Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-12-01T12:39:31.064Z Has data issue: false hasContentIssue false
  • English
  • Français

Comparison of different spectral population models

Published online by Cambridge University Press:  01 December 2006

Mina Koleva ,
Philippe Prugniel ,
Pierre Ocvirk ,
Damien Le Borgne ,
Igor Chilingarian  and
Caroline Soubiran
Mina Koleva*
Affiliation:
Université Lyon 1, Observatoire de Lyon, 9 av. Ch. André, St. Genis Laval, F-69230, France; CNRS, UMR 5574 Department of Astronomy, St. Kl. Ohridski University of Sofia, 5 J. Bourchier Blvd., BG-1164 Sofia, Bulgaria
Philippe Prugniel
Affiliation:
Université Lyon 1, Observatoire de Lyon, 9 av. Ch. André, St. Genis Laval, F-69230, France; CNRS, UMR 5574 Observatoire de Paris, GEPI, 61 Ave. de l'Observatoire, Paris, 75014, France
Pierre Ocvirk
Affiliation:
CEA Saclay/Service d'Astrophysique Orme des Merisiers, Bat 709, Gif-sur-Yvette Cedex, F-91191, France
Damien Le Borgne
Affiliation:
CEA Saclay/Service d'Astrophysique Orme des Merisiers, Bat 709, Gif-sur-Yvette Cedex, F-91191, France
Igor Chilingarian
Affiliation:
Université Lyon 1, Observatoire de Lyon, 9 av. Ch. André, St. Genis Laval, F-69230, France; CNRS, UMR 5574 Sternberg Astronomical Institute, Moscow University, 13 Universitetskij pr., 119992, Moscow, Russia
Caroline Soubiran
Affiliation:
Observatoire de Bordeaux, 2 rue de l'Observatoire, 33270, Floirac, France
*
†[email protected]
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 compared simple stellar populations (SSPs) generated with different population synthesis tools: BC03, Vazdekis and Pégase.HR and different stellar libraries: ELODIE3.1, SteLib and MILES. We find that BC03/SteLib SSPs are biased toward solar metallicity, however Pégase.HR/ELODIE3.1 and Vazdekis/MILES are extremely consistent. The extensive coverage of the space of atmospheric parameters in the large stellar libraries allows precise synthesis for a large range of ages (0.1 .. 10 Gyr) and metallicities (−2 .. +0.4 dex) limited by the quality of the determination of stellar parameters (temperature scale of the giants).

Keywords

galaxies: stellar contentgalaxies: evolutiontechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 183 - 184
Copyright
Copyright © International Astronomical Union 2007

References

Bruzual, & Charlot, , 2003 Bruzual, G. & Charlot, S., 2003, MNRAS 344, 1000CrossRefGoogle Scholar
Koleva, M. et al. , 2006, astro-ph/0602362Google Scholar
Leborgne, J.-F. et al. , 2003, A&A 402, 433Google Scholar
LeBorgne, D. Borgne, D. et al. , 2004, A&A 425, 881Google Scholar
Lejeune, Th., Cuisinier, F., & Buser, R., 1997, A&AS 125, 229Google Scholar
Ocvirk, P. et al. , 2006, MNRAS 365, 74CrossRefGoogle Scholar
Prugniel, Ph. & Soubiran, C., 2001, A&A, 369, 1048Google Scholar
Prugniel, Ph. & Soubiran, C., 2004, astro.ph-/0409214Google Scholar
Sánchez-Blázquez, P. et al. , 2006, MNRAS 371, 701CrossRefGoogle Scholar
Vazdekis, A., 1999, ApJ 513, 224CrossRefGoogle Scholar