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  No Detectable Kilonova Counterpart is Expected for O3 Neutron Star-Black Hole Candidates

Zhu, J.-P., Wu, S., Yang, Y.-P., Zhang, B., Yu, Y.-W., Gao, H., et al. (2021). No Detectable Kilonova Counterpart is Expected for O3 Neutron Star-Black Hole Candidates. The Astrophysical Journal, 921(2): 156. doi:10.3847/1538-4357/ac19a7.

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 Creators:
Zhu, Jin-Ping, Author
Wu, Shichao1, Author              
Yang, Yuan-Pei, Author
Zhang, Bing, Author
Yu, Yun-Wei, Author
Gao, He, Author
Cao, Zhoujian, Author
Liu, Liang-Duan, Author
Affiliations:
1Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR,General Relativity and Quantum Cosmology, gr-qc
 Abstract: We analyse the tidal disruption probability of potential neutron star--black hole (NSBH) merger gravitational wave (GW) events, including GW190426_152155, GW190814, GW200105_162426 and GW200115_042309, detected during the third observing run of the LIGO/Virgo Collaboration, and the detectability of kilonova emission in connection with these events. The posterior distributions of GW190814 and GW200105_162426 show that they must be plunging events and hence no kilonova signal is expected from these events. With the stiffest NS equation of state allowed by the constraint of GW170817 taken into account, the probability that GW190426_152155 and GW200115_042309 can make tidal disruption is $\sim24\%$ and $\sim3\%$, respectively. However, the predicted kilonova brightness is too faint to be detected for present follow-up search campaigns, which explains the lack of electromagnetic (EM) counterpart detection after triggers of these GW events. Based on the best constrained population synthesis simulation results, we find that disrupted events account for only $\lesssim20\%$ of cosmological NSBH mergers since most of the primary BHs could have low spins. The associated kilonovae for those disrupted events are still difficult to be discovered by LSST after GW triggers in the future, because of their low brightness and larger distances. For future GW-triggered multi-messenger observations, potential short-duration gamma-ray bursts and afterglows are more probable EM counterparts of NSBH GW events.

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 Dates: 2021-06-292021-07-302021
 Publication Status: Published in print
 Pages: 13 pages, 6 figures, 3 tables, accepted for publication in ApJ
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 Rev. Type: -
 Identifiers: arXiv: 2106.15781
DOI: 10.3847/1538-4357/ac19a7
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Title: The Astrophysical Journal
Source Genre: Journal
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Pages: - Volume / Issue: 921 (2) Sequence Number: 156 Start / End Page: - Identifier: -