Hostname: page-component-8448b6f56d-sxzjt Total loading time: 0 Render date: 2024-04-19T16:35:10.262Z Has data issue: false hasContentIssue false
  • English
  • Français

MILES SSP Models

Published online by Cambridge University Press:  13 April 2010

A. Vazdekis ,
P. Sánchez-Blázquez ,
J. Falcón-Barroso ,
A. J. Cenarro ,
M. A. Beasley ,
N. Cardiel ,
J. Gorgas  and
R. Peletier
A. Vazdekis*
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain
P. Sánchez-Blázquez
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain
J. Falcón-Barroso
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain
A. J. Cenarro
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain Centro de Estudios de Física del Cosmos de Aragón, C/ General Pizarro 1, E-44001, Teruel, Spain
M. A. Beasley
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain
N. Cardiel
Affiliation:
Dept. de Astrofísica, Fac. de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
J. Gorgas
Affiliation:
Dept. de Astrofísica, Fac. de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
R. Peletier
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV, Groningen, Netherlands
*
†E-mail: vazdekis@iac.es
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 present SEDs for single-age, single-metallicity stellar populations (SSPs) covering the full optical spectral range at resolution (FWHM = 2.3Å). These SEDs can be regarded as our base models, as we combine scaled-solar isochrones with an empirical stellar spectral library (MILES), which follows the chemical evolution pattern of the solar neighbourhood. The models rely as much as possible on empirical ingredients as also employ extensive photometric libraries. Thanks to the unprecedented parameter coverage of the MILES library we synthesize SSP SEDs from intermediate- to very-old age regimes, and the metallicity from super-solar to [M/H] = −2.3, all for a suite of IMF shapes and slopes. We propose a new Line Index System (LIS), based on flux-calibrated spectra, to avoid the intrinsic uncertainties associated with the Lick/IDS system and provide more appropriate, uniform, spectral resolution.

Keywords

galaxies: abundancesgalaxies: star clusters galaxies: dwarf galaxies: elliptical and lenticularcD galaxies: evolution galaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 65 - 68
Copyright
Copyright © International Astronomical Union 2010

References

Alonso, A., Arribas, S., & Martínez-Roger, C. 1995, A&A, 297, 197Google Scholar
Alonso, A., Arribas, S., & Martínez-Roger, C. 1996, A&A, 313, 873Google Scholar
Alonso, A., Arribas, S., & Martínez-Roger, C. 1999, A&AS, 140, 261Google Scholar
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Carretero, C., Vazdekis, A., Beckman, J., Sánchez-Blázquez, P., & Gorgas, J. 2004, ApJ, 609, L45CrossRefGoogle Scholar
Cenarro, A. J. et al. 2007, MNRAS, 374, 664CrossRefGoogle Scholar
Cervantes, J. L. & Vazdekis, A. 2009, MNRAS, 392, 691CrossRefGoogle Scholar
de la Rosa, I. G., de Carvalho, R. R., Vazdekis, A., & Barbuy, B. 2007, AJ, 133, 330CrossRefGoogle Scholar
Edvardsson, B., Andersen, J., Gustafsson, B., Lambert, D. L., Nissen, P. E., & Tomkin, J. 1993, A&AS, 102, 603Google Scholar
Girardi, L., Bressan, A., Bertelli, G., & Chiosi, C. 2000, A&AS, 141, 371Google Scholar
Girardi, L., Bressan, A., Chiosi, C., Bertelli, G., & Nasi, E. 1996, A&AS, 117, 113Google Scholar
Kroupa, P. 2001, MNRAS, 322, 231CrossRefGoogle Scholar
Kuntschner, H., Smith, R. J., Colless, M., Davies, R. L.; Kaldare, R., & Vazdekis, A. 2006, MNRAS, 369, 497CrossRefGoogle Scholar
Michielsen, D. et al. 2008, MNRAS, 385, 1374CrossRefGoogle Scholar
Sánchez-Blázquez, P. et al. 2006, MNRAS, 371, 703CrossRefGoogle Scholar
Schiavon, R. P. 2007, ApJS, 171, 146CrossRefGoogle Scholar
Schiavon, R. P., Rose, J. A., Courteau, S., & MacArthur, L. 2005, ApJS, 160, 163CrossRefGoogle Scholar
Schiavon, R. P., Caldwell, N., & Rose, J. A. 2004, AJ, 127, 1513CrossRefGoogle Scholar
Vazdekis, A., Sánchez-Blázquez, P., Falcón-Barroso, J., Cenarro, A. J., Beasley, M., Cardiel, N., Gorgas, J., & Peletier, R. F. 2010, MNRAS, in press.Google Scholar
Vazdekis, A., Cenarro, A. J., Gorgas, J., Cardiel, N., & Peletier, R. F. 2003, MNRAS, 340, 1317CrossRefGoogle Scholar
Vazdekis, A., Kuntschner, H., Davies, R. L., Arimoto, N., Nakamura, O., & Peletier, R. 2001b, ApJ, 551, L127CrossRefGoogle Scholar
Vazdekis, A. 1999, ApJ, 513, 224CrossRefGoogle Scholar
Vazdekis, A. & Arimoto, N. 1999, ApJ, 525, 144CrossRefGoogle Scholar
Vazdekis, A., Casuso, E., Peletier, R. F., & Beckman, J. E. 1996, ApJS, 106, 307CrossRefGoogle Scholar
Worthey, G., Faber, S. M., Gonzalez, J. J., & Burstein, D. 1994, ApJS, 94, 687CrossRefGoogle Scholar
Yamada, Y., Arimoto, N., Vazdekis, A., & Peletier, R. 2006, ApJ, 637, 200CrossRefGoogle Scholar