Poster - Splinter Exoplanets

Masses and radii of the CARMENES target stars

A. Schweitzer1, V. Bejar2, J. Caballero3, C. Cifuentes4 C. del~Burgo5, D. Montes4, V. Passegger6, E. Solano3, A. Reiners6, I. Ribas7
and the CARMENES consortium
1Hamburger Sternwarte, Universität Hamburg
2Instituto de Astrofisica de Canarias, La Laguna, Spain
3Centro de Astrobiologia, Departamento de Astrofisica, Madrid, Spain
4Departamento de Astrofisica, Universidad Complutense de Madrid, Spain
5Instituto Nacional de Astrofisica, Optica y Electronica, Tonantzintla, Mexico
6Institut für Astrophysik, Georg-August-Universität Göttingen
7Institut de Ciencies de l'Espai, Barcelona, Spain

The mass of an individual, isoloated star can typically only be determined within large error bars. However, in order to also estimate the mass of a potential planetary companion it is crucial to have a small error bar for the mass of the host star. For the CARMENES survey we implement different spectroscopic methods of determening the masses of its targets. Since the CARMENES targets are all nearby M~dwarfs, they have or soon will have accurate trigonometric parallaxes. This allows us to determine luminosities, radii and finally masses. Depending on which spectroscopic parameters (T_eff, \log (g)) are used, which way of estimating B.C. is employed and which further (empirical) relations need to be applied, we get different accuracies for our results. They are further compared to empirical mass-luminosity relations or (if possible) to independent measurements.