论文标题
用进攻性数值相对性替代波形模型对GW190412进行了改进的分析
Improved analysis of GW190412 with a precessing numerical relativity surrogate waveform model
论文作者
论文摘要
Ligo-Virgo合作（LVC）最近对GW190412的观察是第一个高质量比率二进制黑洞（BBH）合并，这为探测在重力波信号中编码的亚抑制谐波和预衰局的影响提供了独特的机会。我们使用\ texttt {NRSUR7DQ4}介绍了GW190412的源参数的精制估计，这是一个最近开发的数值相对性波形替代模型，其中包括所有$ \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell \ ell spin-propen-spin-temeded spherical sheric谐波模式以及进餐的全部物理效应。我们将结果与现象学进攻BBH波形模型的两个不同变体进行比较，\ texttt {imrphenompv3hm}和\ texttt {imrphenomxphm}以及LVC结果。我们的结果与\ texttt {imrphenomxphm}的结果一致，并且与\ texttt {seobnrv4phm}波形模型一起编制的报告LVC分析，但与\ texttt {imrphenompv3hm}的张力。使用\ texttt {NRSUR7DQ4}模型，我们对质量比率（$ 0.26^{+0.08} _ { - 0.06} $）进行了更严格的约束，而LVC估计值则为$ 0.28^{+0.13} _ {+0.13} _ { - 0.07} $（两者都报道为90 creds creds creds creds creds creds creds creds creds creds creds creds creds ndress Inters credian credian vers）。我们还将二进制限制为更多面对面，并为自旋进动参数找到更广泛的后部。我们进一步发现，即使$ \ ell = 4 $谐波模式具有可忽略不计的信噪比，但这些模式的遗漏也会影响几个源参数的估计后验分布，包括Chirp质量，有效的Inspiral Spin，亮度距离，亮度距离和倾斜度。我们还发现，常用的模型近似值，例如忽略不对称模式（通常在进动过程中是兴奋的），对与GW190412类似的中度SNR事件的参数恢复具有可忽略的影响。
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 ($0.26^{+0.08}_{-0.06}$) as compared to the LVC estimate of $0.28^{+0.13}_{-0.07}$ (both reported as median values withs 90\% credible intervals). We also 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 (which are generically excited during precession), have negligible impact on parameter recovery for moderate SNR-events similar to GW190412.
