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The relation between velocity dispersions and chemical abundances in RAVE giants

Published online by Cambridge University Press:  07 March 2018

Rodolfo Smiljanic Open the ORCID record for Rodolfo Smiljanic [Opens in a new window]  and
Rafael Silva de Souza
Rodolfo Smiljanic
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716, Warsaw, Poland email: [email protected]
Rafael Silva de Souza
Affiliation:
MTA Eötvös University, EIRSA “Lendulet” Astrophysics Research Group, Budapest 1117, Hungary email: [email protected]
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Abstract

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We developed a Bayesian framework to determine in a robust way the relation between velocity dispersions and chemical abundances in a sample of stars. Our modelling takes into account the uncertainties in the chemical and kinematic properties. We make use of RAVE DR5 radial velocities and abundances together with Gaia DR1 proper motions and parallaxes (when possible, otherwise UCAC4 data is used). We found that, in general, the velocity dispersions increase with decreasing [Fe/H] and increasing [Mg/Fe]. A possible decrease in velocity dispersion for stars with high [Mg/Fe] is a property of a negligible fraction of stars and hardly a robust result. At low [Fe/H] and high [Mg/Fe] the sample is incomplete, affected by biases, and likely not representative of the underlying stellar population.

Keywords

Stars: abundancesStars: kinematicsGalaxy: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 259 - 260
Copyright
Copyright © International Astronomical Union 2018 

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