The cosmic merger rate density of compact objects: impact of star formation, metallicity, initial mass function, and binary evolution

Santoliquido, Filippo; Mapelli, Michela; Giacobbo, Nicola; Bouffanais, Y.; Artale, M. Celeste

doi:10.1093/mnras/stab280

Cited by 147 publications

(141 citation statements)

References 131 publications

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“…Together with another candidate of a black hole-neutron star binary merger GW190426_152155 (Abbott et al 2021a), we may now safely consider that black hole-neutron star binaries are actually merging in our Universe. The merger rate is currently inferred to be % 12-240 Gpc À3 yr À1 , which is largely consistent with previous theoretical estimation (Dominik et al 2015;Kruckow et al 2018;Neijssel et al 2019;Zevin et al 2020;Santoliquido et al 2021, see also Narayan et al 1991;Phinney 1991 for pioneering rate estimation). Unfortunately, despite the presence of neutron stars, no associated electromagnetic counterpart was detected.…”

supporting

confidence: 87%

Coalescence of black hole–neutron star binaries

2021

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We review the current status of general relativistic studies for coalescences of black hole–neutron star binaries. First, high-precision computations of black hole–neutron star binaries in quasiequilibrium circular orbits are summarized, focusing on the quasiequilibrium sequences and the mass-shedding limit. Next, the current status of numerical-relativity simulations for the merger of black hole–neutron star binaries is described. We summarize our understanding for the merger process, tidal disruption and its criterion, properties of the merger remnant and ejected material, gravitational waveforms, and gravitational-wave spectra. We also discuss expected electromagnetic counterparts to black hole–neutron star coalescences.

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supporting

confidence: 87%

Coalescence of black hole–neutron star binaries

2021

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“…We find a mild preference for efficient CEs in our modeling, which strongly disfavors highly inefficient CEs with α CE 0.2. Inferred values for the CE efficiency α CE have more diversity than natal spins across the literature, from population modeling (e.g., Bavera et al 2020a;Santoliquido et al 2021;Zevin et al 2020) to hydrodynamical simulations (e.g., Fragos et al 2019) and theoretical considerations (e.g., Ivanova et al 2013). Our results, which mildly favor high CE efficiencies, are in agreement with Santoliquido et al (2021), who found high CE efficiencies are necessary to match the merger rate of binary neutron stars in their population models, and with Fragos et al (2019), who modeled the spiral-in phase of CE evolution using hydrodynamic simulations and found a non-negligible fraction of the envelope remains bound to the core after the CE is successfully ejected.…”

Section: Discussionmentioning

confidence: 99%

“…Inferred values for the CE efficiency α CE have more diversity than natal spins across the literature, from population modeling (e.g., Bavera et al 2020a;Santoliquido et al 2021;Zevin et al 2020) to hydrodynamical simulations (e.g., Fragos et al 2019) and theoretical considerations (e.g., Ivanova et al 2013). Our results, which mildly favor high CE efficiencies, are in agreement with Santoliquido et al (2021), who found high CE efficiencies are necessary to match the merger rate of binary neutron stars in their population models, and with Fragos et al (2019), who modeled the spiral-in phase of CE evolution using hydrodynamic simulations and found a non-negligible fraction of the envelope remains bound to the core after the CE is successfully ejected. These results for α CE contrast with those from Bavera et al (2020a), but we find that these conflicting results arise only from the consideration of more forma-tion channels in this work; when considering contributions from only the CE and SMT channels, we also favor low CE efficiencies of α CE 0.5.…”

Section: Discussionmentioning

confidence: 99%

One Channel to Rule Them All? Constraining the Origins of Binary Black Holes Using Multiple Formation Pathways

Zevin

Bavera

Berry

et al. 2021

ApJ

272

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The second LIGO-Virgo catalog of gravitational-wave (GW) transients has more than quadrupled the observational sample of binary black holes. We analyze this catalog using a suite of five state-of-the-art binary black hole population models covering a range of isolated and dynamical formation channels and infer branching fractions between channels as well as constraints on uncertain physical processes that impact the observational properties of mergers. Given our set of formation models, we find significant differences between the branching fractions of the underlying and detectable populations, and that the diversity of detections suggests that multiple formation channels are at play. A mixture of channels is strongly preferred over any single channel dominating the detected population: an individual channel does not contribute to more than 70% of the observational sample of binary black holes. We calculate the preference between the natal spin assumptions and common-envelope efficiencies in our models, favoring natal spins of isolated black holes of 0.1, and marginally preferring common-envelope efficiencies of 2.0 while strongly disfavoring highly inefficient common envelopes. We show that it is essential to consider multiple channels when interpreting GW catalogs, as inference on branching fractions and physical prescriptions becomes biased when contributing formation scenarios are not considered or incorrect physical prescriptions are assumed. Although our quantitative results can be affected by uncertain assumptions in model predictions, our methodology is capable of including models with updated theoretical considerations and additional formation channels.

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“…The details of these results might strongly depend on the star formation rate and metallicity evolution model, which can deeply change the merger rate [36,38,193,194]. We will investigate the impact of these quantities in a follow-up study.…”

Section: Comparison With Bbhs In Gwtc-2mentioning

confidence: 99%

Mass and Rate of Hierarchical Black Hole Mergers in Young, Globular and Nuclear Star Clusters

et al. 2021

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Hierarchical mergers are one of the distinctive signatures of binary black hole (BBH) formation through dynamical evolution. Here, we present a fast semi-analytic approach to simulate hierarchical mergers in nuclear star clusters (NSCs), globular clusters (GCs) and young star clusters (YSCs). Hierarchical mergers are more common in NSCs than they are in both GCs and YSCs because of the different escape velocity. The mass distribution of hierarchical BBHs strongly depends on the properties of first-generation BBHs, such as their progenitor’s metallicity. In our fiducial model, we form black holes (BHs) with masses up to ∼103 M⊙ in NSCs and up to ∼102 M⊙ in both GCs and YSCs. When escape velocities in excess of 100 km s−1 are considered, BHs with mass >103 M⊙ are allowed to form in NSCs. Hierarchical mergers lead to the formation of BHs in the pair instability mass gap and intermediate-mass BHs, but only in metal-poor environments. The local BBH merger rate in our models ranges from ∼10 to ∼60 Gpc−3 yr−1; hierarchical BBHs in NSCs account for ∼10−2–0.2 Gpc−3 yr−1, with a strong upper limit of ∼10 Gpc−3 yr−1. When comparing our models with the second gravitational-wave transient catalog, we find that multiple formation channels are favored to reproduce the observed BBH population.

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The cosmic merger rate density of compact objects: impact of star formation, metallicity, initial mass function, and binary evolution

Cited by 147 publications

References 131 publications

Coalescence of black hole–neutron star binaries

Coalescence of black hole–neutron star binaries

One Channel to Rule Them All? Constraining the Origins of Binary Black Holes Using Multiple Formation Pathways

Mass and Rate of Hierarchical Black Hole Mergers in Young, Globular and Nuclear Star Clusters

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