The χeff − z correlation of field binary black hole mergers and how 3G gravitational-wave detectors can constrain it

Bavera, Simone S.; Fishbach, M.; Zevin, M.; Zapartas, Emmanouil; Fragos, Tassos

doi:10.1051/0004-6361/202243724

Cited by 23 publications

(13 citation statements)

References 83 publications

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“…We model the 𝜒 eff distribution at each redshift as a mixture between a Gaussian centered at zero, representing the "dynamical" subpopulation, and a truncated Gaussian restricted to positive 𝜒 eff . We refer to the fraction of systems in the zero-mean component as 𝑓 dyn (𝑧), and allow both the overall merger rate and 𝑓 dyn (𝑧) to evolve with redshift (similarly to Bavera et al 2022 andBiscoveanu et al 2022; see §A1), thereby measuring the "dynamics" rate as a function of redshift.…”

Section: Merger Rate Evolution Inferred From Gwtc-3mentioning

confidence: 99%

Globular cluster formation histories, masses and radii inferred from gravitational waves

Fishbach¹,

Fragione²

2023

Preprint

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Globular clusters (GCs) are found in all types of galaxies and harbor some of the most extreme stellar systems, including black holes that may dynamically assemble into merging binaries (BBHs). Uncertain GC properties, including when they formed, their initial masses and sizes, affect their production rate of BBH mergers. Using the gravitational-wave catalog GWTC-3, we measure that dynamically-assembled BBHs -those that are consistent with isotropic spin directions -make up 61 +29 −44 % of the total merger rate, with a local merger rate of 10.9 +16.8 −9.3 Gpc −3 yr −1 rising to 58.9 +149.4 −46.0 Gpc −3 yr −1 at 𝑧 = 1. We assume this inferred rate describes the contribution from GCs and compare it against the Cluster Monte Carlo () simulation catalog to directly fit for the GC initial mass function, virial radius distribution, and formation history. We find that GC initial masses are consistent with a Schechter function with slope 𝛽 𝑚 = −1.9 +0.8 −0.8 . Assuming a mass function slope of 𝛽 𝑚 = −2 and a mass range between 10 4 -10 8 𝑀 , we infer a GC formation rate at 𝑧 = 2 of 5.0 +9.4 −4.0 Gpc −3 yr −1 , or 2.1 +3.9 −1.7 × 10 6 𝑀 Gpc −3 yr −1 in terms of mass density. We find that the GC formation rate probably rises more steeply than the global star formation rate between 𝑧 = 0 and 𝑧 = 3 (82% credibility) and implies a local number density that is 𝑓 ev = 22.6 +29.9 −16.2 times higher than the observed density of survived GCs. This is consistent with expectations for cluster evaporation, but may suggest that other environments contribute to the rate of BBH mergers with significantly tilted spins.

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Section: Merger Rate Evolution Inferred From Gwtc-3mentioning

confidence: 99%

Globular cluster formation histories, masses and radii inferred from gravitational waves

Fishbach¹,

Fragione²

2023

Preprint

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“…For the broader range of redshifts that will be accessible to 3G detectors, this is not expected to continue to hold, see e.g. Fishbach et al (2021);van Son et al (2022); Belczynski et al (2022) for the redshift dependence of the mass distribution, and Qin et al (2018); Biscoveanu et al (2022); Bavera et al (2022) for the redshift dependence of the spin distribution. Our choice of redshift-independent mass and spin distributions should therefore be considered only as dictated by simplicity, and will likely have to be modified as the observational and theoretical understanding improve.…”

Section: Bbhmentioning

confidence: 99%

Forecasting the detection capabilities of third-generation gravitational-wave detectors using $\texttt{GWFAST}$

Iacovelli¹,

Mancarella²,

Foffa³

et al. 2022

Preprint

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We introduce GWFAST, a novel Fisher-matrix code for gravitational-wave studies, tuned toward third-generation gravitational-wave detectors such as Einstein Telescope (ET) and Cosmic Explorer (CE). We use it to perform a comprehensive study of the capabilities of ET alone, and of a network made by ET and two CE detectors, as well as to provide forecasts for the forthcoming O4 run of the LVK collaboration. We consider binary neutron stars, binary black holes and neutron star-black hole binaries, and compute basic metrics such as the distribution of signal-to-noise ratio (SNR), the accuracy in the reconstruction of various parameters (including distance, sky localization, masses, spins and, for neutron stars, tidal deformabilities), and the redshift distribution of the detections for different thresholds in SNR and different levels of accuracy in localization and distance measurement. We examine the expected distribution and properties of 'golden events', with especially large values of the SNR. We also pay special attention to the dependence of the results on astrophysical uncertainties and on various technical details (such as choice of waveforms, or the threshold in SNR), and we compare with other Fisher codes in the literature. In the companion paper Iacovelli et al. ( 2022) we discuss the technical aspects of the code. Together with this paper, we publicly release the code GWFAST a) , and the library WF4Py b) implementing state-of-the-art gravitational-wave waveforms in pure Python.

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“…Massive stars with nearly equal masses in close binaries tend to follow the CHE and thus result in binary BHs that could merge within a Hubble time (Marchant et al 2016;du Buisson et al 2020;Zevin et al 2021;Riley et al 2021;Bavera et al 2022aBavera et al , 2022c. Treatments of CHE and predictions of its outcome have been calculated by a variety of techniques, ranging from simplified prescriptions (e.g., Riley et al 2021) to detailed models of massive binary evolution (Marchant et al 2016;du Buisson et al 2020).…”

Section: Properties Of Bbhs Predicted By the Che Channelmentioning

confidence: 99%

Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3

Qin

Wang

Bavera

et al. 2022

ApJ

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The LIGO, Virgo, and KAGRA (LVK) Collaboration has announced 90 coalescing binary black holes (BBHs) with p astro > 50% to date; however, the origin of their formation channels is still an open scientific question. Given various properties of BBHs (BH component masses and individual spins) inferred using the default priors by the LVK, independent groups have been trying to explain the formation of the BBHs with different formation channels. Of all formation scenarios, the chemically homogeneous evolution (CHE) channel has stood out with distinguishing features, namely, nearly equal component masses and preferentially high individual spins aligned with the orbital angular momentum. We perform Bayesian inference on the BBH events officially reported in GWTC-3 with astrophysically predicted priors representing different formation channels of the isolated binary evolution (common-envelope evolution channel, CEE; CHE; stable mass transfer, SMT). Given assumed models, we report strong evidence for GW190517_055101 being most likely to have formed through the CHE channel. Assuming the BBH events in the subsample are all formed through one of the isolated binary evolution channels, we obtain the lower limits on the local merger rate density of these channels at 11.45 Gpc−3 yr−1 (CEE), 0.18 Gpc−3 yr−1 (CHE), and 0.63 Gpc−3 yr−1 (SMT) at 90% credible level.

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The χ_eff − z correlation of field binary black hole mergers and how 3G gravitational-wave detectors can constrain it

Cited by 23 publications

References 83 publications

Globular cluster formation histories, masses and radii inferred from gravitational waves

Globular cluster formation histories, masses and radii inferred from gravitational waves

Forecasting the detection capabilities of third-generation gravitational-wave detectors using $\texttt{GWFAST}$

Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3

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