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Kwak, Kyujin
Computational Astrophysics Lab
Research Interests
  • Computational Fluid Dynamics
  • Astrophysical and Laboratory Plasma
  • Hydrodynamics with Radiation
  • Nuclear, Atomic, and Molecular Reactions

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Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences

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Title
Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences
Author
Abbott, R.LIGO Sci CollaborationVirgo CollaborationKAGRA CollaborationHa, SJung, KKim, Y-MKwak, K.
Issue Date
2021-07
Publisher
IOP PUBLISHING LTD
Citation
ASTROPHYSICAL JOURNAL LETTERS, v.915, no.1, pp.L5
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(-1.5)(+1.2) and 1.9(-0.2)(+0.3)M(circle dot), whereas the source of GW200115 has component masses 5.7(-2.1)(+1.8) and 1.5(-0.3)(+0.7)M(circle dot) (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) and 300(-100)(+150) 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-(+75)(33) Gpc(-3) yr(-1) when assuming that GW200105 and GW200115 are representative of the NSBH population or 130(-69)(+112) Gpc(-3) yr(-1) under the assumption of a broader distribution of component masses.
URI
https://scholarworks.unist.ac.kr/handle/201301/53382
URL
https://iopscience.iop.org/article/10.3847/2041-8213/ac082e
DOI
10.3847/2041-8213/ac082e
ISSN
2041-8205
Appears in Collections:
PHY_Journal Papers
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