论文标题
丽莎如何以银河系的方式探测GW190425样二元中子星的种群？
How can LISA probe a population of GW190425-like binary neutron stars in the Milky Way?
论文作者
论文摘要
GW190425的性质是Ligo/Pirgo科学合作（LVC）检测到的假定的二进制中子星（BNS）合并，总质量为$ 3.4^{+0.3} _ { - 0.1} _ { - 0.1} $ _ $ $ _ $ _ $ _ {\ odot} $，仍然是一个神秘的。由于总质量如此之大，GW190425距离银河BNSS的总质量分布为$ 2.66 \ pm 0.12 $ m $ _ {\ odot} $，距离五个标准偏差。 LVC建议，由于选择效果，该系统可能是由快速合并通道形成的BNS，该通道在无线电波长处呈现其非检测。轨道周期少于几个小时的BNS（Ligo/处女座合并的祖细胞）是未来激光干涉仪空间天线（LISA）的主要目标候选者。如果GW190425样二进制物以银河系的方式存在，Lisa将检测到我们的星系量内，并将其chirp质量测量大于2 MHz的引力波频率的二进制室的chirp质量大于10％。这项工作探讨了我们如何探究带有丽莎的类似银河G190425的BNSS并研究其起源。我们假设银河系的BNS人群由两个不同的子人群组成：一个$ W_1 $的分数，该$ W_1 $遵循观察到的银河BNS Chirp质量分布和$ W_2 $，类似于GW190425的chirp质量。我们表明，丽莎在恢复GW190425样二进制的分数方面的准确性取决于BNS合并率。对于文献中报告的合并费率，$ 21-212 \，$ myr $^{ - 1} $，回收分数的错误在$ \ sim 30-5 $％之间变化。
The nature of GW190425, a presumed binary neutron star (BNS) merger detected by the LIGO/Virgo Scientific Collaboration (LVC) with a total mass of $3.4^{+0.3}_{-0.1}$ M$_{\odot}$, remains a mystery. With such a large total mass, GW190425 stands at five standard deviations away from the total mass distribution of Galactic BNSs of $2.66\pm 0.12$ M$_{\odot}$. LVC suggested that this system could be a BNS formed from a fast-merging channel rendering its non-detection at radio wavelengths due to selection effects. BNSs with orbital periods less than a few hours - progenitors of LIGO/Virgo mergers - are prime target candidates for the future Laser Interferometer Space Antenna (LISA). If GW190425-like binaries exist in the Milky Way, LISA will detect them within the volume of our Galaxy and will measure their chirp masses to better than 10% for those binaries with gravitational wave frequencies larger than 2 mHz. This work explores how we can probe a population of Galactic GW190425-like BNSs with LISA and investigate their origin. We assume that the Milky Way's BNS population consists of two distinct sub-populations: a fraction $w_1$ that follows the observed Galactic BNS chirp mass distribution and $w_2$ that resembles chirp mass of GW190425. We show that LISA's accuracy on recovering the fraction of GW190425-like binaries depends on the BNS merger rate. For the merger rates reported in the literature, $21 - 212\,$Myr$^{-1}$, the error on the recovered fractions varies between $\sim 30 - 5$%.
