Compact binaries in star clusters - II. Escapers and detection rates

Downing, J. M. B.; Benacquista, M.; Giersz, Mirek; Spurzem, Rainer

doi:10.1111/j.1365-2966.2011.19023.x

Cited by 105 publications

(115 citation statements)

References 68 publications

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“…Previous studies have explored the contribution of BBHs from GCs to the Advaned LIGO detection rate [12][13][14][15][16][17]; however, the majority of these studies have relied on either approximate analytic arguments or simpli-fied N -body models with N 10 5 particles and have assumed a single black hole mass of 10M . The one exception is [15], which used a Monte Carlo approach to model GCs of a realistic size (N = 5 × 10 5 ).…”

Section: Computing the Ratementioning

confidence: 99%

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Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO

et al. 2015

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The predicted rate of binary black hole mergers from galactic fields can vary over several orders of magnitude and is extremely sensitive to the assumptions of stellar evolution. But in dense stellar environments such as globular clusters, binary black holes form by well-understood gravitational interactions. In this letter, we study the formation of black hole binaries in an extensive collection of realistic globular cluster models. By comparing these models to observed Milky Way and extragalactic globular clusters, we find that the mergers of dynamically-formed binaries could be detected at a rate of ∼ 100 per year, potentially dominating the binary black hole merger rate. We also find that a majority of cluster-formed binaries are more massive than their field-formed counterparts, suggesting that Advanced LIGO could identify certain binaries as originating from dense stellar environments.

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Section: Computing the Ratementioning

confidence: 99%

“…The one exception is [15], which used a Monte Carlo approach to model GCs of a realistic size (N = 5 × 10 5 ). However, their study only considered GCs of a single mass, and did not extrapolate that result to the observed distribution of GCs in the local universe.…”

Section: Computing the Ratementioning

confidence: 99%

Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO

et al. 2015

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“…Here we explore the effects of our various initial assumptions on the number and properties of BBHs. Dense star clusters are expected to be efficient factories of dynamically created binary BHs (e.g., Kundu et al 2002;Pooley et al 2003;Downing et al 2010Downing et al , 2011 although at any given time the binary fraction for BHs inside the cluster remains low due to an ongoing competition between dynamical creation, and disruption and ejection of binary BHs . Table 4 lists all our models and the corresponding numbers of single and binary BHs, retained and ejected from each cluster over its lifetime.…”

Section: Bh Binariesmentioning

confidence: 99%

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

Chatterjee

Rodriguez

Rasio

2017

ApJ

127

145

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Recent N-body simulations predict that large numbers of stellar black holes (BHs) could at present remain bound to globular clusters (GCs), and merging BH-BH binaries are produced dynamically in significant numbers. We systematically vary "standard" assumptions made by numerical simulations related to, e.g., BH formation, stellar winds, binary properties of high-mass stars, and IMF within existing uncertainties, and study the effects on the evolution of the structural properties of GCs, and the BHs in GCs. We find that variations in initial assumptions can set otherwise identical initial clusters on completely different evolutionary paths, significantly affecting their present observable properties, or even affecting the cluster's very survival to the present. However, these changes usually do not affect the numbers or properties of local BH-BH mergers. The only exception is that variations in the assumed winds and IMF can change the masses and numbers of local BH-BH mergers, respectively. All other variations (e.g., in initial binary properties and binary fraction) leave the masses and numbers of locally merging BH-BH binaries largely unchanged. This is in contrast to binary population synthesis models for the field, where results are very sensitive to many uncertain parameters in the initial binary properties and binary stellar-evolution physics. Weak winds are required for producing GW150914-like mergers from GCs at low redshifts. LVT151012 can be produced in GCs modeled both with strong and weak winds. GW151226 is lower-mass than typical mergers from GCs modeled with weak winds, but is similar to mergers from GCs modeled with strong winds.

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“…The high stellar densities in globular cluster could also give rise to the creation of intermediate-mass black holes (Portegies Zwart & McMillan 2002;Portegies Zwart et al 2004;Giersz et al 2015), which might be the progenitors of supermassive black holes in Galactic centers. Globular clusters are finally important environments for the creation of tight black hole binaries which merge through the emission of gravitational waves (Banerjee, Baumgardt & Kroupa ⋆ E-mail: h.baumgardt@uq.edu.au 2010; Downing et al 2011;Askar et al 2016).…”

Section: Introductionmentioning

confidence: 99%

N-body modelling of globular clusters: masses, mass-to-light ratios and intermediate-mass black holes

Baumgardt

2016

Mon. Not. R. Astron. Soc.

208

252

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We have determined the masses and mass-to-light ratios of 50 Galactic globular clusters by comparing their velocity dispersion and surface brightness profiles against a large grid of 900 N -body simulations of star clusters of varying initial concentration, size and central black hole mass fraction. Our models follow the evolution of the clusters under the combined effects of stellar evolution and two-body relaxation allowing us to take the effects of mass segregation and energy equipartition between stars selfconsistently into account. For a subset of 16 well observed clusters we also derive their kinematic distances. We find an average mass-to-light ratio of Galactic globular clusters of < M/L V >= 1.98 ± 0.03, which agrees very well with the expected M/L ratio if the initial mass function (IMF) of the clusters was a standard Kroupa or Chabrier mass function. We do not find evidence for a decrease of the average mass-to-light ratio with metallicity. The surface brightness and velocity dispersion profiles of most globular clusters are incompatible with the presence of intermediate-mass black holes (IMBHs) with more than a few thousand M ⊙ in them. The only clear exception is ω Cen, where the velocity dispersion profile provides strong evidence for the presence of a ∼40,000 M ⊙ IMBH in the centre of the cluster.

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Compact binaries in star clusters - II. Escapers and detection rates

Cited by 105 publications

References 68 publications

Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO

Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

N-body modelling of globular clusters: masses, mass-to-light ratios and intermediate-mass black holes

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