Bibcode
Fernández-Alvar, E.; Allende Prieto, C.; Schlesinger, K. J.; Beers, T. C.; Robin, A. C.; Schneider, D. P.; Lee, Y. S.; Bizyaev, D.; Ebelke, G.; Malanushenko, E.; Malanushenko, V.; Oravetz, D.; Pan, K.; Simmons, A.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 577, id.A81, 18 pp.
Fecha de publicación:
5
2015
Revista
Número de citas
38
Número de citas referidas
38
Descripción
Aims: We analyze a sample of 3944 low-resolution (R ~ 2000)
optical spectra from the Sloan Digital Sky Survey (SDSS), focusing on
stars with effective temperatures 5800 ≤ Teff ≤ 6300 K,
and distances from the Milky Way plane in excess of 5 kpc, and determine
their abundances of Fe, Ca, and Mg. Methods: We followed the same
methodology as in the previous paper in this series, deriving
atmospheric parameters by χ2 minimization, but this time
we obtained the abundances of individual elements by fitting their
associated spectral lines. Distances were calculated from absolute
magnitudes obtained by a statistical comparison of our stellar
parameters with stellar-evolution models. Results: The
observations reveal a decrease in the abundances of iron, calcium, and
magnesium at large distances from the Galactic center. The median
abundances for the halo stars analyzed are fairly constant up to a
Galactocentric distance r ~ 20 kpc, rapidly decrease between r ~ 20 and
r ~ 40 kpc, and flatten out to significantly lower values at larger
distances, consistent with previous studies. In addition, we examine
[Ca/Fe] and [Mg/Fe] as a function of [Fe/H] and Galactocentric distance.
Our results show that the most distant parts of the halo show a steeper
variation of [Ca/Fe] and [Mg/Fe] with iron. We found that at the range
-1.6 < [Fe/H] < -0.4, [Ca/Fe] decreases with distance, in
agreement with earlier results based on local stars. However, the
opposite trend is apparent for [Mg/Fe]. Our conclusion that the outer
regions of the halo are more metal-poor than the inner regions, based on
in situ observations of distant stars, agrees with recent results based
on inferences from the kinematics of more local stars, and with
predictions of recent galaxy formation simulations for galaxies similar
to the Milky Way.
Table 1 and beginning of Tables 2 and 3 are available in electronic form
at http://www.aanda.orgFull
Tables 2 and 3 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/577/A81
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Allende Prieto