Compact Binary Merger Rates: Comparison With Ligo/Virgo Upper Limits

Belczyński, Krzysztof; Repetto, Serena; Holz, D. E.; O’Shaughnessy, R.; Bulik, T.; Berti, Emanuele; Fryer, Christopher L.; Dominik, M.

doi:10.3847/0004-637x/819/2/108

Cited by 260 publications

(298 citation statements)

References 150 publications

(310 reference statements)

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“…If the stars start too close, they may merge before both black holes are formed. In addition, the core collapse that forms a black hole can impart a kick of tens of km s −1 or more to the hole (see, e.g., [111,112] for recent discussions), which might unbind the binary.…”

Section: Isolated Binariesmentioning

confidence: 99%

“…These effects are incorporated in parameterized ways in various binary population synthesis codes (e.g., [113,114,115,111]; see [116] for a recent discussion of the evolution of compact binaries). The simulators are in a difficult position because massive stars are rare, and because some of the key phases of the evolution are extremely tough to observe, which means that there is reliance on our often-incomplete theoretical understanding of the relevant processes.…”

Section: Isolated Binariesmentioning

confidence: 99%

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Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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Section: Isolated Binariesmentioning

confidence: 99%

Section: Isolated Binariesmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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“…Spera et al, oelbert@uci.edu 2015; Belczynski et al, 2010, and references therein), and have been predicted to dominate the LIGO signal (e.g. Belczynski et al, 2016b). However, the possibility that the GW150914 event was due to primordial black holes (that would constitute some part of the dark matter) has also been advanced Cholis et al, 2016;Carr et al, 2016;Inomata et al, 2016).…”

Section: Introductionmentioning

confidence: 99%

“…Lamberts et al (2016) concluded that the black holes involved in GW150914 likely formed in a massive galaxy at z ∼ 1, but that formation in a dwarf galaxy was also likely possible. Belczynski et al (2016b) suggested that the black holes likely form in low-metallicity systems. Chatterjee et al (2017) explored the formation of BBH systems specifically in globular clusters and came to qualitatively similar conclusions.…”

Section: Introductionmentioning

confidence: 99%

Counting black holes: The cosmic stellar remnant population and implications for LIGO

Elbert

Bullock

Kaplinghat

2017

Monthly Notices of the Royal Astronomical Society

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We present an empirical approach for interpreting gravitational wave signals of binary black hole mergers under the assumption that the underlying black hole population is sourced by remnants of stellar evolution. Using the observed relationship between galaxy mass and stellar metallicity, we predict the black hole count as a function of galaxy stellar mass. We show, for example, that a galaxy like the Milky Way should host millions of ∼ 30 M black holes and dwarf satellite galaxies like Draco should host ∼ 100 such remnants, with weak dependence on the assumed IMF and stellar evolution model. Most low-mass black holes (∼ 10M ) typically reside within massive galaxies (M 10 11 M ) while massive black holes (∼ 50 M ) typically reside within dwarf galaxies (M 10 9 M ) today. If roughly 1% of black holes are involved in a binary black hole merger, then the reported merger rate densities from Advanced LIGO can be accommodated for a range of merger timescales, and the detection of mergers with > 50 M black holes should be expected within the next decade. Identifying the host galaxy population of the mergers provides a way to constrain both the binary neutron star or black hole formation efficiencies and the merger timescale distributions; these events would be primarily localized in dwarf galaxies if the merger timescale is short compared to the age of the universe and in massive galaxies otherwise. As more mergers are detected, the prospect of identifying the host galaxy population, either directly through the detection of electromagnetic counterparts of binary neutron star mergers or indirectly through the anisotropy of the events, will become a realistic possibility.

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“…These discoveries verified earlier predictions that: (i) the first detection would happen when LIGO sensitivity reaches d nsns = 50-100 Mpc, that (ii) BH-BH mergers would dominate the gravitational-wave signal, and that (iii) the merging black holes would be substantially more massive than typical 10 M ⊙ A&A proofs: manuscript no. ms Galactic BHs (Belczynski et al 2010b;Dominik et al 2015;Belczynski et al 2016b).…”

Section: Introductionmentioning

confidence: 99%

The effect of pair-instability mass loss on black-hole mergers

Belczyński

Heger

Gładysz

et al. 2016

A&A

438

426

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Context. Mergers of two stellar origin black holes are a prime source of gravitational waves and are under intensive investigation. One crucial ingredient in their modeling has been neglected: pair-instability pulsation supernovae with associated severe mass loss may suppress the formation of massive black holes, decreasing black hole merger rates for the highest black hole masses. Aims. We demonstrate the effects of pair-instability pulsation supernovae on merger rate and mass using populations of double black hole binaries formed through the isolated binary classical evolution channel. Methods. The mass loss from pair-instability pulsation supernova is estimated based on existing hydrodynamical calculations. This mass loss is incorporated into the StarTrack population synthesis code. StarTrack is used to generate double black hole populations with and without pair-instability pulsation supernova mass loss. Results. The mass loss associated with pair-instability pulsation supernovae limits the Population I/II stellar-origin black hole mass to 50 M ⊙ , in tension with earlier predictions that the maximum black hole mass could be as high as 100 M ⊙ . In our model, neutron stars form with mass 1-2 M ⊙ , then we encounter the first mass gap at 2-5 M ⊙ with an absence of compact objects due to rapid supernova explosions, followed by the formation of black holes with mass 5-50 M ⊙ , with a second mass gap at 50-135 M ⊙ created by pairinstability pulsation supernovae and by pair-instability supernovae. Finally, black holes having masses above 135 M ⊙ may potentially form to arbitrarily high mass limited only by the extent of the initial mass function and the strength of stellar winds. Suppression of double black hole merger rates by pair-instability pulsation supernovae is negligible for our evolutionary channel. Our standard evolutionary model with the inclusion of pair-instability pulsation supernovae and pair-instability supernovae is fully consistent with the LIGO observations of black hole mergers: GW150914, GW151226, and LVT151012. The LIGO results are inconsistent with high ( 400 km s −1 ) BH natal kicks. We predict the detection of several, and up to as many as ∼ 60, BH-BH mergers with a total mass of 10-150 M ⊙ (most likely range: 20-80 M ⊙ ) in the forthcoming ∼ 60 effective days of the LIGO O2 observations, assuming the detectors reach the optimistic target O2 sensitivity. Conclusions.

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Compact Binary Merger Rates: Comparison With Ligo/Virgo Upper Limits

Cited by 260 publications

References 150 publications

Implications of the gravitational wave event GW150914

Implications of the gravitational wave event GW150914

Counting black holes: The cosmic stellar remnant population and implications for LIGO

The effect of pair-instability mass loss on black-hole mergers

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