Radial Velocity Planet Search

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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.