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)M⊙ and 〖1.9〗_(-0.2)^(+0.3)M⊙, whereas the source of GW200115 has component masses 〖5.7〗_(-2.1)^(+1.8)M⊙ and 〖1.5〗_(-0.3)^(+0.7)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〗_(-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 spin or tidal deformation of the secondary component for either event. We infer a NSBH merger rate density of 〖45〗_(-33)^(+75) 〖Gpc〗^(-3) 〖yr〗^(-1) when assuming 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.

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

R. Fittipaldi;A. Paolone;
2021

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)M⊙ and 〖1.9〗_(-0.2)^(+0.3)M⊙, whereas the source of GW200115 has component masses 〖5.7〗_(-2.1)^(+1.8)M⊙ and 〖1.5〗_(-0.3)^(+0.7)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〗_(-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 spin or tidal deformation of the secondary component for either event. We infer a NSBH merger rate density of 〖45〗_(-33)^(+75) 〖Gpc〗^(-3) 〖yr〗^(-1) when assuming 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.
2021
Istituto dei Sistemi Complessi - ISC
Istituto Superconduttori, materiali innovativi e dispositivi - SPIN
COMPACT BINARY COALESCENCE, SPIN-ORBIT MISALIGNMENT, REDUCED-ORDER MODEL, GAMMA-RAY BURSTS, ADVANCED-LIGO
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.14243/399647
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