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Kinematics of M dwarfs in the CARMENES Input Catalogue: Membership in Young Moving Groups

Published online by Cambridge University Press:  27 January 2016

D. Montes ,
J. A. Caballero ,
I. Gallardo ,
M. Cortés-Contreras  and
F. J. Alonso-Floriano
D. Montes
Affiliation:
Dpto. Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain email: [email protected]
J. A. Caballero
Affiliation:
Centro de Astrobiologia (CSIC-INTA), Campus ESAC, PO Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain
I. Gallardo
Affiliation:
Dpto. Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain email: [email protected]
M. Cortés-Contreras
Affiliation:
Dpto. Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain email: [email protected]
F. J. Alonso-Floriano
Affiliation:
Dpto. Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain email: [email protected]
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Abstract

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We present a detailed study of the kinematics of M dwarfs in the CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs) input catalog. We have selected all M dwarfs with known parallactic distance or a good photometric distance estimation, precise proper motion in the literature or as determined by us, and radial velocity measurements. Using these parameters, we computed the M dwarfs galactic space motions (U, V, W). For the stars with U and V velocity components inside or near the boundaries that determine the young disk population, we have analyzed the possible membership in the classical moving groups and nearby loose associations with ages between 10 and 600 Myr. For the candidate members, we have compiled information available in the literature in order to constrain their membership by applying other age-dating methods.

Keywords

Galaxy: open clusters and associationsStars: kinematics and dynamicsStars: late-typeproper motions
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 71 - 72
Copyright
Copyright © International Astronomical Union 2016 

References

Alonso-Floriano, F. J., Morales, J. C., Caballero, J. A., et al. 2015, A&A, 577, A128Google Scholar
Cortés-Contreras, M., Caballero, J. A., & Montes, D. 2014, The Observatory, 134, 348Google Scholar
Eggen, O. J. 1989, PASP, 101, 366Google Scholar
Lépine, S. & Shara, M. M. 2005, AJ, 129, 1483CrossRefGoogle Scholar
Klutsch, A., Freire Ferrero, R., Guillout, P., et al. 2014, A&A, 567, A52Google Scholar
Montes, D., López-Santiago, J., Gálvez, M. C., et al. 2001, MNRAS, 328, 45CrossRefGoogle Scholar
Montes, D. 2010, IAU Special Session SpS7, Highlights of Astronomy, 15, E1Google Scholar
Montes, D. 2015, Highlights of Spanish Astrophysics VIII, p. 606Google Scholar
Passegger, V. M., Wende, S., Reiners, A. 2104, Proceedings of Towards other Earths IIGoogle Scholar
Quirrenbach, A., Amado, P. J., Caballero, J. A., et al. 2014, SPIE Proceeding, 9147, 91471FGoogle Scholar