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Abraham, S.; Agathos, M.; Barker, D.; Barsotti, L.; Bécsy, B.; Booker, P.; Cahillane, C.; Capote, E.; Carney, M. F.; Cella, G.; Chen, C.; Chen, H. Y.; Chu, Y-K.; Cieślar, M.; Ciolfi, R.; Cohadon, P.-F.; Constancio Jr, M.; Countryman, S. T.; Deenadayalan, M.; Divakarla, A. K.; Donovan, F.; Dooley, K. L.; Eddolls, G.; Fair, H.; Feng, F.; Ferguson, D. L.; Fiori, I.; Font, J. A.; Frasconi, F.; Fyffe, M.; Gaebel, S. M.; George, J.; Giacomazzo, B.; Godwin, P.; Gopakumar, A.; Grimes, E.; Guo, Y.; Halim, O.; Hanks, J.; Harder, T.; Heinzel, J.; Hennig, J.; Holt, K.; Huang, G-Z.; Hübner, M. T.; Janssens, K.; Janthalur, N. N.; Jones, D. I.; Kawaguchi, K.; Khadka, S.; Kim, K.; Kim, Y.-M.; Kissel, J. S.; Kondrashov, V.; Kozak, D. B.; Kozakai, C.; Kozu, R.; Kringel, V.; Kumar, Rahul; Leon, E.; Lundgren, A. P.; Macas, R.; Marchio, M.; Masso-Reid, M.; Merritt, J. D.; Miyoki, S.; Mogushi, K.; Molina, I.; Naticchioni, L.; Nayak, B.; Neil, B. F.; Okutani, Y.; Pai, S. A.; Patel, M.; Petterson, D.; Piergiovanni, F.; Placidi, E.; Polini, E.; Pong, D. Y. T.; Raab, F. J.; Ramirez, K. E.; Rapagnani, P.; Rosofsky, S. G.; Sadiq, J.; Setyawati, Y.; Shao, L.; Shcheblanov, N. S.; Summerscales, T. Z.; Talbot, C.; Tiwari, Shubhanshu; Tosta e Melo, I.; Ueshima, G.; Wellmann, F.; Whelan, J. T.; Wipf, C. C.; Yamamoto, H.; Yamamoto, T.; Yeeles, D. W.; Zhang, H.; Zweizig, J.
Astrophysical journal. Letters, 07/2021, Letnik: 915, Številka: 1Journal Article, Web Resource
We report the observation of gravitational waves from two compact binary coalescences in LIGO's and Virgo's third observing run with properties consistent with neutron star-black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo, and the second by all three LIGO-Virgo detectors. The source of GW200105 has component masses 8.9(exp +1.2/-1.5) M⨀ and 1.9(exp +0.3/-0.2) M⨀, whereas the source of GW200115 has component masses 5.7(exp +1.8/-2.1) M⨀ and 1.5(exp +0.7/-0.3) M⨀ (all measurements quoted at the 90% credible level). The probability that the secondary's mass is below the maximal mass of a neutron star is 89%-96% and 87%-98%, respectively, for GW200105 and GW200115, with the ranges arising from different astrophysical assumptions. The source luminosity distances are 280(exp +110/-110) Mpc and 300(+150/-100) Mpc, respectively. The magnitude of the primary spin of GW200105 is less than 0.23 at the 90% credible level, and its orientation is unconstrained. For GW200115, the primary spin has a negative spin projection onto the orbital angular momentum at 88% probability. We are unable to constrain the spin or tidal deformation of the secondary component for either event. We infer an NSBH merger rate density of 45(exp +75/-33) Gpc(exp -3) yr(exp -1) when assuming that GW200105 and GW200115 are representative of the NSBH population, or 130(+112/-69) Gpc(exp -3) yr(exp -1) under the assumption of a broader distribution of component masses.
