Radial Velocity Planet Search

该研究项目是拟议的研究单位“红星周围的蓝色行星”的一部分。该研究单位的主要科学目标是探测M矮星周围的类地行星，这些行星位于所谓的可居住区，那里可以存在液态水。我们的项目将在CARMENES光谱仪提供的径向速度测量中寻找系外行星信号。这种分析将在光学和近红外径向速度测量上进行。围绕M矮星的行星预计很小（质量约为1-10个地球质量），并且处于多个系统中。这些行星将使用各种最先进的周期分析工具进行检测。M矮星可能是活跃的恒星，径向速度活动抖动可能会阻碍行星的检测。光学和近红外测量中发现的信号的比较将有助于区分活动信号和行星信号。为了探测最小的行星，我们将使用各种技术过滤掉活动信号。这项工作将与研究单位的项目P3（轮换和活动）密切合作。对于所有的行星信号，我们将拟合开普勒轨道，以获得准确的轨道参数和实际的误差估计。这些参数可以用于研究我们发现的行星系统的动力学稳定性（研究单位的项目P6）该研究项目的最终“交付物”将是CARMENES项目发现的所有已确认行星的列表。这些可以用来研究M矮星周围行星系统的结构。

This research project is part of the proposed research unit "Blue Planets around Red Stars". This research unit has the main science goal of detecting terrestrial planets around M dwarf stars that reside in the so-called habitable zone where liquid water can exist.Our project will search for exoplanet signals in the radial velocity measurements provided by the CARMENES spectrograph. This analysis will be performed on both the optical and near infrared radial velocity measurements. Planets around M dwarf stars are expected to be small (mass about 1-10 Earth masses) and in multiple systems. These planets will be detected using a variety of state-of-the-art period analysis tools.M dwarfs can be active stars and the radial velocity activity jitter can hinder the detection of planets. A comparison of the signals found in the optical and near infrared measurements will help distinguish between signals due to activity and those from planets. In order to detect the smallest planets we will filter out the activity signal using a variety of techniques. This work will be done in close collaboration with Project P3 (Rotation and Activity) of the research unit. For all the planet signals we will fit Keplerian orbits to derive accurate orbital parameters and realistic estimates of their errors. These parameters can then be used for studies of the dynamical stability of the planetary systems that we find (Project P6 of the research unit)The final "deliverables'' of this research project will be the list of all confirmed planets found by the CARMENES project. These can be used to study the architecture of planetary systems around M dwarf stars.