-2010 di virgilio, angela/E-9078-2015 Bigotta, Stefano/F-8652-2011 Prato, Mirko/AAD-9075-2019 Cuoco, Elena Dr./I-8789-2012 Martelli, Filippo/P-4041-2015 Travasso, Flavio/J-9595-2016 Colla, Alberto/J-4694-2012 Gemme, Gianluca/C-7233-2008 Canuel, Benjamin/C-7459-2014 Poggiani, Rosa/P-8801-2018 Rapagnani, Piero/J-4783-2012 Cuoco, Elena/O-4680-2019 calloni, enrico/K-5852-2019 Drago, Marco/E-7134-2013 Prato, Mirko/D-8531-2012 Vicere', Andrea/J-1742-2012 Gammaitoni, Luca/B-5375-2009 Passaquieti, Roberto/U-3083-2017 }}, ORCID-Numbers = {{Rapagnani, Piero/0000-0002-1865-6126 Toncelli, Alessandra/0000-0003-4400-8808 Cesarini, Elisabetta/0000-0001-9127-3167 Hild, Stefan/0000-0001-9221-6009 Punturo, Michele/0000-0001-8722-4485 Vocca, Helios/0000-0002-1200-3917 Marchesoni, Fabio/0000-0001-9240-6793 Salemi, Francesco/0000-0002-9511-3846 CHASSANDE-MOTTIN, Eric/0000-0003-3768-9908 Prodi, Giovanni Andrea/0000-0001-5256-915X Acernese, Fausto/0000-0003-3103-3473 mosca, simona/0000-0001-7869-8275 Fidecaro, Francesco/0000-0002-6189-3311 Rocchi, Alessio/0000-0002-1382-9016 Puppo, Paola/0000-0003-4677-5015 Vocca, Helios/0000-0002-1200-3917 Garufi, Fabio/0000-0003-1391-6168 Frasconi, Franco/0000-0003-4204-6587 Lorenzini, Matteo/0000-0002-2765-7905 Neri, Igor/0000-0002-9047-9822 DRAGO, Marco/0000-0002-3738-2431 Bondu, Francois/0000-0001-6487-5197 Ferrante, Isidoro/0000-0002-0083-7228 Losurdo, Giovanni/0000-0003-0452-746X Acernese, Fausto/0000-0003-3103-3473 di virgilio, angela/0000-0002-2237-7533 Prato, Mirko/0000-0002-2188-8059 Cuoco, Elena Dr./0000-0002-6528-3449 Martelli, Filippo/0000-0003-3761-8616 Travasso, Flavio/0000-0002-4653-6156 Gemme, Gianluca/0000-0002-1127-7406 Rapagnani, Piero/0000-0002-1865-6126 Cuoco, Elena/0000-0002-6528-3449 Prato, Mirko/0000-0002-2188-8059 Vicere', Andrea/0000-0003-0624-6231 Gammaitoni, Luca/0000-0002-4972-7062 Vedovato, Gabriele/0000-0001-7226-1320 Rosinska, Dorota/0000-0002-3681-9304 PERSICHETTI, GIANLUCA/0000-0001-8424-9791 Barone, Fabrizio/0000-0002-8069-8490 Poggiani, Rosa/0000-0002-9968-2464 Romano, Rocco/0000-0002-0485-6936 Vetrano, Flavio/0000-0002-7523-4296 Piergiovanni, Francesco/0000-0001-8063-828X Chincarini, Andrea/0000-0003-4094-9942 mantovani, maddalena/0000-0002-4424-5726 Jaranowski, Piotr/0000-0001-8085-3414 Bulik, Tomasz/0000-0003-2045-4803 Ricci, Fulvio/0000-0001-5475-4447 Guidi, Gianluca/0000-0002-3061-9870 Coccia, Eugenio/0000-0002-6669-5787 Kowalska-Leszczynska, Izabela/0000-0002-6569-3800 Di Fiore, Luciano/0000-0001-6296-1526 calloni, enrico/0000-0003-4819-3297 Passaquieti, Roberto/0000-0003-4753-9428 Vajente, Gabriele/0000-0002-7656-6882 Freise, Andreas/0000-0001-6586-9901 Di Paolo Emilio, Maurizio/0000-0002-9558-3610 Palomba, Cristiano/0000-0002-4450-9883 van den Brand, Johannes/0000-0003-4434-5353 Granata, Massimo/0000-0003-3275-1186 Majorana, Ettore/0000-0002-2383-3692 DI LIETO, ALBERTO/0000-0002-4787-0754 Swinkels, Bas/0000-0002-3066-3601}}, Unique-ID = {{ISI:000276420300008}}, } @inproceedings{ ISI:000284461800031, Author = {Puppo, Paola}, Editor = {{Marka, Z and Marka, S}}, Title = {{A thermal noise model for a branched system of harmonic oscillators.}}, Booktitle = {{8TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES}}, Series = {{Journal of Physics Conference Series}}, Year = {{2010}}, Volume = {{228}}, Note = {{8th Edoardo Amaldi Conference on Gravitational Waves, Columbia Univ, New York, NY, JUN 21-26, 2009}}, Abstract = {{We have calculated the thermal noise of a branched system of oscillators through the normal mode representation. This model describes well the mechanical behavior of the last stage suspension system like in the Virgo interferometer and is consistent with the predictions coming from the fluctuation-dissipation theorem. Moreover, the developed formalism can be useful to infer informations on the mechanical quantities of the uncoupled elements of the suspension and on the suspension thermal noise predictions for a third generation gravitational interferometer like the Einstein Telescope (ET).}}, DOI = {{10.1088/1742-6596/228/1/012031}}, Article-Number = {{012031}}, ISSN = {{1742-6588}}, ResearcherID-Numbers = {{Puppo, Paola/J-4250-2012}}, ORCID-Numbers = {{Puppo, Paola/0000-0003-4677-5015}}, Unique-ID = {{ISI:000284461800031}}, } @inproceedings{ ISI:000284461800009, Author = {Regimbau, T. and Hughes, Scott A.