Hostname: page-component-54dcc4c588-9xpg2 Total loading time: 0 Render date: 2025-10-10T06:51:34.493Z Has data issue: false hasContentIssue false
  • English
  • Français

Chemical composition of stellar populations in ω Centauri

Published online by Cambridge University Press:  23 April 2010

A. F. Marino ,
G. Piotto ,
R. Gratton ,
A. P. Milone ,
M. Zoccali ,
L. R. Bedin ,
S. Villanova  and
A. Bellini
A. F. Marino
Affiliation:
Dept. of Astronomy, University of Padova, Vicolo dell'osservatorio 3, 35122, Padova, Italy email: anna.marino@unipd.it P. Univ. Católica de Chile, Dept. de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile
G. Piotto
Affiliation:
Dept. of Astronomy, University of Padova, Vicolo dell'osservatorio 3, 35122, Padova, Italy email: anna.marino@unipd.it
R. Gratton
Affiliation:
INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
A. P. Milone
Affiliation:
Dept. of Astronomy, University of Padova, Vicolo dell'osservatorio 3, 35122, Padova, Italy email: anna.marino@unipd.it
M. Zoccali
Affiliation:
P. Univ. Católica de Chile, Dept. de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile
L. R. Bedin
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
S. Villanova
Affiliation:
Dept. de Astronomia, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile
A. Bellini
Affiliation:
Dept. of Astronomy, University of Padova, Vicolo dell'osservatorio 3, 35122, Padova, Italy email: anna.marino@unipd.it Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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 derive abundances of Fe, Na, O, α and s-elements from GIRAFFE@VLT spectra for more than 200 red giant stars in the Milky Way satellite ω Centauri. Our preliminary results are that: (i) we confirm that ω Centauri exhibits large star-to-star metallicity variation (~1.4 dex); (ii) the metallicity distribution reveals the presence of at least five stellar populations with different [Fe/H]; (iii) a distinct Na-O anticorrelation is clearly observed for the metal-poor and metal-intermediate stellar populations while apparently the anticorrelation disappears for the most metal rich populations. Interestingly the Na level grows with iron.

Keywords

galaxy: stellar contentGlobular clusters: individual (Omega Centauri)

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 183 - 184
Copyright
Copyright © International Astronomical Union 2010

References

Bedin, L. R., et al. , 2004, ApJ, 605, L125CrossRefGoogle Scholar
Bellazzini, M., et al. , 2008, AJ, 136, 1147CrossRefGoogle Scholar
Bellini, A., et al. , 2009, A&A, 493, 959Google Scholar
Cannon, R. D. & Stobie, R. S., 1973, MNRAS, 162, 207CrossRefGoogle Scholar
Carretta, E., et al. , 2010, ApJL in pressGoogle Scholar
Marino, A. F., et al. , 2008, A&A, 490, 625Google Scholar
Marino, A. F., et al. , 2009, A&A, 505, 1099Google Scholar
Lee, Y.-W., et al. 1999, Nature, 402, 55CrossRefGoogle Scholar
Pancino, E., et al. , 2000, ApJ, 534, L83CrossRefGoogle Scholar
Piotto, G., et al. , 2005, ApJ, 621, 777CrossRefGoogle Scholar
Sarajedini, A. & Layden, A. C., 1995, AJ, 109, 1086CrossRefGoogle Scholar
Sneden, C. A., 1973, Ph.D. ThesisGoogle Scholar
Villanova, S. et al. , 2007, ApJ, 663, 296CrossRefGoogle Scholar