COMPACT BINARY MERGER RATES: COMPARISON WITH LIGO/VIRGO UPPER LIMITS

By Krzysztof Belczyński, S. Repetto, D. Holz, R. O’Shaughnessy, T. Bulik, Emanuele Berti, Chris L. Fryer, M. Dominik. 2015

156 citations recorded by the source corpus.

We compare evolutionary predictions of double compact object merger rate densities with initial and forthcoming LIGO/Virgo upper limits. We find that: (i) Due to the cosmological reach of advanced detectors, current conversion methods of population synthesis predictions into merger rate densities are insufficient. (ii) Our optimistic models are a factor of 18 below the initial LIGO/Virgo upper limits for BH–BH systems, indicating that a modest increase in observational sensitivity (by a factor of ∼2.5) may bring the first detections or first gravitational wave constraints on binary evolution. (iii) Stellar-origin massive BH–BH mergers should dominate event rates in advanced LIGO/Virgo and can be detected out to redshift z ≃ 2 with templates including inspiral, merger, and ringdown. Normal stars ( < 150 M ⊙ ?> ) can produce such mergers with total redshifted mass up to M tot,z ≃ 400 M ⊙ ?> . (iv) High black hole (BH) natal kicks can severely limit the formation of massive BH–BH systems (both in isolated binary and in dynamical dense cluster evolution), and thus would eliminate detection of these systems even at full advanced LIGO/Virgo sensitivity. We find that low and high BH natal kicks are allowed by current observational electromagnetic constraints. (v) The majority of our models yield detections of all types of mergers (NS–NS, BH–NS, BH–BH) with advanced detectors. Numerous massive BH–BH merger detections will indicate small (if any) natal kicks for massive BHs.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/4d54dca159ed83d9f791eb2836defee13a697e4b

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Citations in the corpus

The effect of pair-instability mass loss on black-hole mergers (2016, methodology): “This assumption about compact-object natal kicks leads to a severe reduction of BH-BH merger rates, moderate reduction of BH-NS merger rates, and small reduction of NS-NS merger rates; we consider it our pessimistic model (Belczynski et al. 2016a).”
ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, methodology): “The significance of (v) and (vi) has been discussed recently for the StarTrack(Belczynski et al. 2008a) models by Dominik et al. (2012) and Belczynski et al. (2015).”
Black Hole Mergers in Galactic Nuclei Induced by the Eccentric Kozai–Lidov Effect (2017, background): “10 And also above this natal kick the mergers of isolated binaries is significantly suppressed (Belczynski et al. 2016b) Recently, Bartos et al. (2017) showed that with a big enough sample of observed BH-BH mergers, a certain BH-BH merger channel can be statistically correlated with rare galaxy…”
The origin of spin in binary black holes (2019, methodology): “To compute the detected BH merger rate by GW detectors, we follow a similar procedure to the one of Belczynski et al. (2016b) which is a refined version of Dominik et al. (2015).”
The Origin of r-process Elements in the Milky Way (2017, methodology): “This involves tracing the formation of NS-NS progenitor systems according to the cosmic star formation history (CSFH, Madau & Dickinson 2014) and following their evolution until they merge using metallicity-dependent delay-time distributions (DTDs, see Belczynski et al. 2016b).”
Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, unknown): “…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), Bartos et al. (2017), McKernan et al. (2017), Stone et al. (2017), Hoang et…”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, unknown): “…pulsar (7 − 49 Myr−1, Kim et al. 2015), somewhat on the higher end of the rates computed in de Mink & Belczynski (2015) (1.4 − 81 Myr−1) and used in Belczynski et al. (2016) (5 − 15 Myr−1) for comparison with LIGO/Virgo upper limits, 0.06 − 77.4 Myr−1 in Dominik et al. (2012) and 0.01 − 80…”
Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, methodology): “8 or 9 or de Mink & Belczynski 2015; Belczynski et al. 2016a).”
MERGING BLACK HOLE BINARIES IN GALACTIC NUCLEI: IMPLICATIONS FOR ADVANCED-LIGO DETECTIONS (2016, background): “…stellar environments (e.g., Portegies Zwart & McMillan 2000; Miller & Lauburg 2009; Banerjee et al. 2010; Downing et al. 2011; Rodriguez et al. 2015), and isolated binary evolution (e.g., Belczynski et al. 2002; Dominik et al. 2012; Spera et al. 2015; Belczynski et al. 2016; de Mink & Mandel 2016).”
Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic N-body Dynamics (2018, background): “From a theoretical perspective, several formation channels have been suggested including isolated field binaries (Dominik et al. 2012, 2013, 2015; Belczynski et al. 2016b,a), dense stellar clusters (Portegies Zwart & McMillan 2000; Banerjee et al. 2010; Tanikawa 2013; Bae et al. 2014; Rodriguez et…”
Where Are LIGO’s Big Black Holes? (2017, methodology): “Before accounting for PPISN or PISN, previous population-synthesis predictions placed the maximum BH mass at 80–135M for zero age main sequence masses MZAMS < 150M (Belczynski et al. 2016c; Eldridge & Stanway 2016; Spera et al. 2016).”
Binary Black Hole Mergers from Field Triples: Properties, Rates, and the Impact of Stellar Evolution (2017, background): “Binary BHs can form as the result of: (i) the evolution of isolated massive binaries in galactic fields (Belczynski et al. 2010, 2016; Mandel & de Mink 2016); (ii) dynamical interactions in galactic nuclei, with and without a massive BH (Antonini & Perets 2012; Antonini & Rasio 2016); (iii)…”
Double neutron stars: merger rates revisited (2017, methodology): “Methods in Belczynski et al. (2016a) for the full list).”