}, Editor = {{Marka, Z and Marka, S}}, Title = {{Confusion background from compact binaries}}, Booktitle = {{8TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES}}, Series = {{Journal of Physics Conference Series}}, Year = {{2010}}, Volume = {{228}}, Note = {{8th Edoardo Amaldi Conference on Gravitational Waves, Columbia Univ, New York, NY, JUN 21-26, 2009}}, Abstract = {{Double neutron stars are one of the most promizing sources for terrestrial gravitational wave interferometers. For actual interferometers and their planned upgrades, the probability of having a signal present in the data is small, but as the sensitivity improves, the detection rate increases and the waveforms may start to overlap, creating a confusion background, ultimately limiting the capabilities of future detectors. The third generation Einstein Telescope, with an horizon of z > 1and very low frequency ``seismic wall{''} may be affected by such confusion noise. At a minimum, careful dataanalysis will be require to separate signals which will appear confused. This result should be borne in mind when designing highly advanced future instruments.}}, DOI = {{10.1088/1742-6596/228/1/012009}}, Article-Number = {{012009}}, ISSN = {{1742-6588}}, Unique-ID = {{ISI:000284461800009}}, } @inproceedings{ ISI:000284461800029, Author = {Schnabel, R. and Britzger, M. and Brueckner, F. and Burmeister, O. and Danzmann, K. and Dueck, J. and Eberle, T. and Friedrich, D. and Lueck, H. and Mehmet, M. and Nawrodt, R. and Steinlechner, S. and Willke, B.}, Editor = {{Marka, Z and Marka, S}}, Title = {{Building blocks for future detectors: Silicon test masses and 1550 nm laser light}}, Booktitle = {{8TH EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES}}, Series = {{Journal of Physics Conference Series}}, Year = {{2010}}, Volume = {{228}}, Note = {{8th Edoardo Amaldi Conference on Gravitational Waves, Columbia Univ, New York, NY, JUN 21-26, 2009}}, Abstract = {{Current interferometric gravitational wave detectors use the combination of quasi-monochromatic, continuous-wave laser light at 1064 nm and fused silica test masses at room temperature. Detectors of the third generation, such as the Einstein-Telescope, will involve a considerable sensitivity increase. The combination of 1550 nm laser radiation and crystalline silicon test masses at low temperatures might be important ingredients in order to achieve the sensitivity goal. Here we compare some properties of the fused silica and silicon test mass materials relevant for decreasing the thermal noise in future detectors as well as the recent technology achievements in the preparation of laser radiation at 1064 nm and 1550 nm relevant for decreasing the quantum noise. We conclude that silicon test masses and 1550 nm laser light have the potential to form the future building blocks of gravitational wave detection.}}, DOI = {{10.1088/1742-6596/228/1/012029}}, Article-Number = {{012029}}, ISSN = {{1742-6588}}, ResearcherID-Numbers = {{Steinlechner, Sebastian S/D-5781-2013 Willke, Benno/U-8992-2017 Schnabel, Roman/V-7759-2019 Gehring, Tobias/A-8596-2016 Lueck, Harald/F-7100-2011}}, ORCID-Numbers = {{Steinlechner, Sebastian S/0000-0003-4710-8548 Willke, Benno/0000-0003-0524-2925 Gehring, Tobias/0000-0002-4311-2593 Lueck, Harald/0000-0001-9350-4846}}, Unique-ID = {{ISI:000284461800029}}, } @inproceedings{ ISI:000350221400005, Author = {Marque, J. and Virgo Collaboration}, Editor = {{Bertolucci, S and Bottigli, U and Oliva, P}}, Title = {{A gravitational wave detector: The Virgo interferometer}}, Booktitle = {{RADIATION AND PARTICLE DETECTORS}}, Series = {{Proceedings of the International School of Physics Enrico Fermi}}, Year = {{2010}}, Volume = {{175}}, Pages = {{105-122}}, Note = {{International School of Physics Enrico Fermi on Radiation and Particle Detectors, Varenna, ITALY, JUL 20-25, 2009}}, Abstract = {{Gravitational waves were predicted in 1916 by Einstein as a consequence of the theory of General Relativity: accelerated masses can produce ripples propagating at the speed of light, which perturb the space-time metric. Thanks to the extremely weak coupling with matter, gravitational waves can cross the universe undisturbed and, hence, are a probe of the regions where they are produced which is not accessible by the eventual electromagnetic counterpart. The gravitational waves