Science with the TianQin observatory: Preliminary results on stellar-mass binary black holes

Abstract

We present a Bayesian parameter estimation progress to infer the stellar mass binary black hole properties by TianQin, LISA, and TianQin+LISA. Two typical Stellar-mass Black Hole Binary systems, GW150914 and GW190521 are chosen as the fiducial sources. In this work, we establish the ability of TianQin to infer the parameters of those systems and first apply the full frequency response in TianQin's data analysis. We obtain the parameter estimation results and explain the correlation between them. We also find the TianQin+LISA could marginally increase the parameter estimation precision and narrow the 1σ area compared with TianQin and LISA individual observations. We finally demonstrate the importance of considering the effect of spin when the binaries have a nonzero component spin and great derivation will appear especially on mass, coalescence time and sky location.

How many extra-Galactic stellar-mass binary black holes will be detected by space gravitational-wave interferometers?

“…At T = 10yr, we have (Ntot, Nmer) = (8.9, 0.83) and (7.8, 3.1), respectively, for LISA and TianQin. These numbers are basically consistent with the results of Liu et al (2020).…”

“…Considering the timeline of the proposed missions such as LISA, Taiji and TianQin, we can expect their joint signal analysis. In this section, we discuss how the BBH detection could be improved by the coherent matched filtering anal- ysis (see also Liu et al 2020). We specifically examine the following potential combinations of two 10yr-missions (i) L2-10: two LISA-equivalent detectors operated concurrently for 10 years (100% time overlap),…”

“…The detection prospects by these future detectors can be evaluated by combining astrophysical as well as instrumental information (noise curve, operation period etc.). In 2016, shortly after the announcement of GW150914 (Abbott et al 2016), the authors studied the expected number of BBH detections with LISA (Kyutoku & Seto 2016, paper 1, see also Sesana 2016;Del Pozzo, Sesana, & Klein 2018;Liu et al 2020). In the past 6 years after the study, along with the significant improvement in our knowledge on BBHs, the sensitivity goal of LISA was refined and narrowed down.…”

Multi-Messenger Constraints on Magnetic Fields in Merging Black Hole-Neutron Star Binaries

“…-From Figure 2 we see that moving GW2001105 or GW2001115 closer, to within 100 Mpc can decrease the upper limit to ∼10 14 G. Because the magnetic field strength upper limit scales as the square root of the flux upper limit, a future BHNS merger with similar properties as GW2001105 could result in a 10 13 G constraint for a 100× better flux upper limit than used here. More robust upper limits may be possible in the future not only with more sensitive EM detectors but with GW pre-warnings from low-frequency detectors such as LISA (Sesana 2016;Amaro-Seoane & et al 2017), Tian-Qin (Luo et al 2016;Liu et al 2020), or DECIGO (Isoyama et al 2018).…”

Constrains on the electric charges of the binary black holes with GWTC-1 events

“…This provides a convincing evidence to support the reasonability of our work. For future space-based GW detectors such as Laser Interferometer Space Antenna (LISA) [35] and TianQin [36], the duration of GW strain from BH binaries are much longer [37,38]. Since the dipole gravitational radiation dominates at −1 PN order, it is more suitable for detecting by LISA and TianQin.…”