论文标题
区分高质量二进制中子星和具有第二代和第三代引力波观测站的二进制黑洞
Distinguishing high-mass binary neutron stars from binary black holes with second- and third-generation gravitational wave observatories
论文作者
论文摘要
（删节）虽然重力波（GW）信号GW170817伴随着各种电磁（EM）对应物，但预计足够高的二进制中子星（BNS）合并有望无法为Bright EM对应物供电。推定的高质量二进制BNS合并GW190425（尚未确定EM对应物）可能是这种系统的一个例子。因此，重要的是要了解我们将如何能够将高质量的BNS和低质量二元黑洞（BBH）与GW信号区分开。为此，我们考虑了中子星在GW信号上的潮汐变形性的烙印，用于合并后迅速发生黑洞形成的系统。我们使用杂交数值相对论 - 潮汐有效的一个体波形对BNS信号进行建模。具体而言，我们考虑一组五个非质量质量BNS信号，质量为2.7、3.0、3.2 MSUN，并且具有三个不同方程式状态以及类似的BBH信号。我们对三个网络中的这些信号进行参数估计：高级Ligo高级处女座和先进的Ligo-Advanced处女座-Kagra，分别具有类似于O3和O4的敏感性，以及两个宇宙探险家（CES）的3G网络（CES）和一个EINSTEIN望远镜，与CE的敏感性相似，我们的敏感性与我们的敏感性相似。即使在40 MPC的情况下，BBHS的可靠水平为90％。但是，我们可以使用O4型网络以40 MPC的> = 95％可信度的BBH区分我们在研究中考虑的所有最紧凑的BNS，甚至可以使用3G网络在369（835）MPC下以> 99.2％（> = 97％）可信的水平来区分它们。此外，我们提出了一种简单的方法，可以计算地球旋转对频域中重力检测器响应的主要作用。
(Abridged) While the gravitational-wave (GW) signal GW170817 was accompanied by a variety of electromagnetic (EM) counterparts, sufficiently high-mass binary neutron star (BNS) mergers are expected to be unable to power bright EM counterparts. The putative high-mass binary BNS merger GW190425, for which no confirmed EM counterpart has been identified, may be an example of such a system. It is thus important to understand how well we will be able to distinguish high-mass BNSs and low-mass binary black holes (BBHs) solely from their GW signals. To do this, we consider the imprint of the tidal deformability of the neutron stars on the GW signal for systems undergoing prompt black hole formation after merger. We model the BNS signals using hybrid numerical relativity -- tidal effective-one-body waveforms. Specifically, we consider a set of five nonspinning equal-mass BNS signals with masses of 2.7, 3.0, 3.2 Msun and with three different equations of state, as well as the analogous BBH signals. We perform parameter estimation on these signals in three networks: Advanced LIGO-Advanced Virgo and Advanced LIGO-Advanced Virgo-KAGRA with sensitivities similar to O3 and O4, respectively, and a 3G network of two Cosmic Explorers (CEs) and one Einstein Telescope, with a CE sensitivity similar to Stage 2. Our analysis suggests that we cannot distinguish the signals from high-mass BNSs and BBHs at a 90% credible level with the O3-like network even at 40 Mpc. However, we can distinguish all but the most compact BNSs that we consider in our study from BBHs at 40 Mpc at a >= 95% credible level using the O4-like network, and can even distinguish them at a > 99.2% (>= 97%) credible level at 369 (835) Mpc using the 3G network. Additionally, we present a simple method to compute the leading effect of the Earth's rotation on the response of a gravitational wave detector in the frequency domain.
