UCM Stellar Astrophysics Group

Our research is currently focused on the spectroscopic analysis of cool stars: spectral classification, radial and rotational velocity determinations, Li abundance, and analysis of the optical chromospheric activity indicators. Our research work was centred in different kind of cool stars including pre-main sequence stars, members of young open clusters, single young rapid rotators, flare stars and chromospherically active binaries. We have compiled different libraries of high and mid-resolution optical spectra of late-type stars (F, G, K and M field stars, from dwarfs to giants). We have been working in the spectroscopic characterization of late-type stars members of young stellar kinematic groups.The group participated on large international collaborations as the Herschel Open time Key Program: DUNES: DUst around NEarby Stars, the Gaia-ESO spectroscopic Survey (GES), and on instrumental projects as the high-resolution visible and near-infrared spectrograph CARMENES (3.5m telescope, Calar Alto, Almería) and the multi-object spectrograph WEAVE (4.2m William Herschel Telescope, La Palma). Related with the CARMENES project, the group is one of the members of international consortium and have been awarded with several coordinated projects dedicated to the construction of the instrument, the science preparation and currently another one dedicated to science exploitation. In addition, the group participates in several of the working groups dedicated to the scientific exploitation.

The main lines of research of the UCM Stellar Astrophysics group are:

(1) The characterization of the main properties of M dwarfs which are the targets of the main science goal of CARMENES instrument. The knowledge of the physical properties (fundamental stellar parameters, rotation, multiplicity, chromospheric activity and kinematics) are essential for the science exploitation of CARMENES in order to better characterize the discovered exoplanets and their atmospheres, to quantify the activity-induced radial velocity jitter, the star-planet interactions, and to carry out comparative planetology (i.e. relating planet properties to the astrophysical characteristics of their host stars). All the parameters determined in this way (level of non-thermal radiation, magnetic field, rotation, cycles, etc.) will allow better understanding the differences between dwarfs with different convective depth and fully convective stars and understanding the possible coexisting different dynamos.

(2) The determination of stellar parameters and abundances of the FGK stars of the Gaia-ESO spectroscopic Survey (GES) in order to kine-chemical tagging FGK stars with GES/UVES data in order to search for new members of stellar kinematic groups (SKGs). Using the radial velocities provided by the survey, the astrometry available in the literature and an estimation of the distance using our derived spectroscopic stellar parameters we will make a first kinematic selection of possible members to SKGs of difference ages. For these subsamples of stars a detailed differential abundance analysis (chemical tagging) and additional information derived from the spectra will allowed us to discern between real physical structures of coeval stars with a common origin and field-like stars.

Interested applicants should submit to the contact person
the following documents before the deadline:
(1) a cover letter with her/his research interests and the names of two referees
(2) a recent Curriculum Vitae, including a list of publications
(3) a research statement
(4) two reference letters