1 cm/s时的重心校正，用于精确的多普勒速度
Barycentric Corrections at 1 cm/s for precise Doppler velocities
摘要：
本文的目的是建立一个重心校正的要求与RMS的$\lesssim 1$厘米/秒，这是一个数量级优于真正的地球类似物（$\sim9$厘米/秒）的多普勒探测所需的。我们描述的理论和实施会计精确多普勒测量的望远镜通过空间的运动的影响，主要是从地球的旋转和轨道运动，以及太阳系相对于目标恒星的运动（即“重心校正”）。我们描述了实现这一点所需的最小算法，以及它与简单的速度减法（即伽利略变换）的不同之处。我们证明了代码的有效性，我们已经开发的加州行星调查代码通过比较脉冲星定时包，TEMPO 2。我们估计的各种条款和影响，包括相对论效应的大小，并与不完整的知识望远镜的位置，定时，恒星的位置和运动的错误。我们注意到，色差将在观测时间上造成不确定性，这将使探测真正的地球类似物的努力复杂化。我们的代码可供公众使用和验证。
英文摘要：
The goal of this paper is to establish the requirements of a barycentric correction with an RMS of $\lesssim 1$ cm/s, which is an order of magnitude better than necessary for the Doppler detection of true Earth analogs ($\sim9$ cm/s). We describe the theory and implementation of accounting for the effects on precise Doppler measurements of motion of the telescope through space, primarily from rotational and orbital motion of the Earth, and the motion of the solar system with respect to target star (i.e. the "barycentric correction"). We describe the minimal algorithm necessary to accomplish this and how it differs from a naïve subtraction of velocities (i.e. a Galilean transformation). We demonstrate the validity of code we have developed from the California Planet Survey code via comparison with the pulsar timing package, TEMPO2. We estimate the magnitude of various terms and effects, including relativistic effects, and the errors associated with incomplete knowledge of telescope position, timing, and stellar position and motion. We note that chromatic aberration will create uncertainties in the time of observation, which will complicate efforts to detect true Earth analogs. Our code is available for public use and validation.
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