Gravitational-wave constraints on the GWTC-2 events by measuring the tidal deformability and the spin-induced quadrupole moment

Narikawa, Tatsuya; Uchikata, Nami; Tanaka, Takahiro

doi:10.48550/arxiv.2106.09193

Cited by 4 publications

(5 citation statements)

References 87 publications

(137 reference statements)

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“…In Refs. [78,79], observational constraint on spin induced quadrupole moment has been found. Individual measurement suffers from broad posterior distribution, pointing towards low measurability with current detectors.…”

Section: B New Waveform Parameters Characterizing Quadrupole Momentmentioning

confidence: 94%

Recognizing black holes in gravitational-wave observations: Challenges in telling apart impostors in mass-gap binaries

2021

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We study how by careful monitoring of the presence or absence of tidal deformability (TD) and tidalheating (TH) in the inspiral signal of compact object binaries in ground-based gravitational wave (GW) detectors, one can test if its components are black holes or not. The former property (TD) is finite for neutron stars but vanishes for black holes (in general relativity), whereas the latter is finite for black holes and negligible for neutron stars, and affects the GW phase evolution of binaries in a distinctly different way. We introduce waveform parameters that characterize the strength of tidal-heating and are zero when there is no horizon. We develop Bayesian methods that use TD and TH for distinguishing the presence or absence of horizons in a binary. This is timely owing to several claims that these stellar-mass objects, especially, with masses heavier than those of neutron stars, may not have a horizon but may be black hole mimickers or exotic compact objects (ECOs). It is also astrophysically important to have the tools to test the presence or absence of horizons in mass-gap binaries and, thereby, help detect the heaviest neutron star or the lightest black hole. A proper accounting of tidal-heating in binary waveform models will also be critical for an unbiased measurement of characteristics of the equation of state of neutron stars in GW observations of binaries containing them-or even to probe the existence of ECOs. We show that purely based on GW waveforms it will not be possible to discern binary horizons in the mass gap in Advanced LIGO, Virgo and KAGRA detectors unless the binary is within a few tens of Mpc. However, third generation ground-based detectors will be able to do so for binaries a few hundred Mpc away.

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Section: B New Waveform Parameters Characterizing Quadrupole Momentmentioning

confidence: 94%

Recognizing black holes in gravitational-wave observations: Challenges in telling apart impostors in mass-gap binaries

2021

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“…[31] have derived the complete and correct form up to 2.5PN order (relative 5+2.5PN order) for the mass quadrupole, current quadrupole, and mass octupole contributing to the GW tidal phase Ψ PNTidal (f ). We rewrite it for the mass quadrupole interactions to use data analysis as a function of the dimensionless tidal deformability of each object Λ 1,2 by [32]…”

Section: B Waveform Models For Inspiraling Binary Neutron Starsmentioning

confidence: 99%

“…Recently, the complete and correct PN tidal phase up to 5+2.5PN order for mass quadrupole, mass octupole, and current quadrupole interactions have been derived by the PN-matched multiplolar-post-Minkowskian formalism [31]. In our previous study [32], we rewrite the the complete and correct form for the mass quadrupole interactions as a function of the dimensionless tidal deformability for the individual stars, Λ, in a convenient way for data analyses. And we have reanalyzed the data around low-mass events identified as binary black holes (BBHs) by using the corrected version of the PNTidal model to test the exotic compact object hypothesis.…”

Section: Introductionmentioning

confidence: 99%

Follow-up analyses of the binary-neutron-star signals GW170817 and GW190425 by using post-Newtonian waveform models

Narikawa¹,

Uchikata²

2022

Preprint

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We reanalyze the binary-neutron-star signals, GW170817 and GW190425, focusing on the inspiral regime to avoid uncertainties on waveform modeling in the postinspiral regime. We use post-Newtonian waveform models as templates, which are theoretically rigid and efficiently describe the inspiral regime. We study potential systematic difference in estimates of the binary tidal deformability Λ by using different descriptions for the point-particle dynamics and tidal effects. We find that the estimates of Λ show no significant systematic difference among three models for the point-particle parts: TF2, TF2g, and TF2+, when they employ the same tidal model. We compare different tidal descriptions given by different post-Newtonian orders in the tidal phase. Our results indicate that the estimates of Λ slightly depend on the post-Newtonian order in the tidal phase and an increase in the tidal post-Newtonian order does not lead to a monotonic change in the estimate of Λ. We also compare the estimate of Λ obtained by the post-Newtonian tidal model and numerical-relativity calibrated tidal models. We find that the post-Newtonian model gives slightly larger estimate of Λ and wider posterior distribution than the numerical-relativity calibrated models. According to Bayesian model comparison, it is difficult to identify a preference among the post-Newtonian orders by relying on the GW170817 and GW190425 data. Our results indicate no preference among numerical-relativity calibrated tidal models over the post-Newtonian model. Additionally, we present constraints on equation-of-state models for neutron stars with the post-Newtonian model, which show that the GW170817 data disfavor less compact models, though they are slightly weaker constraints than the numerical-relativity calibrated tidal models.

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“…Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. [10,[12][13][14][15][16][17][18][19][20][21][22], multipole moments [12,[23][24][25][26][27], echoes in postmerger [28][29][30][31][32][33][34][35][36] and electromagnetic observations [34,[37][38][39][40] has been proposed in the literature.…”

Section: Introductionmentioning

confidence: 99%

Probing horizon scale quantum effects with Love

Datta

2022

Class. Quantum Grav.

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Future gravitational wave detectors have been projected to be able to probe the nature of compact objects in great detail. In this work, we study the potential observability of the small length scale physics near black hole horizon with the tidal deformability of the compact objects in an inspiraling binary. We find that it is possible to probe them with extreme mass ratio inspirals. We discuss how the quantum effects can affect the gravitational wave observables. This as a consequence is bound to shape our understanding of the quantum scale near the horizon.

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Gravitational-wave constraints on the GWTC-2 events by measuring the tidal deformability and the spin-induced quadrupole moment

Cited by 4 publications

References 87 publications

Recognizing black holes in gravitational-wave observations: Challenges in telling apart impostors in mass-gap binaries

Recognizing black holes in gravitational-wave observations: Challenges in telling apart impostors in mass-gap binaries

Follow-up analyses of the binary-neutron-star signals GW170817 and GW190425 by using post-Newtonian waveform models

Probing horizon scale quantum effects with Love

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