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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 (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). 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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 133 1303 Atmospheric parameters and abundances
See also: J/A+A/572/A33 : Abundances from Gaia-ESO Survey (Mikolaitis+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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
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) 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.
Acknowledgements: Rodolfo Smiljanic, rsmiljanic(at)
(End) Rodolfo Smiljanic [CAMK, Poland], Patricia Vannier [CDS] 26-Feb-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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