The joint observation of the gravitational-wave and electromagnetic signal from the binary neutron-star merger GW170817 allowed for a new independent measurement of the Hubble constant $H_0$, albeit with an uncertainty of about 15\% at 1$σ$. Observations of similar sources with a network of future detectors will allow for more precise measurements of $H_0$. These, however, are currently largely limited by the intrinsic degeneracy between the luminosity distance and the inclination of the source in the gravitational-wave signal. We show that the higher-order modes in gravitational waves can be used to break this degeneracy in astrophysical parameter estimation in both the inspiral and post-merger phases of a neutron star merger. We show that for systems at distances similar to GW170817, this method enables percent-level measurements of $H_0$ with a single detection. This would permit the study of time variations and spatial anisotropies of $H_0$ with unprecedented precision. We investigate how different network configurations affect measurements of $H_0$, and discuss the implications in terms of science drivers for the proposed 2.5- and third-generation gravitational-wave detectors. Finally, we show that the precision of $H_0$ measured with these future observatories will be solely limited by redshift measurements of electromagnetic counterparts.
Estimation of the Hubble parameter from unedited compact object merger catalogues
Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo（东京大学理学研究科早期宇宙研究中心）；Department of Physics, Graduate School of Science, The University of Tokyo（东京大学理学研究科物理系）；University of British Columbia（不列颠哥伦比亚大学）
Hubble constant measurement with 13 bright standard sirens from binary black hole mergers inside active galactic nuclei
Beijing Institute of Mathematical Sciences and Applications（北京数学与应用研究所）；Department of Physics, National Institute of Technology Agartala（阿加塔拉国立理工学院物理系）；Institute for Gravitation and the Cosmos, Department of Physics, Pennsylvania State University（宾夕法尼亚州立大学引力与宇宙学研究所）；National Institute of Technology Agartala（阿加塔拉国立理工学院）
The Stochastic Siren: Astrophysical Gravitational-Wave Background Measurements of the Hubble Constant
University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Illinois Center for Advanced Studies of the Universe, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校宇宙高级研究中心）；The University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, The University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）
Towards a few percent measurement of the Hubble constant with the current network of gravitational wave detectors without using electromagnetic information
A Pixelated Approach to Galaxy Catalogue Incompleteness: Improving the Dark Siren Measurement of the Hubble Constant
利用引力波标准警报器进行宇宙学分析已成为众所周知的事情，人们对测量哈勃常数$H_0$特别感兴趣，并对当前早期和晚期测量之间的紧张关系进行了说明。目前的紧张局势是超过$4σ$和标准警报器将能够提供一个完全独立的测量。暗警报（没有电磁对应物的双黑洞或中子星合并）可以提供信息，如果丢失的红移信息通过使用星系目录来识别合并的潜在宿主星系。然而，星系目录的不完整性影响这一分析，它的准确建模是必不可少的$H_0$获得一个公正的测量。以前，这是通过假设引力波事件的天空区域内的均匀完整性来实现的。本文提出了一种更新的方法，其中的星系目录的完整性估计在一个方向依赖的问题，通过像素化的天空和计算的完整性的星系目录沿每条视线。单个事件的$H_0$推断是在逐像素的基础上执行的，并且像素被组合以获得最终结果。对第一个引力波瞬变目录（GWTC-1）中的事件进行重新分析，结果表明，与等效LIGO和Virgo结果的68.3%最高密度间隔相比，$H_0$的测量值提高了约5%，$H_0$的测量值为$H_0= 68.8^{+15.9}_{-7.8}$ km s $^{-1}$ Mpc $^{-1}$。
What do gravitational-wave observations tell us about Luminous Red Novae?
Aryabhatta Research Institute of Observational Sciences (ARIES)（阿亚巴塔观测科学研究所）；Department of Applied Physics, Mahatma Jyotibha Phule Rohilkhand University（马哈特玛·乔蒂巴·普勒罗希尔坎德大学应用物理系）；Inter-University Centre for Astronomy and Astrophysics（大学间天文学与天体物理学中心）；Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham（伯明翰大学引力波天文台及物理与天文学学院）；Bareilly College, Mahatma Jyotibha Phule Rohilkhand University（马哈特玛·乔蒂巴·普勒罗希尔坎德大学巴雷利学院）；Chennai Mathematical Institute（金奈数学研究所）
