We perform Bayesian analysis of gravitational-wave signals from non-spinning, intermediate-mass black-hole binaries (IMBHBs) with observed total mass, $M_{\mathrm{obs}}$, from $50\mathrm{M}_{\odot}$ to $500\mathrm{M}_{\odot}$ and mass ratio $1\mbox{--}4$ using advanced LIGO and Virgo detectors. We employ inspiral-merger-ringdown waveform models based on the effective-one-body formalism and include subleading modes of radiation beyond the leading $(2,2)$ mode. The presence of subleading modes increases signal power for inclined binaries and allows for improved accuracy and precision in measurements of the masses as well as breaking of extrinsic parameter degeneracies. For low total masses, $M_{\mathrm{obs}} \lesssim 50 \mathrm{M}_{\odot}$, the observed chirp mass $\mathcal{M}_{\rm obs} = M_{\mathrm{obs}}\,η^{3/5}$ ($η$ being the symmetric mass ratio) is better measured. In contrast, as increasing power comes from merger and ringdown, we find that the total mass $M_{\mathrm{obs}}$ has better relative precision than $\mathcal{M}_{\rm obs}$. Indeed, at high $M_{\mathrm{obs}}$ ($\geq 300 \mathrm{M}_{\odot}$), the signal resembles a burst and the measurement thus extracts the dominant frequency of the signal that depends on $M_{\mathrm{obs}}$. Depending on the binary's inclination, at signal-to-noise ratio (SNR) of $12$, uncertainties in $M_{\mathrm{obs}}$ can be as large as $\sim 20 \mbox{--}25\%$ while uncertainties in $\mathcal{M}_{\rm obs}$ are $\sim 50 \mbox{--}60\%$ in binaries with unequal masses (those numbers become $\sim 17\%$ versus $\sim22\%$ in more symmetric binaries). Although large, those uncertainties will establish the existence of IMBHs. Our results show that gravitational-wave observations can offer a unique tool to observe and understand the formation, evolution and demographics of IMBHs, which are difficult to observe in the electromagnetic window. (abridged)
A Hamiltonian Monte Carlo method for Bayesian Inference of Supermassive Black Hole Binaries
本文研究了利用Hamilton Monte Carlo方法计算超大质量黑洞双星的后验密度函数。虽然以前的马尔可夫链蒙特卡罗（MCMC）方法，如Metropolis-Hastings MCMC，已成功地用于许多不同的引力波源，这些方法基本上是随机游走算法。哈密顿蒙特卡罗将逆似然曲面视为“引力势”，并通过引入正则位置和动量，通过求解哈密顿运动方程动态地演化马尔可夫链。我们提出了一种实现的哈密顿马尔可夫链，是更快，更有效的一个因素的参数空间的尺寸，比标准的MCMC。
Probing missing physics from inspiralling compact binaries via time-frequency tracks
Fudan University（复旦大学）；Université Catholique de Louvain（天主教鲁汶大学）；Royal Observatory of Belgium（比利时皇家天文台）；Indian Institute of Technology Gandhinagar（甘地纳加尔印度理工学院）；New Uzbekistan University（新乌兹别克斯坦大学）
Assessing signal cross talk between extreme-mass-ratio inspirals and Galactic binaries in LISA data
Argelander Institut für Astronomie, Universität Bonn（波恩大学阿根兰德天文研究所）；Astroparticule et Cosmologie, CNRS, Université Paris Cité（巴黎 Cité 大学国家科学研究中心天体粒子与宇宙学）
