Bibcode
Smiljanic, R.; Korn, A. J.; Bergemann, M.; Frasca, A.; Magrini, L.; Masseron, T.; Pancino, E.; Ruchti, G.; San Roman, I.; Sbordone, L.; Sousa, S. G.; Tabernero, H.; Tautvaišienė, G.; Valentini, M.; Weber, M.; Worley, C. C.; Adibekyan, V. Zh.; Allende Prieto, C.; Barisevičius, G.; Biazzo, K.; Blanco-Cuaresma, S.; Bonifacio, P.; Bragaglia, A.; Caffau, E.; Cantat-Gaudin, T.; Chorniy, Y.; de Laverny, P.; Delgado-Mena, E.; Donati, P.; Duffau, S.; Franciosini, E.; Friel, E.; Geisler, D.; González Hernández, J. I.; Gruyters, P.; Guiglion, G.; Hansen, C. J.; Heiter, U.; Hill, V.; Jacobson, H. R.; Jofre, P.; Jönsson, H.; Lanzafame, A. C.; Lardo, C.; Ludwig, H.-G.; Maiorca, E.; Mikolaitis, Š.; Montes, D.; Morel, T.; Mucciarelli, A.; Muñoz, C.; Nordlander, T.; Pasquini, L.; Puzeras, E.; Recio-Blanco, A.; Ryde, N.; Sacco, G.; Santos, N. C.; Serenelli, A. M.; Sordo, R.; Soubiran, C.; Spina, L.; Steffen, M.; Vallenari, A.; Van Eck, S.; Villanova, S.; Gilmore, G.; Randich, S.; Asplund, M.; Binney, J.; Drew, J.; Feltzing, S.; Ferguson, A.; Jeffries, R.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Alfaro, E.; Babusiaux, C.; Bensby, T.; Blomme, R.; Flaccomio, E.; François, P.; Irwin, M.; Koposov, S.; Walton, N.; Bayo, A.; Carraro, G.; Costado, M. T.; Damiani, F.; Edvardsson, B.; Hourihane, A.; Jackson, R.; Lewis, J.; Lind, K.; Marconi, G.; Martayan, C.; Monaco, L.; Morbidelli, L. et al.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 570, id.A122, 38 pp.
Fecha de publicación:
10
2014
Revista
Número de citas
208
Número de citas referidas
185
Descripción
Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using
FLAMES at the VLT to obtain high-quality medium-resolution Giraffe
spectra for about 105 stars and high-resolution UVES spectra
for about 5000 stars. With UVES, the Survey has already observed 1447
FGK-type stars. Aims: These UVES spectra are analyzed in parallel
by several state-of-the-art methodologies. Our aim is to present how
these analyses were implemented, to discuss their results, and to
describe how a final recommended parameter scale is defined. We also
discuss the precision (method-to-method dispersion) and accuracy (biases
with respect to the reference values) of the final parameters. These
results are part of the Gaia-ESO second internal release and will be
part of its first public release of advanced data products.
Methods: The final parameter scale is tied to the scale defined by the
Gaia benchmark stars, a set of stars with fundamental atmospheric
parameters. In addition, a set of open and globular clusters is used to
evaluate the physical soundness of the results. Each of the implemented
methodologies is judged against the benchmark stars to define weights in
three different regions of the parameter space. The final recommended
results are the weighted medians of those from the individual methods.
Results: The recommended results successfully reproduce the
atmospheric parameters of the benchmark stars and the expected
Teff-log g relation of the calibrating clusters. Atmospheric
parameters and abundances have been determined for 1301 FGK-type stars
observed with UVES. The median of the method-to-method dispersion of the
atmospheric parameters is 55 K for Teff, 0.13 dex for log g
and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between
50-100 K for Teff, 0.10-0.25 dex for log g and 0.05-0.10 dex
for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg,
Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd,
and Eu. The typical method-to-method dispersion of the abundances varies
between 0.10 and 0.20 dex. Conclusions: The Gaia-ESO sample of
high-resolution spectra of FGK-type stars will be among the largest of
its kind analyzed in a homogeneous way. The extensive list of elemental
abundances derived in these stars will enable significant advances in
the areas of stellar evolution and Milky Way formation and evolution.
Based on observations made with the ESO/VLT, at Paranal Observatory,
under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs
Gilmore and Randich). Appendices are available in electronic form at http://www.aanda.org
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