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http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1814| THE LICK/SDSS LIBRARY. II. [Ca/Fe] AND [Mg/Fe] IN F, G, AND K STARS FROM SDSS-DR7 | |
| MIGUEL CHAVEZ DAGOSTINO | |
| Acceso Abierto | |
| Atribución-NoComercial-SinDerivadas | |
| Galaxy: stellar content Stars: abundances Stars: fundamental parameters Stars: late-type | |
| We analyzed the spectra of 17,600 F, G, and K stars extracted from the seventh Sloan Digital Sky Survey Data Release (SDSS-DR7) database in order to derive 〈[α/Fe]〉, [Ca/Fe], and [Mg/Fe] ratios. Particular attention has been devoted to estimating homogeneous and self-consistent atmospheric parameter values, Teƒƒ, log g, and [Fe/H], by comparing synthetic and observational Lick/SDSS indices. We present results for the sub-sample of more than 4000 spectra whose overall quality allowed us to derive fairly accurate stellar atmospheric parameter values and, therefore, reliable abundance ratios. A Monte Carlo approach was adopted to evaluate both the errors in the observational Lick/SDSS indices and in the derived parameter estimates. The analysis of the trends of [Ca/Fe] and [Mg/Fe] versus [Fe/H] pointed out that (1) the [Ca/Fe] and [Mg/Fe] ratios increase with decreasing [Fe/H] with different slopes reaching maximum average levels of +0.25 and +0.40 dex at [Fe/H]≃1.75, respectively; (2) our sample contains, at a given [Fe/H], stars characterized by significantly different amounts of α-enhancement, thus belonging to different Galactic populations; and (3) the analyzed sample shows a predominance of thick disk stars for [Fe/H] > −0.5 and the presence of stars belonging to the “high-α” halo population for −2.0 < [Fe/H] < −0.5. | |
| The Astrophysical Journal | |
| 01-04-2011 | |
| Artículo | |
| Inglés | |
| Estudiantes Investigadores Público en general | |
| Franchini, M., et al., (2011), THE LICK/SDSS LIBRARY. II. [Ca/Fe] AND [Mg/Fe] IN F, G, AND K STARS FROM SDSS-DR7, The Astrophysical Journal, Vol.730(117):1-13 | |
| ASTRONOMÍA Y ASTROFÍSICA | |
| Versión aceptada | |
| acceptedVersion - Versión aceptada | |
| Aparece en las colecciones: | Artículos de Astrofísica |
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