Volume 609, January 2018
|Number of page(s)||11|
|Section||Galactic structure, stellar clusters and populations|
|Published online||22 December 2017|
1 Department of PhysicsLancaster University LA1 4YB Lancaster UK
2 Zentrum für Astronomie der Universität Heidelberg, Astronomisches Recheninstitut, Mönchhofstr. 12, 69120 Heidelberg, Germany
3 Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101, USA
4 Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
5 Saint Martin’s University, Old Main, 5000 Abbey Way SE, Lacey, WA 98503, USA
Received: 22 June 2017
Accepted: 11 September 2017
Star clusters, particularly those objects in the disk-bulge-halo interface are as yet poorly charted, despite the fact that they carry important information about the formation and the structure of the Milky Way. Here, we present a detailed chemical abundance study of the recently discovered object Gaia 1. Photometry has previously suggested it as an intermediate-age, moderately metal-rich system, although the exact values for its age and metallicity remained ambiguous in the literature. We measured detailed chemical abundances of 14 elements in four red giant members, from high-resolution (R = 25 000) spectra that firmly establish Gaia 1 as an object associated with the thick disk. The resulting mean Fe abundance is −0.62 ± 0.03(stat.)± 0.10(sys.) dex, which is more metal-poor than indicated by previous spectroscopy from the literature, but it is fully in line with values from isochrone fitting. We find that Gaia 1 is moderately enhanced in the α-elements, which allowed us to consolidate its membership with the thick disk via chemical tagging. The cluster’s Fe-peak and neutron-capture elements are similar to those found across the metal-rich disks, where the latter indicate some level of s-process activity. No significant spread in iron nor in other heavy elements was detected, whereas we find evidence of light-element variations in Na, Mg, and Al. Nonetheless, the traditional Na-O and Mg-Al (anti-)correlations, typically seen in old globular clusters, are not seen in our data. This confirms that Gaia 1 is rather a massive and luminous open cluster than a low-mass globular cluster. Finally, orbital computations of the target stars bolster our chemical findings of Gaia 1’s present-day membership with the thick disk, even though it remains unclear which mechanisms put it in that place.
Key words: Stars: abundances / Galaxy: abundances / Galaxy: structure / open clusters and associations: individual: Gaia 1 / Galaxy: disk / globular clusters
This paper includes data gathered with the 2.5 meter du Pont Telescope located at Las Campanas Observatory, Chile.
Full Table 2 is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A13
© ESO, 2017
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