Hostname: page-component-7c8c6479df-995ml Total loading time: 0 Render date: 2024-03-28T01:28:46.722Z Has data issue: false hasContentIssue false

Chemical Abundances in Metal-Rich Bulge-like Stars

Published online by Cambridge University Press:  01 December 2006

L. Pompéia
Affiliation:
Universidade de São Paulo, IAG, C.P. 3386, 01060-970 São Paulo, Brazil email: pompeia@astro.iag.usp.br, barbuy@astro.iag.usp.br
B. Barbuy
Affiliation:
Universidade de São Paulo, IAG, C.P. 3386, 01060-970 São Paulo, Brazil email: pompeia@astro.iag.usp.br, barbuy@astro.iag.usp.br
M. Grenon
Affiliation:
Observatoire de Genève, Chemin des Maillettes 51, CH-1290 Sauverny, Switzerland email: Michel.Grenon@obs.unige.ch
B. Gustafsson
Affiliation:
Department of Astronomy and Space Physics, University of Uppsala, Uppsala, Sweden email: bg@astro.uu.se
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have derived chemical abundances for Ca, Ti, Si, Mg, O, Na, Al, Ni, Co and Cr for a sample of stars with peculiar kinematics and probable origin near the bulge. Our sample stars are in the metallicity range = −0.8 ≤ [Fe/H] ≤ +0.6 dex, and have small pericentric distances, Rp ≤ 3.5 kpc, small scale height, with Zmax < 0.16 kpc, and old ages, 9 to 11 Gyr. We have found that the abundance distributions of O, Mg and Al lie between bulge and both thin and thick disks distributions, i. e., with an enhanced pattern relative to thin and thick disk stars, and an underabundant behavior compared to bulge stars. [Na/Fe] ratios ovelarp the bulge distribution in the metal-poor tail, and show similar values compared to thin and thick disk stars for the super-solar metallicity range. Ca, Ti and Si values are similar to those of the thick disk stars in the metal-poor range, while an underabundant behavior is seen relative to thin disk stars for metallicities [Fe/H] > +0.3 dex. Compared to bulge stars, such elements are deficient in our sample stas. For the iron-peak elements Cr and Ni we have found a slightly overabundant behavior relative to both thin and thick disks distributions in the metal-poor range, and a smooth decreasing trend for [Cr/Fe] for stars in the supersolar regime. [Co/Fe] ratios track the solar value in the metal-poor range, and show an underabundant behavior relative do thin disk stars for metallicities [Fe/H] > 0.0 dex.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

Allende Prieto, C., Barklem, P. S., Lambert, D. L., & Cunha, K. 2004 A&A 420, 183Google Scholar
Bensby, T., Feltzing, S., & Lundstrm, I. 2004, A&A 415, 155Google Scholar
Bensby, T.Feltzing, S., Lundstrm, I., & Ilyin, I. 2005, A&A 433, 185Google Scholar
Fulbright, J.P., & Rich, R.M., & McWilliam, A. 2006 astro-ph/0609087Google Scholar
Lecureur, A., Hill, V., Zoccali, M., Barbuy, B., Gomez, A., Minniti, D., Ortolani, S., & Renzini, A. 2006 astro-ph/0610346Google Scholar
Pompéia, L., Barbuy, B. & Grenon, M. 2002, ApJ 566, 84CrossRefGoogle Scholar
Pompéia, L., Barbuy, B. & Grenon, M. 2003, ApJ 592, 1173CrossRefGoogle Scholar
Reddy, B. E., Tomkin, J., Lambert, D. L., & Allende Prieto, C.MNRAS 340, 304CrossRefGoogle Scholar
Thorén, P., Feltzing, S. 2000 A&A 363, 692Google Scholar