sources of detectable amplitudes are expected to be compact astrophysical sources such as the coalescence of binaries formed by black holes and neutron stars, the collapses of stellar cores, or the rotation of non-axis-symmetric neutron stars. For more than 40 years the search for gravitational waves has been pursued with resonant detectors made of metallic bars. The development of gravitational wave detectors based on laser interferometers started in the early seventies. After more than two decades of development, the construction of the first interferometers with kilometer scale arms started in the nineties. The sensitivity of such detectors is fundamentally proportional to its length, and with its 3 kilometer long arms Virgo is the largest gravitational wave detector in Europe, and the third largest in the world. It is located at the European Gravitational Observatory (EGO), close to Pisa, and it is designed to detect gravitational waves emitted by astrophysical sources in the frequency range between 10 Hz and a few kHz. Among the other current ground-based gravitational wave detectors, Virgo is the one having the best sensitivity at low frequency, thanks to the particular seismic attenuators, from which the mirrors are suspended. Construction started in 1996 and ended in July 2003. After a very intense commissioning phase, the performances of the detector are now very close to the design ones, and the detector is entering the operation phase. In parallel, the design phase of the second generation of interferometers should be finalized this year with a construction planned to start in 2011. Also, the conceptual design is under study for a third generation. The corresponding European project is called the ``Einstein Telescope{''}.}}, DOI = {{10.3254/978-1-60750-630-0-105}}, ISSN = {{0074-784X}}, ISBN = {{978-1-60750-631-7; 978-1-60750-630-0}}, ResearcherID-Numbers = {{Cuoco, Elena Dr./I-8789-2012}}, ORCID-Numbers = {{Cuoco, Elena Dr./0000-0002-6528-3449}}, Unique-ID = {{ISI:000350221400005}}, } @inproceedings{ ISI:000280470400076, Author = {van den Brand, J. F. J. and Beker, M. G. and Doets, M. and Hennes, E. and Rabeling, D. S.}, Editor = {{Coccia, E and Pandola, L and Fornengo, N and Aloisio, R}}, Title = {{Einstein Telescope site selection: seismic and gravity gradient noise}}, Booktitle = {{TOPICS IN ASTROPARTICLE AND UNDERGROUND PHYSICS (TAUP2009)}}, Series = {{Journal of Physics Conference Series}}, Year = {{2010}}, Volume = {{203}}, Note = {{11th International Conference on Topics in Astroparticle and Underground Physics, Rome, ITALY, JUL 01-05, 2009}}, Organization = {{INFN Gran Sasso Natl Lab}}, Abstract = {{Gravity gradient noise generated by seismic displacements may be the limiting factor for the sensitivity of third-generation gravitational wave detectors at frequencies below 10 Hz. A finite element framework has been developed to calculate the soil response to various excitations. The accompanying gravity gradients as a result of the seismic displacement field can then be evaluated. The results of the gravity gradient noise are in good agreement with previous analytical results. Finally results of gravity gradient noise from a single pulse excitation of a homogenous medium are discussed for an underground detector.}}, DOI = {{10.1088/1742-6596/203/1/012076}}, Article-Number = {{012076}}, ISSN = {{1742-6588}}, ORCID-Numbers = {{van den Brand, Johannes/0000-0003-4434-5353}}, Unique-ID = {{ISI:000280470400076}}, } @inproceedings{ ISI:000284017700076, Author = {Trinchieri, Ginevra}, Editor = {{Comastri, A and Cappi, M and Angelini, L}}, Title = {{X-ray properties of normal galaxies in the local universe}}, Booktitle = {{X-RAY ASTRONOMY-2009: PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES, PROCEEDINGS}}, Series = {{AIP Conference Proceedings}}, Year = {{2010}}, Volume = {{1248}}, Pages = {{223-228}}, Note = {{International Conference on X-Ray Astronomy-2009: Present Status, Multi-Wavelength Approach and Future Perspectives, Bologna, ITALY, SEP 07-11, 2009}}, Organization = {{NASA, European Space Agcy; Italian Natl Inst Astrophys; Univ Bologna, Astron Dept}}, Abstract = {{Normal galaxies are intrinsically faint and complex systems, located in different environment that are often stronger sources of X-ray emission than the galaxies themselves. Therefore the study of their properties requires high quality images from telescopes with excellent spatial and spectral resolution, and large collecting area to compensate for their low fluxes. Since the pioneering work with the Einstein telescope, we have acquired a more detailed understanding of the characteristics of galaxies of different morphologies, star formation activity and in different environments. This review will of necessity be brief and will overlook many of the aspects that are of importance, unfortunately thereby omitting important contributions of many active researchers.