The Gaia-ESO Survey: New constraints on the Galactic disc velocity dispersion and its chemical dependencies⋆
Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte
d’Azur, CNRS, Boulevard de l’Observatoire,
Nice Cedex 4,
2 Leibniz-Institut für Astrophysik Potsdam (AIP) An der Sternwarte 16, 14482 Potsdam, Germany
3 Physics and Astronomy Department, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
5 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Florence, Italy
6 Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, 221 00 Lund, Sweden
7 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
8 Moscow MV Lomonosov State University, Sternberg Astronomical Institute, 119992 Moscow, Russia
9 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy ASI Science Data Center, via del Politecnico SNC, 00133 Roma, Italy
10 Instituto de Física y Astronomía, Universidad de Valparaíso, 2360102 Valparaíso, Chile
11 Instituto de Astrofísica de Andalucía-CSIC, Apdo. 3004, 18080 Granada, Spain
12 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK
13 Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden
14 INAF–Padova Observatory, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
Received: 13 February 2015
Accepted: 26 August 2015
Context. Understanding the history and the evolution of the Milky Way is one of the main goals of modern astrophysics. In particular, the formation of the Galactic disc is a key problem of Galactic archaeology.
Aims. We study the velocity dispersion behaviour of Galactic disc stars as a function of the [Mg/Fe] ratio, which for small metallicity bins can be used as a proxy of relative age. This key relation is essential to constrain the formation mechanisms of the disc stellar populations as well as the cooling and settling processes.
Methods. We used the recommended parameters and chemical abundances of 7800 FGK Milky Way field stars from the second internal data release of the Gaia-ESO spectroscopic Survey. These stars were observed with the GIRAFFE spectrograph (HR10 and HR21 setups), and cover a large spatial volume in the intervals 6 <R< 10 kpc and | Z | < 2 kpc. Based on a chemical criterion, we separated the thin- from the thick-disc sequence in the [Mg/Fe] vs. [Fe/H] plane.
Results. From analysing the Galactocentric velocity of the stars for the thin disc, we find a weak positive correlation between Vφ and [Fe/H] that is due to a slowly rotating [Fe/H]-poor tail. For the thick disc stars, a strong correlation with [Fe/H] and [Mg/Fe] is established. In addition, we have detected an inversion of the velocity dispersion trends with [Mg/Fe] for thick-disc stars with [Fe/H] < −0.10 dex and [Mg/Fe] > +0.20 dex for the radial component. First, the velocity dispersion increases with [Mg/Fe] at all [Fe/H] ratios for the thin-disc stars, and then it decreases for the thick-disc population at the highest [Mg/Fe] abundances. Similar trends are observed for several bins of [Mg/Fe] within the errors for the azimuthal velocity dispersion, while a continuous increase with [Mg/Fe] is observed for the vertical velocity dispersion. The velocity dispersion decrease agrees with previous measurements of the RAVE survey, although it is observed here for a greater metallicity interval and a larger spatial volume.
Conclusions. Thanks to the Gaia-ESO Survey data, we confirm the existence of [Mg/Fe]-rich thick-disc stars with cool kinematics in the generally turbulent context of the primitive Galactic disc. This is discussed in the framework of the different disc formation and evolution scenarios.
Key words: Galaxy: abundances / Galaxy: disk / Galaxy: kinematics and dynamics / Galaxy: stellar content / stars: abundances
© ESO, 2015