J/A+A/591/A37 Gaia-ESO Survey. Parameters for cluster members (Jacobson+, 2016)
The Gaia-ESO Survey: Probes of the inner disk abundance gradient.
Jacobson H.R., Friel E.D., Jilkova L., Magrini L., Bragaglia A.,
Vallenari A., Tosi M., Randich S., Donati P., Cantat-Gaudin T., Sordo R.,
Smiljanic R., Overbeek J.C., Carraro G., Tautvaisiene G., San Roman I.,
Villanova S., Geisler D., Munoz C., Jimenez-Esteban F., Tang B.,
Gilmore G., Alfaro E.J., Bensby T., Flaccomio E., Koposov S.E.,
Korn A.J., Pancino E., Recio-Blanco A., Casey A.R., Costado M.T.,
Franciosini E., Heiter U., Hill V., Hourihane A., Lardo C., de Laverny P.,
Lewis J., Monaco L., Morbidelli L., Sacco G.G., Sousa S.G., Worley C.C.,
Zaggia S.
<Astron. Astrophys. 591, A37 (2016)>
=2016A&A...591A..37J 2016A&A...591A..37J (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Abundances ; Radial velocities ;
Effective temperatures
Keywords: Galaxy: formation - Galaxy: disk - Galaxy: abundances -
stars: abundances
Abstract:
The nature of the metallicity gradient inside the solar circle
(RGC<8kpc) is poorly understood, but studies of Cepheids and a small
sample of open clusters suggest that it steepens in the inner disk. We
investigate the metallicity gradient of the inner disk using a sample
of inner disk open clusters that is three times larger than has
previously been studied in the literature to better characterize the
gradient in this part of the disk. We used the Gaia-ESO Survey (GES)
[Fe/H] values and stellar parameters for stars in 12 open clusters in
the inner disk from GES-UVES data. Cluster mean [Fe/H] values were
determined based on a membership analysis for each cluster. Where
necessary, distances and ages to clusters were determined via
comparison to theoretical isochrones. The GES open clusters exhibit a
radial metallicity gradient of -0.10±0.02dex/kpc, consistent with
the gradient measured by other literature studies of field red giant
stars and open clusters in the range RGC∼6-12kpc. We also measure a
trend of increasing [Fe/H] with increasing cluster age, as has also
been found in the literature. We find no evidence for a steepening of
the inner disk metallicity gradient inside the solar circle as earlier
studies indicated. The age-metallicity relation shown by the clusters
is consistent with that predicted by chemical evolution models that
include the effects of radial migration, but a more detailed
comparison between cluster observations and models would be premature.
Description:
Parameters for confirmed stellar members of the open clusters Berkeley
44, Berkeley 81, NGC 2516, NGC 3532, NGC 4815, NGC 6005, NGC 6633,
NGC 6705, NGC 6802, Pismis 18, Trumpler 20, Trumpler 23.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 97 155 Parameters for 155 stars in 12 open clusters
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Cluster Cluster name
13- 28 A16 --- Star GES ID (HHMMSSss+DDMMSSs)
31- 41 F11.7 deg RAdeg Right ascension (J2000.0)
44- 54 F11.7 deg DEdeg Declination (J2000.0)
57- 61 F5.2 [-] [Fe/H] Metallicity
64- 67 F4.2 [-] e_[Fe/H] Uncertainty on [Fe/H]
70- 73 I4 K Teff Effective temperature
76- 78 I3 K e_Teff Uncertainty on Teff
81- 84 F4.2 [cm/s2] logg Surface gravity
87- 90 F4.2 [cm/s2] e_logg Uncertainty on surface gravity
93- 97 F5.1 km/s RV Radial velocity
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Acknowledgements:
Heather Jacobson, hrj(at)mit.edu
(End) Patricia Vannier [CDS] 13-May-2016