发表机构
Max Planck Institute for Gravitational Physics (Albert Einstein Institute); Leibniz University Hannover; Jet Propulsion Lab, California Institute of Technology; Theoretical Astrophysics, California Institute of Technology（马克斯·普朗克引力物理研究所（爱因斯坦研究所）; 汉诺威莱布尼茨大学; 加州理工学院喷气推进实验室; 加州理工学院理论天体物理学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过对比LALSuite与PINT的计时模型，验证了LALSuite计时模型的精度，推导了计时误差与信号功率损失的关系，测试了双星延迟并讨论了太阳内部信号的夏皮罗延迟。
AI 中文摘要
我们针对连续引力波的计时模型，开展了对现代高精度脉冲星计时软件包PINT的系统验证，结果如下。精确的计时模型对跟踪信号相位至关重要，是探测和精准表征连续引力波的基础。为量化计时不精确性的影响，我们推导并验证了 leading-order 关系 $\u03bc \u2248 (2\u03c0 f)^2\u03c3_\u03c4^2$，其中 $\u03bc$ 为信号功率的分数损失，$f$ 为信号频率，$\u03c3_\u03c4^2$ 为计时误差的方差。随后，我们对比了LALSuite计时模型中的太阳系和双星分量与PINT对应模型的差异。采用原始LALSuite爱因斯坦延迟实现时，总差异由该分量主导，$\u03c3_\u03c4 \u2248 \text{2.3}\u00b5\text{s}$（对应 $f=\text{1000 Hz}$ 时，$\u03bc \u2248 \text{0.02%}$）；采用更新的爱因斯坦延迟实现时，一年总差异降至 $\u03c3_\u03c4 \u2264 \text{31 ns}$（对应 $f=\text{1000 Hz}$ 时，$\u03bc \u2264 \text{4e-8}$），且差异由LALSuite采用近似地球自转模型导致的天文台对罗默延迟的贡献主导。我们还使用474个已编目双脉冲星的轨道参数测试双星延迟，验证了LALSuite源时间导数的自洽性。最后，我们推导并讨论了LALSuite针对穿过太阳内部的信号的夏皮罗延迟，该情况仅与引力波相关。
英文摘要
We present results of a systematic validation of the \lalsuite{} timing model for continuous gravitational waves against \pint{}, a modern high-accuracy pulsar-timing package. An accurate timing model is essential for tracking the signal phase, and hence for detecting and accurately characterizing continuous gravitational waves. In order to quantify the impact of timing inaccuracies, we derive and validate the leading-order relation $μ\approx (2πf)^2\stddtau^2$, where $μ$ is the fractional loss of signal power, $f$ is the signal frequency, and $\stddtau^2$ is the variance of the timing errors. We then compare the solar-system and binary components of the \lalsuite{} timing model against the corresponding models in \pint{}. With the original \lalsuite{} Einstein-delay implementation, the total disagreement is dominated by that component and has $\stddtau\simeq\SI{2.3}{\micro\second}$ (corresponding to $μ\simeq\SI{0.02}{\percent}$ at $f=\SI{1000}{\hertz}$). With the newer Einstein-delay implementation, the total disagreement (over one year) drops to $\stddtau\lesssim\SI{31}{\nano\second}$ (or $μ\lesssim\num{4e-8}$ at $f=\SI{1000}{\hertz}$) and is dominated by the observatory contribution to the \Romer{} delay, owing to the approximate Earth-rotation model used by \lalsuite{}. We additionally test binary delays using orbital parameters from \num{474} catalogued binary pulsars and verify the self-consistency of the \lalsuite{} source-time derivatives. Finally, we derive and discuss the \lalsuite{} Shapiro delay for signals passing through the solar interior, a case only relevant to gravitational waves.
