标题： 暗双中子星引力波的群体、宇宙学和中子星状态方程的联合推断 显示英文标题

标题： Joint Inference of Population, Cosmology, and Neutron Star Equation of State from Gravitational Waves of Dark Binary Neutron Stars

摘要： 引力波（GWs）来自双中子星（BNSs），通常会伴随电磁（EM）辐射，这有助于识别宿主星系。 由于GW事件可以直接测量其光度距离，BNS的联合GW-EM观测有助于研究宇宙学，特别是不受宇宙距离阶梯系统误差影响的哈勃常数。 然而，从BNS合并中检测EM对应体并不总是可行的。 此外，BNS组分的潮汐形变提供了关于中子星（NS）状态方程（EoS）的见解。 在这些情况下，结合NS状态方程知识的NS潮汐参数可以打破质量参数和红移之间的退化，从而推断哈勃常数。 一些研究试图利用没有EM对应体的BNS潮汐参数来推断哈勃常数，这类BNS被称为暗BNS。 此外，一些研究集中在对种群和NS状态方程的联合估计，以实现无偏的NS状态方程估计。 然而，目前的研究尚未在贝叶斯框架内一致结合种群、宇宙学和NS状态方程的不确定性。 在本研究中，我们提出了一种新颖的贝叶斯分析方法，利用通过GW观测检测到的暗BNS种群来联合约束NS状态方程、种群和宇宙学参数。 这种方法可以仅使用当前一代探测器的$5$个BNS观测很好地限制哈勃常数。 在没有NS状态方程的情况下，这种精度是无法实现的，尤其是在观测没有EM对应体信息的BNS合并时。 显示英文摘要

摘要： Gravitational waves (GWs) from binary neutron stars (BNSs) are expected to be accompanied by electromagnetic (EM) emissions, which help to identify the host galaxy. Since GW events directly measure their luminosity distances, joint GW-EM observations from BNSs help to study cosmology, particularly the Hubble constant, unaffected by cosmic distance ladder systematics. However, detecting EM counterparts from BNS mergers is not always possible. Additionally, the tidal deformations of BNS components offer insights into the neutron star (NS) equation of state (EoS). In such cases, the tidal parameters of NSs, combined with the knowledge of the NS EoS, can break the degeneracy between mass parameters and redshift, allowing for the inference of the Hubble constant. Several efforts have aimed to infer the Hubble constant using the tidal parameters of BNSs, without EM counterparts, termed dark BNSs. Moreover, some studies have focused on the joint estimation of population and NS EoS for unbiased NS EoS estimation. However, none of the works consistently combined the uncertainties of population, cosmology, and NS EoS within a Bayesian framework. In this study, we propose a novel Bayesian analysis to jointly constrain the NS EoS, population, and cosmological parameters using a population of dark BNSs detected through GW observations. This method can well constrain the Hubble constant with as few as $5$ BNS observations using current-generation detectors. This level of precision is unattainable without incorporating the NS EoS, especially when observing BNS mergers without EM counterpart information.