}}, DOI = {{10.1063/1.3475216}}, ISSN = {{0094-243X}}, ISBN = {{978-0-7354-0795-4}}, ORCID-Numbers = {{Trinchieri, Ginevra/0000-0002-0227-502X}}, Unique-ID = {{ISI:000284017700076}}, } @article{ ISI:000270514600010, Author = {Gair, Jonathan R. and Mandel, Ilya and Sesana, Alberto and Vecchio, Alberto}, Title = {{Probing seed black holes using future gravitational-wave detectors}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2009}}, Volume = {{26}}, Number = {{20}}, Month = {{OCT 21}}, Abstract = {{Identifying the properties of the first generation of seeds of massive black holes is the key to understanding the merger history and growth of galaxies. Mergers between similar to 100M(circle dot) seed black holes generate gravitational waves in the 0.1-10 Hz band that lies between the sensitivity bands of existing ground-based detectors and the planned space-based gravitational wave detector, the Laser Interferometer Space Antenna (LISA). However, there are proposals for more advanced detectors that will bridge this gap, including the third generation ground-based Einstein Telescope and the space-based detector DECIGO. In this paper, we demonstrate that such future detectors should be able to detect gravitational waves produced by the coalescence of the first generation of light seed black hole binaries and provide information on the evolution of structure in that era. These observations will be complementary to those that LISA will make of subsequent mergers between more massive black holes. We compute the sensitivity of various future detectors to seed black hole mergers, and use this to explore the number and properties of the events that each detector might see in three years of observation. For this calculation, we make use of galaxy merger trees and two different seed black hole mass distributions in order to construct the astrophysical population of events. We also consider the accuracy with which networks of future ground-based detectors will be able to measure the parameters of seed black hole mergers, in particular the luminosity distance to the source. We show that distance precisions of similar to 30\% are achievable, which should be sufficient for us to say with confidence that the sources are at high redshift.}}, DOI = {{10.1088/0264-9381/26/20/204009}}, Article-Number = {{204009}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Vecchio, Alberto/F-8310-2015 Sesana, Alberto/Q-9826-2016 }}, ORCID-Numbers = {{Vecchio, Alberto/0000-0002-6254-1617 Sesana, Alberto/0000-0003-4961-1606 Mandel, Ilya/0000-0002-6134-8946}}, Unique-ID = {{ISI:000270514600010}}, } @article{ ISI:000271353700050, Author = {Yunes, Nicolas and Arun, K. G. and Berti, Emanuele and Will, Clifford M.}, Title = {{Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2009}}, Volume = {{80}}, Number = {{8}}, Month = {{OCT}}, Abstract = {{We lay the foundations for the construction of analytic expressions for Fourier-domain gravitational waveforms produced by eccentric, inspiraling compact binaries in a post-circular or small-eccentricity approximation. The time-dependent, ``plus'' and ``cross'' polarizations are expanded in Bessel functions, which are then self-consistently reexpanded in a power series about zero initial eccentricity to eighth order. The stationary-phase approximation is then employed to obtain explicit analytic expressions for the Fourier transform of the post-circular expanded, time-domain signal. We exemplify this framework by considering Newtonian-accurate waveforms, which in the post-circular scheme give rise to higher harmonics of the orbital phase and to amplitude corrections of the Fourier-domain waveform. Such higher harmonics lead to an effective increase in the inspiral mass reach of a detector as a function of the binary's eccentricity e(0) at the time when the binary enters the detector sensitivity band. Using the largest initial eccentricity allowed by our approximations (e(0) < 0.4), the mass reach is found to be enhanced up to factors of approximately 5 relative to that of circular binaries for Advanced LIGO, LISA, and the proposed Einstein Telescope at a signal-to-noise ratio of ten. A post-Newtonian generalization of the post-circular scheme is also discussed, which holds the promise to provide ``ready-to-use'' Fourier-domain waveforms for data analysis of eccentric inspirals.