The Cosmic Evolution of Binary Black Holes in Young, Globular and Nuclear Star Clusters: Rates, Masses, Spins and Mixing Fractions

Mapelli, Michela; Bouffanais, Yann; Santoliquido, Filippo; Sedda, Manuel Arca; Artale, M. Celeste

doi:10.48550/arxiv.2109.06222

Cited by 3 publications

(5 citation statements)

References 155 publications

(227 reference statements)

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“…Their Figure 1 shows evidence that the stable RLOF channel preferentially forms higher chirp masses than the CE channel. Mapelli et al (2021) compare the rate evolution of the intrinsic BBH merger rate from isolated binaries to the rate from nuclear star clusters, globular star clusters and young stellar clusters. They find that the primary BH mass function is more top heavy at high redshift for both globular and nuclear star clusters.…”

Section: Contribution From Other Formation Channelsmentioning

confidence: 99%

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The redshift evolution of the binary black hole merger rate: a weighty matter

van Son,

de Mink,

Callister

et al. 2021

Preprint

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Gravitational wave detectors are starting to reveal the redshift evolution of the binary black hole (BBH) merger rate, R BBH (z). We make predictions for R BBH (z) as a function of black hole mass for systems originating from isolated binaries. To this end, we investigate correlations between the delay time and black hole mass by means of the suite of binary population synthesis simulations, COMPAS. We distinguish two channels: the common envelope (CE), and the stable Roche-lobe overflow (RLOF) channel, characterised by whether the system has experienced a common envelope or not. We find that the CE channel preferentially produces BHs with masses below about 30 M and short delay times (t delay 1 Gyr), while the stable RLOF channel primarily forms systems with BH masses above 30 M and long delay times (t delay 1 Gyr). We provide a new fit for the metallicity specific starformation rate density based on the Illustris TNG simulations, and use this to convert the delay time distributions into a prediction of R BBH (z). This leads to a distinct redshift evolution of R BBH (z) for high and low primary BH masses. We furthermore find that, at high redshift, R BBH (z) is dominated by the CE channel, while at low redshift it contains a large contribution (∼ 40%) from the stable RLOF channel. Our results predict that, for increasing redshifts, BBHs with component masses above 30 M will become increasingly scarce relative to less massive BBH systems. Evidence of this distinct evolution of R BBH (z) for different BH masses can be tested with future detectors.

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Section: Contribution From Other Formation Channelsmentioning

confidence: 99%

“…The redshift evolution of source property distributions remains relatively obscured, though it is actively being studied (see e.g. Neijssel et al 2019;Mapelli et al 2021). Recent work hints towards relations between source properties and redshift evolution.…”

Section: Introductionmentioning

confidence: 99%

The redshift evolution of the binary black hole merger rate: a weighty matter

van Son,

de Mink,

Callister

et al. 2021

Preprint

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“…However, in general we would expect the evolution to change the shape of p(m 1z , m 2z |z), see e.g. [62,63], and, therefore, cosmology and evolution of the mass distribution can be disentangled. Nonetheless, we can imagine that time evolution might affect one of the edges of one of our mass bins.…”

mentioning

confidence: 99%

“…[65]). Recent work has explored the evolution of the mass distribution in field binaries [62] and clusters [63], and searches have been performed in current data [66]. These works show that the high-mass end of the distribution is more susceptible to environmental effects such as metallicity that are expected to evolve with cosmic time, as well as the time delay distribution [40,62].…”

mentioning

confidence: 99%

Spectral sirens: cosmology from the full mass distribution of compact binaries

Ezquiaga¹,

Holz²

2022

Preprint

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We explore the use of the mass spectrum of neutron stars and black holes in gravitational-wave compact binary sources as a cosmological probe. These standard siren sources provide direct measurements of luminosity distance. In addition, features in the mass distribution, such as mass gaps or peaks, will redshift, and thus provide independent constraints on their redshift distribution. We argue that the mass spectrum of LIGO/Virgo/KAGRA events introduces at least five independent mass "features": the upper and lower edges of the pair instability supernova (PISN) gap, the upper and lower edges of the neutron star-black hole gap, and the minimum neutron star mass. We find that the PISN gap dominates the cosmological inference with current detectors (2G), as shown in previous work. We further argue that the lower mass gap will provide the most powerful constraints in the era of Cosmic Explorer and Einstein Telescope (3G). We demonstrate that degeneracies between redshift evolution of the source masses and cosmology can be broken, unless an astrophysical conspiracy shifts all features of the full mass distribution simultaneously following the (non-trivial) Hubble diagram evolution. We find that this "spectral siren" method has the potential to constrain both cosmology and the evolution of the mass distribution, with 2G achieving better than 10% precision on H(z) at z 1 within a year, and 3G reaching 1% at z 2 within one month.

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“…Various studies were carried out, based on some analytical models (e.g., [11][12][13][14]) and some non-parametric approaches (e.g., [15][16][17]), some formation/evolution characteristics of the compact binaries are being revealed (e.g. [18][19][20][21][22][23][24][25][26]).…”

mentioning

confidence: 99%

Divergence in mass ratio distributions between low-mass and high-mass coalescing binary black holes

Li,

Wang,

Tang

et al. 2022

Preprint

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The coalescing binary black hole (BBH) systems were likely formed in several channels and the identification of them is a challenging task. Previously, people have found out that at the mass of ∼ 34M there is a distinct Gaussian-like peak superposed on the power-law mass function of the primary components. In this work, with the refined Power Law + Peak primary mass distribution models, we identify a population of BBHs with a much stronger preference for equalmass binaries, which dominates the Peak, for the first time. These BBHs have a pairing function with a β = 8.56 +3.08 −5.62 , or with a σm = 3.14 +4.99 −1.76 M , where σm represents the width of the distribution of m1 − m2 (i.e., the difference between and the primary and secondly masses). The BBHs in the Power Law have a much flatter pairing function with a β = −0.11 +2.48 −1.55 . All these parameter ranges are reported for 90% credibility. Our finding likely points towards the chemically homogeneous evolution channel featured by a high mass ratio for the BBHs with a total mass above ∼ 55M . As shown in our simulation, the increase of the GWTC-3 sample by a factor of several would formally establish the presence of the high q population of massive BBHs.

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The Cosmic Evolution of Binary Black Holes in Young, Globular and Nuclear Star Clusters: Rates, Masses, Spins and Mixing Fractions

Cited by 3 publications

References 155 publications

The redshift evolution of the binary black hole merger rate: a weighty matter

The redshift evolution of the binary black hole merger rate: a weighty matter

Spectral sirens: cosmology from the full mass distribution of compact binaries

Divergence in mass ratio distributions between low-mass and high-mass coalescing binary black holes

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