Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences
Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences
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DOI：
10.3847/2041-8213/ac082e
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发表时间：
2021-07-01
影响因子：
7.9
通讯作者：
Zweizig, J.
中科院分区：
文献类型：
--
作者：
Abbott, R.;Abbott, T. D.;Zweizig, J.
我们报告了利戈（Ligo）的两个紧凑型二元合并的重力波和处女座的第三次观察，其特性与中子星 - 黑洞（NSBH）二进制文件一致。这两个事件命名为GW200105_162426和GW200115_042309，缩写为GW200105和GW200115； Ligo Livingston和Pirgo观察到了第一个，第二个Ligo-Virgo探测器都观察到了第一个。 GW200105的来源具有组件质量8.9（-1.5）（+1.2）和1.9（-0.2）（+0.3）m（circle dot），而GW200115的来源具有组件质量5.7（-2.1）（-2.1）（-2.1）（+1.8）（+1.8）和1.5（-0.3）（+0.7）m（圆圈点）（所有测量值均在90％可靠水平上引用）。对于GW200105和GW200115，次级质量低于中子恒星的最大质量分别为89％-96％和87％-98％，范围来自不同的天体物理假设。源光度距离分别为280（-110）（+110）和300（-100）（+150）MPC。 GW200105的一级自旋的大小在90％可靠水平上小于0.23，并且其方向不受限制。对于GW200115，主要自旋在88％的概率上对轨道角动量产生负自旋投影。我们无法限制任何一个事件的次级成分的自旋或潮汐变形。当假设GW200105和GW200115的NSBH合并率密度为45-（+75）（+75）（33）GPC（-3）yr（-1）时（-3）YR（-1）在较广泛的组分质量分布的假设下。
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.