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Disentangling Nitrogen and Carbon Abundances in Early-Type Galaxies

Published online by Cambridge University Press:  13 April 2010

Elisa Toloba ,
Patricia Sánchez-Blázquez ,
Javier Gorgas  and
Brad K. Gibson
Elisa Toloba
Affiliation:
Universidad Complutense de Madrid, 28040, Madrid, Spain email: etj@astrax.fis.ucm.es
Patricia Sánchez-Blázquez
Affiliation:
Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK Instituto de Astrofísica de Canarias, Via Lactea S/N, 38205, La Laguna, Spain
Javier Gorgas
Affiliation:
Universidad Complutense de Madrid, 28040, Madrid, Spain email: etj@astrax.fis.ucm.es
Brad K. Gibson
Affiliation:
Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK
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Abstract

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The near-UV NH3360 feature has been measured in a sample of 35 early-type galaxies in a wide range of masses and environments. We found that, contrary to what is seen with Mg- and C-sensitive Lick-style indices, NH3360 does not vary significantly with galaxy velocity dispersion. When compared with solar-scaled stellar population models N/Fe appears mildly enhanced. We do not detect any difference in the NH3360 index between galaxies in different environments. We outline the important implications of these conclusions for our understanding of the origin of carbon and nitrogen, and the star formation histories of early-type galaxies.

Keywords

galaxies: abundancesgalaxies: elliptical and lenticularcDgalaxies: evolution
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 438 - 439
Copyright
Copyright © International Astronomical Union 2010

References

Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Burstein, D. 2003, ASPC, 297, 253Google Scholar
Davidge, T. J. & Clark, C. C. 1994, AJ, 107, 946CrossRefGoogle Scholar
Henry, R. B. C., Edmunds, M. G., & Köppen, J. 2000, ApJ, 541, 660CrossRefGoogle Scholar
Ponder, J. M., Burstein, D., O'Connell, R. W., Rose, J. A. et al. 1998, AJ, 116, 2297CrossRefGoogle Scholar
Sánchez-Blázquez, P., Gorgas, J., Cardiel, N., Cenarro, J., & González, J. 2003, ApJ, 590, L91CrossRefGoogle Scholar
Sánchez-Blázquez, P., Gorgas, J., Cardiel, N., & González, J. J. 2006 a, A&A, 457, 787Google Scholar
Sánchez-Blázquez, P., Gorgas, J., Cardiel, N., & González, J. J. 2006b, A&A, 457, 809Google Scholar
Schiavon, R. P. 2007, ApJS, 171, 146CrossRefGoogle Scholar
Serven, J., Worthey, G., & Briley, M. M. 2005, ApJ, 627, 754CrossRefGoogle Scholar
Tomkin, J. & Lambert, D. L. 1984, ApJ, 279, 220CrossRefGoogle Scholar
Worthey, G. 1998, PASP, 110, 888CrossRefGoogle Scholar