标题： 利用LISA识别中子星和黑洞的银河系双星系统 显示英文标题

标题： Identifying galactic binary systems of neutron stars and black holes with LISA

摘要： 激光干涉空间天线（LISA）将探测约100个由黑洞（BHs）和中子星（NSs）组成的银河系双星系统。 将这些双星的组分确定为BHs或NSs，并将其与$\sim 10^4$检测到的双白矮星区分开来将是具有挑战性的。 在没有其他信息的情况下，可以利用组分质量的推断值来对这些物体的性质进行分类。 然而，短周期银河系双星$\sim 10^7 - 10^3$年从合并开始会产生一个准单色信号，该信号携带的关于其质量的信息很少。 我们生成了包含来自通过孤立双星演化通道产生的天体物理上现实种群的银河系双黑洞（BHs）、双中子星（NSs）和黑洞-中子星（BHNSs）引力波（GWs）的合成LISA数据集。 我们使用端到端贝叶斯推理流程处理数据，以探索个体组分质量测量的准确性。 我们发现对于$\approx 10\% - 50\%$的检测系统， LISA可以通过测量轨道偏心率、近日点进动频率和引力波引起的频率导数来测量个体组分质量。 典型的质量分数误差为$\approx 1\% - 100\%$（取决于源参数的具体值），这将在许多情况下使物体被分类为BHs或NSs。 对于这些双星，LISA还能够确定它们在银河系中的三维位置。 LISA探测到的这些双致密天体样本将提供关于银河系中BHs和NSs种群、银河系恒星形成历史以及导致这些系统形成的天体物理过程的新信息。 然而，对于LISA探测到的双星中相当大比例的系统，其组分物体的性质可能仍然不清楚。 显示英文摘要

摘要： The Laser Interferometer Space Antenna (LISA) will detect ~ 100 galactic binary systems comprised of black holes (BHs) and neutron stars (NSs). Identifying the nature of the constituents of these binaries as BHs or NSs, and distinguishing them from $\sim 10^4$ detected double white dwarfs will be challenging. In the absence of any other information, the inferred values of the component masses can be used to classify the nature of these objects. However, short-period galactic binaries $\sim 10^7 - 10^3$ yr from coalescence produce a quasi-monochromatic signal which carries little information about their masses. We generate synthetic LISA data sets containing gravitational waves (GWs) from galactic binary BHs, binary NSs and BHNSs drawn from an astrophysically realistic population produced through the isolated binary evolution channel. We process the data with an end-to-end Bayesian inference pipeline to explore the accuracy with which the individual component masses can be measured. We find that for $\approx 10\% - 50\%$ of the detected systems LISA will be able to measure the individual component masses by measuring the orbital eccentricity, periapse precession frequency, and GW induced frequency derivative. Typical fractional mass errors are $\approx 1\% - 100\%$ (depending on the specific value of the source parameters), which will enable in many circumstances the classification of the objects as BHs or NSs. For these binaries, LISA will also be able to determine their 3-dimensional position in the Milky Way. The LISA-detected sample of these double compact objects will provide new information about the galactic population of BHs and NSs, the star formation history of the Milky Way and the astrophysical processes leading to the formation of these systems. However, for a significant fraction of the LISA-detected binaries the nature of their constituent objects may remain unclear.