Search for Eccentric Binary Black Hole Mergers with Advanced LIGO and Advanced Virgo during Their First and Second Observing Runs
Search for Eccentric Binary Black Hole Mergers with Advanced LIGO and Advanced Virgo during Their First and Second Observing Runs
复制标题
DOI：
10.3847/1538-4357/ab3c2d
复制
发表时间：
2019-10-01
影响因子：
4.9
通讯作者：
Salemi, F.
中科院分区：
文献类型：
--
作者：
Abbott, B. P.;Abbott, R.;Salemi, F.
当通过动力学相互作用形成时，恒星质量的双星黑洞（BBH）可能会保留偏心轨道（在10 Hz时e > 0.1），可以被地面引力波探测器探测到。因此，偏心率可用于区分动态形成的二进制文件与孤立的BBH合并。目前基于模板的引力波搜索不使用与偏心轨道相关的波形模型，这使得对偏心双星系统的搜索效率较低。在这里，我们提出了一个搜索的BBH合并，inspiral在偏心轨道上使用的数据从第一次和第二次观测运行（O 1和O2）的高级LIGO和高级处女座的结果。我们使用相干WaveBurst算法进行搜索，该算法对信号形态使用最少的假设，并且不依赖于二进制波形模板。我们发现，它是敏感的二进制合并的检测范围是弱依赖于所有绑定系统的偏心率。我们的搜索没有发现任何新的二元合并候选人。我们解释这些结果的偏心二元形成模型。我们排除了形成通道的速率大于或接近100 Gpc（-3）yr（-1）的e > 0.1，假设黑洞质量谱的幂律指数小于或接近2。
When formed through dynamical interactions, stellar-mass binary black holes (BBHs) may retain eccentric orbits (e > 0.1 at 10 Hz) detectable by ground-based gravitational-wave detectors. Eccentricity can therefore be used to differentiate dynamically formed binaries from isolated BBH mergers. Current template-based gravitational-wave searches do not use waveform models associated with eccentric orbits, rendering the search less efficient for eccentric binary systems. Here we present the results of a search for BBH mergers that inspiral in eccentric orbits using data from the first and second observing runs (O1 and O2) of Advanced LIGO and Advanced Virgo. We carried out the search with the coherent WaveBurst algorithm, which uses minimal assumptions on the signal morphology and does not rely on binary waveform templates. We show that it is sensitive to binary mergers with a detection range that is weakly dependent on eccentricity for all bound systems. Our search did not identify any new binary merger candidates. We interpret these results in light of eccentric binary formation models. We rule out formation channels with rates greater than or similar to 100 Gpc(-3) yr(-1) for e > 0.1, assuming a black hole mass spectrum with a power-law index less than or similar to 2.