Capability for detection of GW190521-like binary black holes with TianQin

TL;DR

This paper evaluates TianQin's ability to detect GW190521-like binary black hole mergers, demonstrating its potential for early detection, precise parameter estimation, and contribution to cosmology and astrophysics.

Contribution

The study systematically assesses TianQin's detection prospects for GW190521-like sources, highlighting its capabilities in detection, parameter recovery, and scientific implications.

Findings

TianQin can detect up to a dozen GW190521-like sources with SNR > 8.

It can precisely recover merger parameters, including coalescence time and sky location.

TianQin could constrain the Hubble constant with 10% accuracy.

Abstract

The detection of GW190521 gains huge attention because it is the most massive binary that LIGO and Virgo ever confidently detected until the release of GWTC-3 (GW190426_190642 is more massive), and it is the first black hole merger whose remnant is believed to be an intermediate mass black hole. Furthermore, the primary black hole mass falls in the black hole mass gap, where the pair-instability supernova prevents the formation of astrophysical black holes in this range. In this paper, we systematically explore the prospect of TianQin on detecting GW190521-like sources. For sources with small orbital eccentricities, (i) TianQin could resolve up to a dozen of sources with signal-to-noise ratio (SNR) larger than 8. Even if the signal-to-noise ratio threshold increases to 12, TianQin could still detect GW190521-like binaries. (ii) The parameters of sources merging within several years would be precisely recovered. The precision of coalescence time and sky localization closes to $1\ {\rm s}$ and $1\ {\rm deg^{2}}$ respectively. This indicates that TianQin could provide early warnings for ground-based gravitational waves detectors and electromagnetic telescopes for these sources. Furthermore, TianQin could distinguish the formation channels of these sources by measuring the orbital eccentricities with a relative precision of $10^{-4}$. (iii) TianQin could constrain the Hubble constant with a $10\%$ precision with GW190521-like sources. Finally, for very eccentric GW190521-like sources, although their gravitational wave signal might be too weak for TianQin to detect, even the null detection of TianQin could still present a significant contribution to the understanding of the underlying science.