}}, DOI = {{10.1103/PhysRevD.80.084001}}, Article-Number = {{084001}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, ResearcherID-Numbers = {{Yunes, Nicolas/AAG-3146-2019 Berti, Emanuele/AAI-1513-2019 Berti, Emanuele/C-9331-2016}}, ORCID-Numbers = {{Yunes, Nicolas/0000-0001-6147-1736 Berti, Emanuele/0000-0003-0751-5130}}, Unique-ID = {{ISI:000271353700050}}, } @article{ ISI:000268180400004, Author = {Arun, K. G. and Will, Clifford M.}, Title = {{Bounding the mass of the graviton with gravitational waves: effect of higher harmonics in gravitational waveform templates}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2009}}, Volume = {{26}}, Number = {{15}}, Month = {{AUG 7}}, Abstract = {{Observations by laser interferometric detectors of gravitational waves from inspiraling compact binary systems can be used to search for a dependence of the waves' propagation speed on wavelength, and thereby to bound the mass or Compton wavelength of a putative graviton. We study the effect of including higher harmonics, as well as their post-Newtonian amplitude corrections, in the template gravitational waveforms employed in the process of parameter estimation using matched filtering. We consider the bounds that could be achieved using advanced LIGO, a proposed third generation instrument called an Einstein telescope and the proposed space interferometer LISA. We find that in all cases, the bounds on the graviton Compton wavelength are improved by almost an order of magnitude for higher masses when amplitude corrections are included.}}, DOI = {{10.1088/0264-9381/26/15/155002}}, Article-Number = {{155002}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, Unique-ID = {{ISI:000268180400004}}, } @article{ ISI:000267052600013, Author = {Sesana, Alberto and Gair, Jonathan and Mandel, Ilya and Vecchio, Alberto}, Title = {{OBSERVING GRAVITATIONAL WAVES FROM THE FIRST GENERATION OF BLACK HOLES}}, Journal = {{ASTROPHYSICAL JOURNAL LETTERS}}, Year = {{2009}}, Volume = {{698}}, Number = {{2}}, Pages = {{L129-L132}}, Month = {{JUN 20}}, Abstract = {{The properties of the first generation of black hole seeds trace and distinguish different models of formation of cosmic structure in the high-redshift universe. The observational challenge lies in identifying black holes in the mass range similar to 100-1000 M-circle dot at redshift z similar to 10. The typical frequencies of gravitational waves produced by the coalescence of the first generation of light seed black hole binaries fall in the gap between the spectral ranges of low-frequency space-borne detectors (e. g., LISA) and high-frequency ground-based detectors (e. g., LIGO, Virgo, and GEO 600). As such, these sources are targets for proposed third-generation ground-based instruments, such as the Einstein Telescope which is currently in design study. Using galaxy merger trees and four different models of black hole accretion-which are meant to illustrate the potential of this new type of source rather than to yield precise event-rate predictions-we find that such detectors could observe a few to a few tens of seed black hole merger events in three years and provide possibly unique information on the evolution of structure in the corresponding era. We show further that a network of detectors may be able to measure the luminosity distance to sources to a precision of similar to 40\%, allowing us to be confident of the high-redshift nature of the sources.}}, DOI = {{10.1088/0004-637X/698/2/L129}}, ISSN = {{2041-8205}}, EISSN = {{2041-8213}}, ResearcherID-Numbers = {{Sesana, Alberto/Q-9826-2016 Vecchio, Alberto/F-8310-2015}}, ORCID-Numbers = {{Sesana, Alberto/0000-0003-4961-1606 Vecchio, Alberto/0000-0002-6254-1617}}, Unique-ID = {{ISI:000267052600013}}, } @article{ ISI:000264762500006, Author = {Regimbau, T. and Hughes, Scott A.