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Chemo-dynamical signatures in simulated Milky Way-like galaxies

Published online by Cambridge University Press:  07 March 2018

Alessandro Spagna Open the ORCID record for Alessandro Spagna [Opens in a new window] ,
Anna Curir ,
Marco Giammaria ,
Mario G. Lattanzi ,
Giuseppe Murante  and
Paola Re Fiorentin
Alessandro Spagna
Affiliation:
INAF – Osservatorio Astrofisico di Torino via Osservatorio 20, 10025 Pino Torinese, Italy email: spagna@oato.inaf.it
Anna Curir
Affiliation:
INAF – Osservatorio Astrofisico di Torino via Osservatorio 20, 10025 Pino Torinese, Italy email: spagna@oato.inaf.it
Marco Giammaria
Affiliation:
Universitá degli Studi di Torino, Italy
Mario G. Lattanzi
Affiliation:
INAF – Osservatorio Astrofisico di Torino via Osservatorio 20, 10025 Pino Torinese, Italy email: spagna@oato.inaf.it
Giuseppe Murante
Affiliation:
INAF – Osservatorio Astronomico di Trieste, Italy
Paola Re Fiorentin
Affiliation:
INAF – Osservatorio Astrofisico di Torino via Osservatorio 20, 10025 Pino Torinese, Italy email: spagna@oato.inaf.it
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Abstract

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We have investigated the chemo-dynamical evolution of a Milky Way-like disk galaxy, AqC4, produced by a cosmological simulation integrating a sub-resolution ISM model. We evidence a global inside-out and upside-down disk evolution, that is consistent with a scenario where the “thin disk” stars are formed from the accreted gas close to the galactic plane, while the older “thick disk” stars are originated in situ at higher heights. Also, the bar appears the most effective heating mechanism in the inner disk. Finally, no significant metallicity-rotation correlation has been observed, in spite of the presence of a negative [Fe/H] radial gradient.

Keywords

Galaxy: abundanceevolutionstructurekinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 263 - 264
Copyright
Copyright © International Astronomical Union 2018 

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