J/A+A/589/A115 Na and Al abundances of 1303 stars (Smiljanic+, 2016)
The Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs -
Implications for stellar and Galactic chemical evolution.
Smiljanic R., Romano D., Bragaglia A., Donati P., Magrini L., Friel E.,
Jacobson H., Randich S., Ventura P., Lind K., Bergemann M., Nordlander T.,
Morel T., Pancino E., Tautvaisiene G., Adibekyan V., Tosi M., Vallenari A.,
Gilmore G., Bensby T., Francois P., Koposov S., Lanzafame A. C.,
Recio-Blanco A., Bayo A., Carraro G., Casey A. R., Costado M. T.,
Franciosini E., Heiter U., Hill V., Hourihane A., Jofre P., Lardo C.,
de Laverny P., Lewis J., Monaco L., Morbidelli L., Sacco G. G.,
Sbordone L., Sousa S. G., Worley C. C., Zaggia S.
<Astron. Astrophys. 589, A115 (2016)>
=2016A&A...589A.115S 2016A&A...589A.115S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Stars, late-type ; Abundances
Keywords: Galaxy: abundances - Galaxy: evolution - stars: abundances -
stars: evolution - stars: late-type
Abstract:
Stellar evolution models predict that internal mixing should cause
some sodium overabundance at the surface of red giants more massive
than ∼1.5-2.0M{aun}. The surface aluminium abundance should not be
affected. Nevertheless, observational results disagree about the
presence and/or the degree of Na and Al overabundances. In addition,
Galactic chemical evolution models adopting different stellar yields
lead to very different predictions for the behavior of [Na/Fe] and
[Al/Fe] versus [Fe/H]. Overall, the observed trends of these
abundances with metallicity are not well reproduced.
We re-address both issues, using new Na and Al abundances determined
within the Gaia-ESO Survey. Our aim is to obtain better observational
constraints on the behavior of these elements using two samples: i)
more than 600 dwarfs of the solar neighborhood and of open clusters
and ii) low- and intermediate-mass clump giants in six open clusters.
Abundances were determined using high-resolution UVES spectra. The
individual Na abundances were corrected for nonlocal thermodynamic
equilibrium effects. For the Al abundances, the order of magnitude of
the corrections was estimated for a few representative cases. For
giants, the abundance trends with stellar mass are compared to stellar
evolution models. For dwarfs, the abundance trends with metallicity
and age are compared to detailed chemical evolution models.
Description:
File table1.dat contains atmospheric parameters and abundances, of
sodium and aluminium, of 1303 stars that are part of the second and
third internal releases of the Gaia-ESO Spectroscopic Survey.
Parameters and abundances were determined using high-resolution UVES
spectra. The spectrum analysis was carried out with the Gaia-ESO
multiple pipelines strategy as described in Smiljanic et al.
(2014A&A...570A.122S 2014A&A...570A.122S). Each parameter and abundance value is given
together with an estimate of the method-to-method dispersion and the
number of pipelines used for its computation. The individual Na
abundances are also given corrected for nonlocal thermodynamic
equilibrium (non-LTE) effects. The non-LTE Na abundances were computed
only for the stars part of the 'best-quality' sample, as described in
the paper (Section 2.3). The Al abundances are given only in LTE.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 133 1303 Atmospheric parameters and abundances
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See also:
J/A+A/572/A33 : Abundances from Gaia-ESO Survey (Mikolaitis+, 2014)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- GES-ID Gaia-ESO identification index
18- 28 A11 --- Field *Field where the star was observed
30- 39 F10.6 deg RAdeg ? Right ascension (J2000)
41- 50 F10.6 deg DEdeg ? Declination (J2000)
52- 55 I4 K Teff Effective temperature
57- 59 I3 K s_Teff Dispersion of multiple Teff measurements
61- 62 I2 --- o_Teff Number of different pipelines providing
Teff measurements
64- 67 F4.2 [cm/s2] logg Logarithm of the surface gravity
69- 72 F4.2 [cm/s2] s_logg Dispersion of multiple logg measurements
74- 75 I2 --- o_logg Number of different pipelines providing
logg measurements
77- 81 F5.2 [Sun] [Fe/H] *Metallicity
83- 86 F4.2 [Sun] s_[Fe/H] Dispersion of multiple [Fe/H] measurements
88- 89 I2 --- o_[Fe/H] Number of different pipelines providing
[Fe/H] measurements
91- 94 F4.2 km/s Xi ? Microturbulence velocity
96- 99 F4.2 km/s s_Xi ? Dispersion of multiple Xi measurements
101-102 I2 --- o_Xi ? Number of different pipelines providing
Xi measurements
104-107 F4.2 [-] A(Na) *? Abundance of Na in LTE
109-112 F4.2 [-] s_A(Na) ? Dispersion of multiple A(Na) measurements
114-115 I2 --- o_A(Na) ? Number of different pipelines providing
A(Na) measurements
117-120 F4.2 [-] A(Na)NLTE *? Abundance of Na in non-LTE
122-125 F4.2 [-] A(Al) *? Abundance of Al in LTE
127-130 F4.2 [-] s_A(Al) ? Dispersion of multiple A(Al) measurements
132-133 I2 --- o_A(Al) ? Number of different pipelines providing
A(Al) measurements
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Note on Field:
One of the following possibilities:
The name of the open cluster in which field the star was observed
A name of the star, in case of a bright star observed for calibration
purposes
GES MW, indicating that the star is part of one of the Gaia-ESO Milky Way
fields (solar neighbourhood, Bulge line of sight, or CoRoT fields).
Note on [Fe/H]:
For the solar reference iron abundance, the value A(Fe) = 7.45 from
Grevesse et al. (2007SSRv..130..105G 2007SSRv..130..105G) is adopted.
Note on A(Na), A(Al), and A(Na)NLTE:
The logarithmic abundance by number on a scale where the number of hydrogen
atoms is 10+12.
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Acknowledgements:
Rodolfo Smiljanic, rsmiljanic(at)ncac.torun.pl
(End) Rodolfo Smiljanic [CAMK, Poland], Patricia Vannier [CDS] 26-Feb-2016