Observation of gravitational waves from two neutron star-black hole coalescences

The LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, R. Abbott, G. S. Davies, O. Edy, I. W. Harry, D. Keitel, A. P. Lundgren, R. Macas, Connor McIsaac, S. Mozzon, L. K. Nuttall, A. R. Williamson

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Abstract

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 +1.2 −1.5 M and 1.9 +0.3 −0.2 M, whereas the source of GW200115 has component masses 5.7 +1.8 −2.1 M and 1.5 +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 +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 spin or tidal deformation of the secondary component for either event. We infer a NSBH merger rate density of 45 +75 −33 Gpc−3yr−1 when assuming GW200105 and GW200115 are representative of the NSBH population, or 130 +112 −69 Gpc−3yr−1 under the assumption of a broader distribution of component masses.
Original languageEnglish
Article numberL5
Number of pages24
JournalAstrophysical Journal Letters
Volume915
Issue number1
DOIs
Publication statusPublished - 29 Jun 2021

Keywords

  • astro-ph.HE
  • RCUK
  • STFC
  • GW_HIGHLIGHT

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