How to confirm the existence of population III stars by observations of gravitational waves

Miyamoto, A.; Kinugawa, Tomoya; Nakamura, Takashi; Kanda, Nobuyuki

doi:10.1103/physrevd.96.064025

Cited by 10 publications

(9 citation statements)

References 40 publications

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“…Conversely, we provide simple approaches to extend our phenomenological approach in sophistication and complexity as several thousand compact binary mergers provide sharp constraints on their underlying properties. This approach complements inferences that work within a concrete model family as explored in other proof-of-concept investigations (see, e.g., [16,17,[23][24][25][26][27][28] and references therein).…”

Section: Introductionmentioning

confidence: 86%

Reconstructing phenomenological distributions of compact binaries via gravitational wave observations

2019

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Gravitational wave measurements will provide insight into the population of coalescing compact binaries throughout the universe. We describe and demonstrate a flexible parametric method to infer the event rate as a function of compact binary parameters, accounting for Poisson error and selection biases. Using synthetic data based on projections for LIGO and Virgo's third observing run (O3), we discuss how well GW measurements could constrain the mass and spin distribution of coalescing neutron stars and black holes in the near future, within the context of several phenomenological models described in this work. We demonstrate that only a few tens of events can enable astrophysically significant constraints on the spin magnitude and orientation distribution of BHs in merging binaries. We discuss how astrophysical priors or other measurements can inform the interpretation of future measurements. Using publicly-available results, we estimate the event rate versus mass for binary black holes. To connect to previously-published work, we provide estimates including reported O2 BBH candidates, making several unwarranted but simplifying assumptions for the sensitivity of the network and completeness of the reported set of events. Consistent with prior work, we find BHs in binaries likely have low natal spin. With available results and a population favoring low spin, we can't presently constrain the typical misalignments of the binary black hole population. All of the tools described in this work are publicly available and ready-to-use to interpret real or synthetic LIGO data, and to synthesize projected data from future observing runs. a I. * dw2081@rit.edu a https://git.ligo.org/daniel.wysocki/bayesianparametric-population-models/ and https://git.ligo.org/daniel.wysocki/synthetic-PE-posteriors

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Section: Introductionmentioning

confidence: 86%

Reconstructing phenomenological distributions of compact binaries via gravitational wave observations

2019

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“…In this paper, we consider only the inspiral phase of gravitational waves to compute the expected signal-to-noise ratio for simplicity. This assumption has also been used in the literature to discuss detectabilities of binary BH mergers in future detectors (e.g., Taylor & Gair 2012;Miyamoto et al 2017;Li et al 2018). In this case, the signal-to-noise ratio ρ of binary BH mergers with masses m1 and m2 is computed as (Finn 1996)…”

Section: Signal-to-noise Ratiomentioning

confidence: 99%

Effect of gravitational lensing on the distribution of gravitational waves from distant binary black hole mergers

Oguri

2018

Monthly Notices of the Royal Astronomical Society

150

179

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The detailed observation of the distribution of redshifts and chirp masses of binary black hole mergers is expected to provide a clue to their origin. In this paper, we develop a hybrid model of the probability distribution function of gravitational lensing magnification taking account of both strong and weak gravitational lensing, and use it to study the effect of gravitational lensing magnification on the distribution of gravitational waves from distant binary black hole mergers detected in ongoing and future gravitational wave observations. We find that the effect of gravitational lensing magnification is significant at high ends of observed chirp mass and redshift distributions. While a high mass tail in the observed chirp mass distribution is produced by highly magnified gravitational lensing events, we find that highly demagnified images of strong lensing events produce a high redshift (z obs 15) tail in the observed redshift distribution, which can easily be observed in the third-generation gravitational wave observatories. Such a demagnified, apparently high redshift event is expected to be accompanied by a magnified image that is observed typically 10 − 100 days before the demagnified image. For highly magnified events that produce apparently very high chirp masses, we expect pairs of events with similar magnifications with time delays typically less than a day. This work suggests the critical importance of gravitational lensing (de-)magnification on the interpretation of apparently very high mass or redshift gravitational wave events.

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“…The mechanism by which these black holes came to be in binaries is unknown, although a variety of formation scenarios have been proposed. Recent work investigates how measurements of black hole mass and spin distributions can elucidate the population properties of binary black holes [11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29]. It has also been suggested that the future Laser Interferometer Space Antenna (LISA) will be able to observe nearby stellar-mass BBH during the early inspiral phase.…”

Section: Introductionmentioning

confidence: 99%

Measuring eccentricity in binary black hole inspirals with gravitational waves

et al. 2018

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When binary black holes form in the field, it is expected that their orbits typically circularize before coalescence. In galactic nuclei and globular clusters, binary black holes can form dynamically. Recent results suggest that ≈ 5% of mergers in globular clusters result from three-body interactions. These three-body interactions are expected to induce significant orbital eccentricity 0.1 when they enter the Advanced LIGO and Virgo band at a gravitational-wave frequency of 10 Hz. Measurements of binary black hole eccentricity therefore provide a means for determining whether or not dynamic formation is the primary channel for producing binary black hole mergers. We present a framework for performing Bayesian parameter estimation on gravitational-wave observations of eccentric black hole inspirals. Using this framework, and employing the nonspinning, inspiral-only EccentricFD waveform approximant, we determine the minimum detectable eccentricity for an event with masses and distance similar to GW150914. At design sensitivity, we find that the current generation of advanced observatories will be sensitive to orbital eccentricities of 0.05 at a gravitational-wave frequency of 10 Hz, demonstrating that existing detectors can use eccentricity to distinguish between circular field binaries and globular cluster triples. We compare this result to eccentricity distributions predicted to result from three black hole binary formation channels, showing that measurements of eccentricity could be used to infer the population properties of binary black holes. arXiv:1806.05350v3 [astro-ph.HE] 1 Nov 2018

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How to confirm the existence of population III stars by observations of gravitational waves

Cited by 10 publications

References 40 publications

Reconstructing phenomenological distributions of compact binaries via gravitational wave observations

Reconstructing phenomenological distributions of compact binaries via gravitational wave observations

Effect of gravitational lensing on the distribution of gravitational waves from distant binary black hole mergers

Measuring eccentricity in binary black hole inspirals with gravitational waves

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