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J/A+A/572/A33       Abundances from Gaia-ESO Survey          (Mikolaitis+, 2014)

The Gaia-ESO Survey: the chemical structure of the Galactic discs from the first internal data release. Mikolaitis S., Hill V., Recio-Blanco A., de Laverny P., Allende Prieto C., Kordopatis G., Tautvaisiene G., Romano D., Gilmore G., Randich S., Feltzing S., Micela G., Vallenari A., Alfaro E.J., Bensby T., Bragaglia A., Flaccomio E., Lanzafame A.C., Pancino E., Smiljanic R., Bergemann M., Carraro G., Costado M.T., Damiani F., Hourihane A., Jofre P., Lardo C., Magrini L., Maiorca E., Morbidelli L., Sbordone L., Sousa S.G., Worley C.C., Zaggia S. <Astron. Astrophys. 572, A33 (2014)> =2014A&A...572A..33M
ADC_Keywords: Stars, normal ; Spectroscopy ; Abundances Keywords: Galaxy: disc - Galaxy: stellar content - techniques: spectroscopic Abstract: Most high-resolution spectroscopic studies of the Galactic discs were mostly confined to objects in the solar vicinity. Here we aim at enlarging the volume in which individual chemical abundances are used to characterise both discs, using the first internal data release of the Gaia-ESO survey. We derive and discuss the abundances of eight elements (Mg, Al, Si, Ca, Ti, Fe, Cr, Ni, and Y). The trends of these elemental abundances with iron are very similar to those in the solar neighbourhood. We find a natural division between α-rich and α-poor stars, best seen in the bimodality of the [Mg/M] distributions in bins of metallicity, which we attribute to thick- and thin-disc sequences, respectively. With the possible exception of Al, the observed dispersion around the trends is well described by the expected errors, leaving little room for astrophysical dispersion. Using previously derived distances from Recio-Blanco et al. (2014A&A...567A...5R), we further find that the thick-disc is more extended vertically and is more centrally concentrated towards the inner Galaxy than the thin-disc, which indicates a shorter scale-length. We derive the radial and vertical gradients in metallicity, iron, four α-element abundances, and Al for the two populations, taking into account the identified correlation between RGC and |Z|. Radial metallicity gradient is found in the thin disc. The positive radial individual [α/M] gradients found are at variance from the gradients observed in the RAVE survey. The thin disc also hosts a negative vertical metallicity gradient, accompanied by positive individual [α/M] and [Al/M] gradients. The thick-disc, presents no radial metallicity gradient, a shallower vertical metallicity gradient than the thin-disc, an α-elements-to-iron radial gradient in the opposite sense than that of the thin disc, and positive vertical individual [α/M] and [Al/M] gradients. Description: Table2 contains chemical abundances of 1916 stars from GES DR1. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 156 1916 Abundances of 1916 stars
See also: I/324 : The Initial Gaia Source List (IGSL) (Smart, 2013) J/MNRAS/426/1767 : Gaia spectrophotometric standard stars I. (Pancino+, 2012) J/A+A/552/A64 : Gaia-RVS standards (Soubiran+, 2013) J/A+A/566/A98 : The Gaia Benchmark Stars - Library (Blanco-Cuaresma+, 2014) J/A+A/565/A11 : Gaia photometry for white dwarfs (Carrasco+, 2014) J/A+A/564/A133 : Gaia FGK benchmark stars: metallicity (Jofre+, 2014) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- ID [1/1916] Identification number 6- 21 A16 --- CName Target Name in the Gaia-ESO archive, HHMMSSss+DDMMSSs 23- 37 A15 --- Name Object Name in the Gaia-ESO archive 38- 42 F5.2 [-] A(Mg1) [6.0/8.0]? MgI abundance, 12+log(N/H) 44- 48 F5.2 [-] e_A(Mg1) ? rms uncertainty of Mg1 abundance 50- 54 F5.2 [-] A(Al1) [5.2/7.0]? AlI abundance, 12+log(N/H) 56- 60 F5.2 [-] e_A(Al1) ? rms uncertainty of Al1 abundance 62- 66 F5.2 [-] A(Si1) [5.9/8.2]? SiI abundance, 12+log(N/H) 68- 72 F5.2 [-] e_A(Si1) ? rms uncertainty of Si1 abundance 74- 78 F5.2 [-] A(Ca1) [3.7/6.9]? CaI abundance, 12+log(N/H) 80- 84 F5.2 [-] e_A(Ca1) ? rms uncertainty of Ca1 abundance 86- 90 F5.2 [-] A(Ca2) [3.7/6.8]? CaII abundance, 12+log(N/H) 92- 96 F5.2 [-] e_A(Ca2) ? rms uncertainty of Ca2 abundance 98-102 F5.2 [-] A(Ti1) [3.2/5.4]? TiI abundance, 12+log(N/H) 104-108 F5.2 [-] e_A(Ti1) ? rms uncertainty of Ti1 abundance 110-114 F5.2 [-] A(Ti2) [3.4/5.6]? TiII abundance, 12+log(N/H) 116-120 F5.2 [-] e_A(Ti2) ? rms uncertainty of Ti2 abundance 122-126 F5.2 [-] A(Cr1) [2.8/6.1]? CrI abundance, 12+log(N/H) 128-132 F5.2 [-] e_A(Cr1) ? rms uncertainty of Cr1 abundance 134-138 F5.2 [-] A(Ni1) [4.5/6.9]? NiI abundance, 12+log(N/H) 140-144 F5.2 [-] e_A(Ni1) ? rms uncertainty of Ni1 abundance 146-150 F5.2 [-] A(Y2) [-0.2/3]? YII abundance, 12+log(N/H) 152-156 F5.2 [-] e_A(Y2) ? rms uncertainty of Y2 abundance
Acknowledgements: Sarunas Mikolaitis, Sarunas.Mikolaitis(at)
(End) Sarunas Mikolaitis [OCA, Nice, France], Patricia Vannier [CDS] 10-Sep-2014
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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