}, Title = {{Gravitational-wave confusion background from cosmological compact binaries: Implications for future terrestrial detectors}}, Journal = {{PHYSICAL REVIEW D}}, Year = {{2009}}, Volume = {{79}}, Number = {{6}}, Month = {{MAR}}, Abstract = {{Increasing the sensitivity of a gravitational-wave (GW) detector improves our ability to measure the characteristics of detected sources. It also increases the number of weak signals that contribute to the data. Because GW detectors have nearly all-sky sensitivity, they can be subject to a confusion limit: Many sources which cannot be distinguished may be measured simultaneously, defining a stochastic noise floor to the sensitivity. For GW detectors operating at present and for their planned upgrades, the projected event rate is sufficiently low that we are far from the confusion-limited regime. However, some detectors currently under discussion may have large enough reach to binary inspiral that they enter the confusion-limited regime. In this paper, we examine the binary inspiral confusion limit for terrestrial detectors. We consider a broad range of inspiral rates in the literature, several planned advanced gravitational-wave detectors, and the highly advanced ``Einstein telescope{''} design. Though most advanced detectors will not be impacted by this limit, the Einstein telescope with a very low-frequency ``seismic wall{''} may be subject to confusion noise. At a minimum, careful data analysis will be require to separate signals which will appear confused. This result should be borne in mind when designing highly advanced future instruments.}}, DOI = {{10.1103/PhysRevD.79.062002}}, Article-Number = {{062002}}, ISSN = {{1550-7998}}, EISSN = {{1550-2368}}, Unique-ID = {{ISI:000264762500006}}, } @article{ ISI:000263061600013, Author = {Cokelaer, T. and Pathak, D.}, Title = {{Searching for gravitational-wave signals emitted by eccentric compact binaries using a non-eccentric template bank: implications for ground-based detectors}}, Journal = {{CLASSICAL AND QUANTUM GRAVITY}}, Year = {{2009}}, Volume = {{26}}, Number = {{4}}, Month = {{FEB 21}}, Abstract = {{Most of the inspiralling compact binaries are expected to be circularized by the time their gravitational-wave signals enter the frequency band of ground-based detectors such as LIGO or VIRGO. However, it is not excluded that some of these binaries might still possess a significant eccentricity at a few tens of hertz. Despite this possibility, current search pipelines-based on matched filtering techniques-consider only non-eccentric templates. The effect of such an approximation on the loss of signal-to-noise ratio (SNR) has been investigated by Martel and Poisson (1999 Phys. Rev. D 60 124008) in the context of initial LIGO detector. They ascertained that non- eccentric templates will be successful at detecting eccentric signals. We revisit their work by incorporating current and future ground-based detectors and precisely quantify the exact loss of SNR. In order to be more faithful to an actual search, we maximized the SNR over a template bank, whose minimal match is set to 95\%. For initial LIGO detector, we claim that the initial eccentricity does not need to be taken into account in our searches for any system with total mass M is an element of {[}2-45] M circle dot if e(0) less than or similar to 0.05 because the loss of SNR (about 5\%) is consistent with the discreteness of the template bank. Similarly, this statement is also true for systems with M is an element of {[}6-35] M circle dot and e(0) less than or similar to 0.10. However, by neglecting the eccentricity in our searches, significant loss of detection ( larger than 10\%) may arise as soon as e(0) >= 0.05 for neutron-star binaries. We also provide exhaustive results for VIRGO, Advanced LIGO and Einstein Telescope detectors. It is worth noting that for Einstein Telescope, neutron star binaries with e(0) >= 0.02 lead to a 10\% loss of detection.}}, DOI = {{10.1088/0264-9381/26/4/045013}}, Article-Number = {{045013}}, ISSN = {{0264-9381}}, EISSN = {{1361-6382}}, ResearcherID-Numbers = {{Cokelaer, Thomas/AAN-8240-2020 Pathak, Devanka/B-7833-2017}}, ORCID-Numbers = {{Cokelaer, Thomas/0000-0001-6286-1138 Pathak, Devanka/0000-0002-1768-8353}}, Unique-ID = {{ISI:000263061600013}}, }