Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave

By T. Kinugawa, Kohei Inayoshi, K. Hotokezaka, Daisuke Nakauchi, Takashi Nakamura. 2014

224 citations recorded by the source corpus.

We perform population synthesis simulations for Population III (Pop III) coalescing binary neutron stars (NS-NSs), neutron star - black hole binaries (NS-BHs), and binary black holes (BH-BHs) which merge within the age of the universe. We found that the typical mass of Pop III BH-BHs is $\sim 30\ \rm{M}_{\odot}$ so that the inspiral chirp signal of gravitational waves can be detected up to z=0.28 by KAGRA, Adv. LIGO, Adv. Virgo and GEO network. Our simulations suggest that the detection rate of the coalescing Pop III BH-BHs is $140 (68) \cdot ({\rm SFR}_{\rm p}/10^{-2.5} \rm{M}_{\odot} {\rm yr}^{-1} {\rm Mpc}^{-3}) \cdot {\rm Err}_{\rm sys} ~{\rm events} ~{\rm yr}^{-1}$ for the flat (Salpeter) initial mass function (IMF), respectively, where $\rm SFR_p$ and $\rm Err_{sys}$ are the peak value of the Pop III star formation rate and the possible systematic errors due to the assumptions in Pop III population synthesis, respectively. $\rm Err_{sys}=1$ correspond to conventional parameters for Pop I stars. From the observation of the chirp signal of the coalescing Pop III BH-BHs, we can determine both the mass and the redshift of the binary for the cosmological parameters determined by Planck satellite. Our simulations suggest that the cumulative redshift distribution of the coalescing Pop III BH-BHs depends almost only on the cosmological parameters. We might be able to confirm the existence of Pop III massive stars of mass $\sim 30~\rm M_{\odot}$ by the detections of gravitational waves if the merger rate of the Pop III massive BH-BHs dominates that of Pop I BH-BHs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ede1fa4e1409a75643b8f7c3b8b3f9037c5b8819

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1. Michela Mapelli
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Citations in the corpus

• The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, result): “We refer to other studies (e.g. Kinugawa et al. 2014, 2016; Belczynski et al. 2016a; Hartwig et al. 2016; Inayoshi et al. 2017) for a more accurate treatment of BHBs from population III stars.”
• One Channel to Rule Them All? Constraining the Origins of Binary Black Holes Using Multiple Formation Pathways (2020, background): “Extremely low-metallicity Population III stars in binary systems have also been proposed for forming the high-mass BBH mergers observed (Madau & Rees 2001; Kinugawa et al. 2014; Inayoshi et al. 2017).”
• Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. (2016, background): “For instance, a scenario based on Population III binaries also explains the high event rate with the peak of the BH mass distribution around ∼ 30 M⊙ [17, 18] (see also [19]).”
• The effect of pair-instability mass loss on black-hole mergers (2016, background): “Additionally, Population III stars have also been considered as possible venues for BH-BH formation and gravitational wave detection for over thirty years (Bond et al. 1984; Belczynski et al. 2004; Kinugawa et al. 2014).”
• Binary Black Hole Mergers in the First Advanced LIGO Observing Run (2016, background): “[168–173]), possibly from population III binaries [174,175], or chemically homogeneous evolution in close tidally locked binaries [176,177].”
• Primordial black holes as generators of cosmic structures (2018, background): “…LIGO might detect gravitational waves from coalescing intermediate mass Population III black holes was first made by Bond & Carr (1984) more than 30 years ago and - rather remarkably - Kinugawa et al. (2014) predicted a Population III coalescence peak at 30M shortly before the first LIGO detection.”
• Solving puzzles of GW150914 by primordial black holes (2016, result): “However, the contribution of PopIII stars to the formation of BH binaries with masses ∼ 30 + 30M can be negligible, contradicting the population synthesis results [12, 13].”
• Building up the Population III initial mass function from cosmological initial conditions (2016, background): “(e.g. Abbott et al. 2016; Kinugawa et al. 2014; Kowalska et al. 2012; Belczynski et al. 2004; Hartwig et al. 2016; Inayoshi et al. 2016).”
• Assisted inspirals of stellar mass black holes embedded in AGN discs: solving the ‘final au problem’ (2016, background): “…a massive main sequence binary and resulting homogeneous stellar evolution has recently been proposed (Mandel & de Mink 2016; Marchant et al. 2016), which predicts a rate of ∼ 10 Gpc−3 yr−1; a similar rate has been predicted at z ≈ 0 from PopIII stellar remnant BH binaries (Kinugawa et al. 2014).”
• ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “…binaries are not very different from binary populations in the local universe (admittedly a considerable extrapolation), then recently predicted BBH total masses agree astonishingly well with GW150914 and can have sufficiently long merger times to occur in the nearby universe(Kinugawa et al. 2014).”
• Does the Black Hole Merger Rate Evolve with Redshift? (2018, background): “It has also been proposed that the progenitors of BBHs are Population III stars formed at zero metallicity, in which case we might expect an even steeper increase of the merger rate with increasing redshift (Belczynski et al. 2004; Kinugawa et al. 2014).”
• Primordial Black Holes as Dark Matter: Recent Developments (2020, background): “predicted a Population III coalescence peak at 30M shortly before the first LIGO detection of black holes of that mass [41].”
• Formation and Evolution of Compact-object Binaries in AGN Disks (2019, methodology): “Possible compact-object merger pathways include isolated binary evolution (Dominik et al. 2012; Kinugawa et al. 2014; Belczynski et al. 2016, 2017; Breivik et al. 2016; Giacobbo et al. 2018; Bavera et al. 2019; Spera et al. 2019) accompanied by mass transfer (Inayoshi et al. 2017a; Pavlovskii et…”
• Black Hole Mergers in Galactic Nuclei Induced by the Eccentric Kozai–Lidov Effect (2017, background): “Some studies also suggested that these LIGO detections are sourced in the first stars (Kinugawa et al. 2014, 2016; Hartwig et al. 2016; Inayoshi et al. 2016; Dvorkin et al. 2016), cores of massive stars (Reisswig et al. 2013; Loeb 2016; Woosley 2016), or dark matter halos comprised of primordial…”
• Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, background): “…these rates: see Abadie et al. (2010) for a partial list of historical compact binary coalescence rate predictions, and Dominik et al. (2013), Kinugawa et al. (2014), Abbott et al. (2016a, 2016b, 2016f, 2016g, 2016h), Belczynski et al. (2016), Rodriguez et al. (2016a), Sasaki et al. (2016),…”