OCCASO – II. Physical parameters and Fe abundances of red clump stars in 18 open clusters

Abstract Open clusters have long been used to study the chemodynamical evolution of the Galactic disc. This requires a homogeneously analysed sample covering a wide range of ages and distances. In this paper, we present the Open Clusters Chemical Abundances from Spanish Observatories (OCCASO) second...

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Published in:	Monthly notices of the Royal Astronomical Society 2017-10, Vol.470 (4), p.4363-4381
Main Authors:	Casamiquela, L, Carrera, R, Blanco-Cuaresma, S, Jordi, C, Balaguer-Núñez, L, Pancino, E, Anders, F, Chiappini, C, Díaz-Pérez, L, Aguado, D. S, Aparicio, A, Garcia-Dias, R, Heiter, U, Martínez-Vázquez, C. E, Murabito, S, del Pino, A
Format:	Article
Language:	eng
Subjects:	Clusters of galaxies Cúmuls de galàxies Espectroscòpia Galaxy: disc open clusters and associations: general Spectrum analysis techniques: spectroscopic
Online Access:	Get full text
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Summary:	Abstract Open clusters have long been used to study the chemodynamical evolution of the Galactic disc. This requires a homogeneously analysed sample covering a wide range of ages and distances. In this paper, we present the Open Clusters Chemical Abundances from Spanish Observatories (OCCASO) second data release. This comprises a sample of high-resolution (R > 65 000) and high signal-to-noise spectra of 115 red clump stars in 18 open clusters. We derive atmospheric parameters (T eff, log g, ξ), and [Fe/H] abundances using two analysis techniques: equivalent widths and spectral synthesis. A detailed comparison and a critical review of the results of the two methods are made. Both methods are carefully tested between them, with the Gaia FGK benchmark stars, and with an extensive sample of literature values. We perform a membership study using radial velocities and the resulting abundances. Finally, we compare our results with a chemodynamical model of the Milky Way thin disc concluding that the oldest open clusters are consistent with the models only when dynamical effects are taken into account.
ISSN:	0035-8711 1365-2966 1365-2966