Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

Tang, Shao-Peng; Wang, Hao; Wang, Yuan-Zhu; Han, Ming-Zhe; Fan, Yi‐Zhong; Wei, Da-Ming

doi:10.3847/1538-4357/ab77bf

Cited by 10 publications

(4 citation statements)

References 77 publications

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“…As for the NSBH binary, at that time, the NSBH merger detection rate will be enhanced by a factor of a few tens. With a reasonably large sample, the BH mass function in the merging NSBH systems can be reliably reconstructed (Tang et al 2020;Yang et al 2018), which will shed light on the formation or evolutionary paths of these BHs, and the difference between the BH mass functions for the merging NSBH and BBH systems, if significant, would be revealed too.…”

Section: Discussionmentioning

confidence: 99%

GW190426_152155: a merger of neutron star-black hole or low mass binary black holes?

Li,

Han,

Tang

et al. 2020

Preprint

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GW190426 152155 was recently reported as one of the 39 candidate gravitational wave (GW) events in Abbott et al. ( 2020), which has an unusual source-frame chirp mass ∼ 2.4M and may be the first GW signal from a neutron star-black hole (NSBH) merger. Assuming an astrophysical origin, we reanalyze GW190426 152155 using several waveforms with different characteristics, and consider two different priors for the mass ratio of the binary (Uniform and LogUniform). We find that the results are influenced by the priors of mass ratio, and this candidate could also be from the merger of two low mass black holes (BH). In the case for a binary black hole (BBH) merger, the effective spin is likely negative and the effective precession spin is non-negligible. As for the NSBH merger, supposing the mass of the light object follow the distribution of current neutron stars (NSs) with a reasonably measured/constrained mass, the spin of the low mass BH is so small that is hard to generate bright electromagnetic emission. Finally, we estimate a merger rate of GW190426 152155-like systems to be 59 +137 −51 Gpc −3 yr −1 .

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Section: Discussionmentioning

confidence: 99%

GW190426_152155: a merger of neutron star-black hole or low mass binary black holes?

Li,

Han,

Tang

et al. 2020

Preprint

Self Cite

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“…The luminosity distance is computed from the redshift assuming PLANCK18 flat ΛCDM (Planck Collaboration et al 2020). We then use the complete GW parameters (for a list and description of these parameters, one can refer, for example, to Table 1 of Tang et al 2020) to calculate the Fisher Information Matrix (FIM), except for fixing the tidal deformability of the BH to 0. We discard all events where the inversion error of the FIM exceeds 0.05 and where the optimal signal-to-noise ratio (S/N) is below 12.…”

Section: Methodsmentioning

confidence: 99%

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

Tang,

Gao,

et al. 2023

ApJ

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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.

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“…Following The LIGO Scientific Collaboration et al (2020), we choose the false alarm rate (FAR) of 1yr −1 as the threshold to select the events. To increase the purity Reconstruction with l = 0.9 Reconstruction with l = 0.9 of sample and avoid misidentification of BBH (Tang et al 2020), the GW190426, GW190719, and GW190909 are not included in this analysis. In addition, we further exclude the unusual asymmetry system GW190814 (Abbott et al 2020b), which is a significant outlier (The LIGO Scientific Collaboration et al 2020).…”

Section: Reconstruction With Data Of Gwtc-2mentioning

confidence: 99%

A flexible Gaussian process reconstruction method and the mass function of the coalescing binary black hole systems

Li,

Wang,

Han

et al. 2021

Preprint

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We develop a new method based on Gaussian process to reconstruct the mass distribution of binary black holes (BBHs). Instead of prespecifying the formalisms of mass distribution, we introduce a more flexible and nonparametric model with which the distribution can be mainly determined by the observed data. We first test our method with simulated data, and find that it can well recover the injected distribution. Then we apply this method to analyze the data of BBHs' observations from LIGO-Virgo Gravitational-Wave Transient Catalog 2. By reconstructing the chirp mass distribution, we find that there is a peak or a platform locating at 20 − 30 M rather than a single-power-lawlike decrease from low mass to high mass. Moreover, one or two peaks in the chirp mass range of M < 20 M may be favored by the data. Assuming a mass-independent mass ratio distribution of p(q) ∝ q 1.4 , we further obtain a distribution of primary mass, and find that there is a feature locating in the range of ( 30, 40) M , which can be related to Broken Power Law and Power Law + Peak distributions described in The LIGO Scientific Collaboration et al. (2020). Besides, the merger rate of BBHs is estimated to R = 25.53 +13.87 −8.76 Gpc −3 yr −1 supposing there is no redshift evolution. 1. INTRODUCTION

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Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

Cited by 10 publications

References 77 publications

GW190426_152155: a merger of neutron star-black hole or low mass binary black holes?

GW190426_152155: a merger of neutron star-black hole or low mass binary black holes?

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

A flexible Gaussian process reconstruction method and the mass function of the coalescing binary black hole systems

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