Improved analysis of GW190412 with a precessing numerical relativity surrogate waveform model
Improved analysis of GW190412 with a precessing numerical relativity surrogate waveform model
复制标题
DOI：
10.1103/physrevd.103.104027
复制
发表时间：
2020-10
期刊：
影响因子：
--
通讯作者：
Tousif Islam;Scott E. Field;C. Haster;Rory J. E. Smith
中科院分区：
文献类型：
--
作者：
Tousif Islam;Scott E. Field;C. Haster;Rory J. E. Smith
LIGO-Virgo合作项目（LVC）最近对GW190412的观测为探测引力波信号中编码的次谐波和进动效应的影响提供了一个独特的机会。GW190412是第一个高质量比双黑洞（BBH）并合。我们使用\texttt{NRSur7dq4对GW190412的源参数进行了精细估计，NRSur7dq4}是一个最近开发的数值相对论波形替代模型，包括所有$\ell \leq 4$自旋加权球谐模以及进动的全部物理效应。我们将结果与两种不同的现象处理BBH波形模型\texttt{IMRPhenomPv3HM}和\texttt{IMRPhenomXPHM}以及LVC结果进行了比较。我们的结果与\texttt{IMRPhenomXPHM}的结果以及用\texttt{SEOBNRv4PHM}波形模型编译的LVC分析大致一致，但与\texttt{IMRPhenomPv3HM}的结果不一致。使用\texttt{NRSur7dq4}模型，与$0.28^{+0.13}_{-0.07}$的LVC估计相比，我们对质量比（$0.26^{+0.07}_{-0.05}$）提供了更严格的约束（两者都报告为具有90％可信区间的中位数）。我们推断光度距离$\sim 4 \%$比用现象学模型和引用的LVC结果估计的值更大，约束双星更加正面，并为自旋进动参数找到更宽的后验。我们进一步发现，尽管$\ell=4$谐波模式的信噪比可以忽略不计，但忽略这些模式将影响几个源参数的估计后验分布，包括啁啾质量、有效自旋、光度距离和倾角。我们还发现，对于类似GW190412的中等信噪比事件，通常使用的模型近似，例如忽略非对称模态（在进动期间激发），对参数恢复的影响可以忽略不计。
The recent observation of GW190412, the first high-mass ratio binary black-hole (BBH) merger, by the LIGO-Virgo Collaboration (LVC) provides a unique opportunity to probe the impact of subdominant harmonics and precession effects encoded in a gravitational wave signal. We present refined estimates of source parameters for GW190412 using \texttt{NRSur7dq4}, a recently developed numerical relativity waveform surrogate model that includes all $\ell \leq 4$ spin-weighted spherical harmonic modes as well as the full physical effects of precession. We compare our results with two different variants of phenomenological precessing BBH waveform models, \texttt{IMRPhenomPv3HM} and \texttt{IMRPhenomXPHM}, as well as to the LVC results. Our results are broadly in agreement with \texttt{IMRPhenomXPHM} results and the reported LVC analysis compiled with the \texttt{SEOBNRv4PHM} waveform model, but in tension with \texttt{IMRPhenomPv3HM}. Using the \texttt{NRSur7dq4} model, we provide a tighter constraint on the mass-ratio ($0.26^{+0.07}_{-0.05}$) as compared to the LVC estimate of $0.28^{+0.13}_{-0.07}$ (both reported as median values withs 90\% credible intervals). We infer the luminosity distance to be $\sim 4 \%$ larger than the estimated values with phenomenological models and the quoted LVC result, constrain the binary to be more face-on, and find a broader posterior for the spin precession parameter. We further find that even though $\ell=4$ harmonic modes have negligible signal-to-noise ratio, omission of these modes will influence the estimated posterior distribution of several source parameters including chirp mass, effective inspiral spin, luminosity distance, and inclination. We also find that commonly used model approximations, such as neglecting the asymmetric modes (excited during precession), have negligible impact on parameter recovery for moderate SNR-events similar to GW190412.