Potential Subpopulations and Assembling Tendency of the Merging Black Holes

Wang, Yuan-Zhu; Li, Yinjie; Fan, Yi‐Zhong; Tang, Shao-Peng; Qin, Ying; Wei, Da-Ming

doi:10.3847/2041-8213/aca89f

Cited by 10 publications

(3 citation statements)

References 96 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Second, confirming the presence of 2G BHs presents its own unique challenges. Current mass-spin population studies for BBHs suggest that first-generation (1G) BHs typically exhibit low spin (Wang et al 2022;Abbott et al 2023;Li et al 2023). And binary evolution simulation also shows that the BHs in ordinary BH-NS systems have a dimensionless spin parameter less than about 0.2 (Xing et al 2023).…”

Section: Summary and Discussionmentioning

confidence: 99%

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Tang,

Gao,

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

The mass (M TOV) and radius (R TOV) of the maximum-mass nonrotating neutron star (NS) play a crucial role in constraining the elusive equation of state of cold dense matter and in predicting the fate of remnants from binary neutron star (BNS) mergers. In this study, we introduce a novel method to deduce these parameters by examining the mergers of second-generation (2G) black holes (BHs) with NSs. These 2G BHs are assumed to originate from supramassive neutron stars (SMNSs) formed in BNS mergers. Since the properties of the remnant BHs arising from the collapse of SMNSs follow a universal relation governed by M TOV and R TOV, we anticipate that by analyzing a series (∼100 detections) of mass and spin measurements of the 2G BHs using the third-generation ground-based gravitational-wave detectors, M TOV and R TOV can be determined with a precision of ∼0.01M ⊙ and ∼0.6 km, respectively.

show abstract

Section: Summary and Discussionmentioning

confidence: 99%

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Tang,

Gao,

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Hence, the constraints inferred by Sadiq et al (2022) cannot be used directly to probe the aforementioned astrophysical phenomena without first converting them into constraints on the astrophysical population (as opposed to the detectable one) by means of appropriately constructed selection functions (Farr 2019;Mandel et al 2019;Vitale et al 2020). Hence, previous studies on the existence of correlations in the astrophysical BBH population (such as the parameterized approaches of Callister et al 2021;Fishbach et al 2021;Biscoveanu et al 2022 or the mixture-model-based approaches of Wang et al 2022;Abbott et al 2023;Godfrey et al 2023;Li et al 2023) have mostly been carried out while making strong assumptions regarding the functional form of said correlations, rendering the inferred constraints susceptible to the previously mentioned limitations of parametric population modeling.…”

Section: Introductionmentioning

confidence: 99%

Nonparametric Inference of the Population of Compact Binaries from Gravitational-wave Observations Using Binned Gaussian Processes

Ray,

Hernandez,

Mohite

et al. 2023

ApJ

View full text Add to dashboard Cite

The observation of gravitational waves from multiple compact binary coalescences by the LIGO–Virgo–KAGRA detector networks has enabled us to infer the underlying distribution of compact binaries across a wide range of masses, spins, and redshifts. In light of the new features found in the mass spectrum of binary black holes and the uncertainty regarding binary formation models, nonparametric population inference has become increasingly popular. In this work, we develop a data-driven clustering framework that can identify features in the component mass distribution of compact binaries simultaneously with those in the corresponding redshift distribution, from gravitational-wave data in the presence of significant measurement uncertainties, while making very few assumptions about the functional form of these distributions. Our generalized model is capable of inferring correlations among various population properties, such as the redshift evolution of the shape of the mass distribution itself, in contrast to most existing nonparametric inference schemes. We test our model on simulated data and demonstrate the accuracy with which it can reconstruct the underlying distributions of component masses and redshifts. We also reanalyze public LIGO–Virgo–KAGRA data from events in GWTC-3 using our model and compare our results with those from some alternative parametric and nonparametric population inference approaches. Finally, we investigate the potential presence of correlations between mass and redshift in the population of binary black holes in GWTC-3 (those observed by the LIGO–Virgo–KAGRA detector network in their first three observing runs), without making any assumptions about the specific nature of these correlations.

show abstract

“…A number of previous studies have looked for covariance between various parameters describing the BBH population (Safarzadeh et al 2020;Callister et al 2021;Fishbach et al 2021;Adamcewicz & Thrane 2022;Belczynski et al 2022;Biscoveanu et al 2022;Franciolini & Pani 2022;Hoy et al 2022;Tiwari 2022;Vitale et al 2022;Wang et al 2022;Baibhav et al 2023;Ray et al 2023). In particular, Callister et al (2021) argued that the data support an anticorrelation between mass ratio º ( ) q m m , 1 2 1 and effective inspiral spin (Damour 2001)…”

Section: Introductionmentioning

confidence: 99%

Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins

Adamcewicz,

Lasky,

Thrane

2023

ApJ

View full text Add to dashboard Cite

The astrophysical origins of the binary black hole systems seen with gravitational waves are still not well understood. However, features in the distribution of black hole masses, spins, redshifts, and eccentricities provide clues into how these systems form. Much has been learned by investigating these distributions one parameter at a time. However, we can extract additional information by studying the covariance between pairs of parameters. Previous work has shown preliminary support for an anticorrelation between mass ratio q ≡ m 2/m 1 and effective inspiral spin χ eff in the binary black hole population. In this study, we test for the existence of this anticorrelation using updated data from the third gravitational-wave transient catalog and improve our copula-based framework to employ a more robust model for black hole spins. We find evidence for an anticorrelation in (q, χ eff) with 99.7% credibility. This may imply high common-envelope efficiencies, stages of super-Eddington accretion, or a tendency for binary black hole systems to undergo mass-ratio reversal during isolated evolution. Covariance in (q, χ eff) may also be used to investigate the physics of tidal spinup as well as the properties of binary black hole–forming active galactic nuclei.

show abstract

Potential Subpopulations and Assembling Tendency of the Merging Black Holes

Cited by 10 publications

References 96 publications

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Nonparametric Inference of the Population of Compact Binaries from Gravitational-wave Observations Using Binned Gaussian Processes

Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins

Contact Info

Product

Resources

About