论文标题
由于合并二进制中子星的参数估计的偏心率，系统偏见
Systematic bias due to eccentricity in parameter estimation for merging binary neutron stars
论文作者
论文摘要
我们研究偏心率对二元中子星系重力波参数估计的影响。对于注入高级LIGO灵敏度的信号，我们使用圆形波形模型执行贝叶斯参数估计，并显示如何从其真实值中偏见恢复的参数，重点介绍chirp质量（$ m_c $）的内在参数，对称的质量比（$η$）和$ $ $（$η$）和$ themability（$η$）和$ tefors（$）。通过比较贝叶斯和分析的Fisher-Cutler-Vallisneri（FCV）方法之间的结果，我们获得了FCV方法的有效标准。采用FCV方法并使用分布在$ m_1 $ - $ m_2 $ - $ $ e_0 $空间中的二进制中子星源的现实种群，其中$ e_0 $表示偏心率在10Hz时，我们计算了测量误差（$σ_θ$），并获得$δch/σ_θ$的范围（$δch/σ_θ$） \ leq 0.025 $。我们发现，对于所有三个参数，偏差随着$ e_0 $的增加而增加，对于较大的$ e_0 $，这种增加速度更快。偏差主要取决于$ e_0 $的值和弱取决于组件质量，因此分布在$ e_0 $ - $δθ/σ_θ$平面中显示了一个狭窄的频段。我们提出了各种后示例，以说明我们的新发现，例如后代的双峰性。特别是，我们给出了一个特定的注射回收示例，以证明将偏心率包括在参数估计中以避免对状态的中子星方程的错误预测。
We study the impact of eccentricity on gravitational-wave parameter estimation for binary neutron star systems. For signals with small eccentricity injected into the advanced LIGO sensitivity, we perform Bayesian parameter estimation using the circular waveform model and show how the recovered parameters can be biased from their true values, focusing on the intrinsic parameters the chirp mass ($M_c$), the symmetric mass ratio ($η$), and the tidal deformability ($\tildeλ$). By comparing the results between the Bayesian and the analytic Fisher-Cutler-Vallisneri (FCV) methods, we obtain the valid criteria for the FCV approach. Employing the FCV method and using the realistic population of binary neutron star sources distributed in the $m_1$-$m_2$-$e_0$ space, where $e_0$ indicates the eccentricity at 10Hz, we calculate the measurement errors ($σ_θ$) and the systematic biases ($Δθ/σ_θ$) and obtain their generalized distributions in the range of $0 \leq e_0 \leq 0.025$. We find that for all of the three parameters, the biases increase with increasing $e_0$, and this increase is faster for larger $e_0$. The bias is mainly dependent on the value of $e_0$ and weakly dependent on the component masses, and thus the distribution shows a narrow band in the $e_0$-$Δθ/σ_θ$ plane. We present various posterior examples to illustrate our new findings, such as the bimodality of posteriors. In particular, we give a specific injection-recovery example to demonstrate the importance of including eccentricity in parameter estimation to avoid incorrect predictions of the neutron star equation of state.
