Hostname: page-component-8448b6f56d-xtgtn Total loading time: 0 Render date: 2024-04-19T05:47:11.210Z Has data issue: false hasContentIssue false
  • English
  • Français

Chemical Composition of the Galactic Bulge in Baade's Window

Published online by Cambridge University Press:  09 March 2010

Andrew McWilliam ,
Jon Fulbright  and
R. Michael Rich
Andrew McWilliam
Affiliation:
Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA, USA email: andy@obs.carnegiescience.edu
Jon Fulbright
Affiliation:
Johns Hopkins University, Physics & Astronomy, N. 3400 Charles St., Baltimore, MD, USA
R. Michael Rich
Affiliation:
University of California, Los Angeles, Physics & Astronomy, 430 Portola Plaza, Box 951547, Los Angeles, CA, 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.

1. McWilliam and Zoccali (2009) show the existence of two Red Clump populations towards the Galactic bulge, based on 2MASS data. 2.Measured [Mg/Fe], [Al/Fe], and [La/Eu] ratios in the bulge are consistent with a rapid formation timescale (<1Gyr), which also requires a slightly top-heavy IMF to reproduce the mean bulge metallicity. The [C/O] and [O/Fe] ratios are consistent if their predicted metal-dependent yields from massive stars with winds are considered. The decline in explosive [α/Fe] (Si, Ca, and Ti) can only be understood if their yields also decline with metallicity above [Fe/H]~−1.

Keywords

stars: abundancesGalaxy: abundancesGalaxy: bulgenucleosynthesis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 279 - 284
Copyright
Copyright © International Astronomical Union 2010

References

Arnett, W. D. 1971, ApJ, 166, 153CrossRefGoogle Scholar
Ballero, S. K., Matteucci, F., Origlia, L., & Rich, R. M. 2007, A&A, 467, 123Google Scholar
Burris, D. L., Pilachowski, C. A., Armandroff, T. E., et al. 2000, ApJ, 544, 302CrossRefGoogle Scholar
Cescutti, G., Matteucci, F., McWilliam, A., & Chiappini, C. 2009, A&A, 505, 605Google Scholar
Conti, P. S., Greenstein, J. L., Spinrad, H., Wallerstein, G., & Vardya, M. S. 1967, ApJ, 148, 105CrossRefGoogle Scholar
Fulbright, J. F., McWilliam, A., & Rich, A. 2007, ApJ, 661, 1152CrossRefGoogle Scholar
Lecureur, A., Hill, V., & Zoccali, M., et al. 2007, A&A, 465, 799Google Scholar
Maeder, A. 1992, A&A, 264, 105Google Scholar
Matteucci, F. & Brocato, E. 1990, ApJ, 365, 539CrossRefGoogle Scholar
McWilliam, A. & Rich, R. M. 1994, ApJS, 91, 749CrossRefGoogle Scholar
McWilliam, A. & Rich, R. M. 2004, Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series. Edited by A. McWilliam and M. Rauch, 2004. Pasadena (arXiv:astro-ph/0312628)Google Scholar
McWilliam, A., Matteucci, F., Ballero, A., et al. 2008, AJ, 136, 367CrossRefGoogle Scholar
Meynet, G. & Maeder, A. 2002, A&A, 390, 561Google Scholar
Meléndez, J., Asplund, M. & Alves-Brito, A., et al. 2008, A&A, 484, L21Google Scholar
Nomoto, K., Thielemann, F-K., & Yokoi, K. 1994, ApJ, 286, 644CrossRefGoogle Scholar
Patsis, P. A., Skokos, Ch., & Athanassoula, E. 2002, MNRAS, 337, 578CrossRefGoogle Scholar
Smecker-Hane, T. & Wyse, R. F. G. 1992, AJ, 103, 1621CrossRefGoogle Scholar
Tinsley, B. M. 1979, ApJ, 229, 1046CrossRefGoogle Scholar
Wallerstein, G. 1962, ApJS, 6, 407CrossRefGoogle Scholar
Woosley, S. E. & Weaver, T. A. 1995, ApJS, 101, 181CrossRefGoogle Scholar
Wyse, R. F. G. & Gilmore, G. 1993, ASP Conference Series, 48, 727Google Scholar
Zoccali, M., Hill, V., Lecureur, A., Barbuy, B., Renzini, A., et al. 2008, A&A, 486, 177Google Scholar