Hostname: page-component-686fd747b7-n7dl9 Total loading time: 0 Render date: 2025-02-13T14:14:03.623Z Has data issue: false hasContentIssue false
  • English
  • Français

Fixing the Stellar M/L Ratio by Chemospectrophotometric Evolution Models

Published online by Cambridge University Press:  05 December 2011

Marie-Maude de Denus-Baillargeon ,
Samuel Boissier ,
Claude Carignan ,
Olivier Hernandez  and
Philippe Amram
Marie-Maude de Denus-Baillargeon
Affiliation:
Département de physique, Université de Montréal C.P. 6128, succ. Centre-Ville, Montréal, H3C 3J7, Canada email: mmaude@astro.umontreal.ca
Samuel Boissier
Affiliation:
Laboratoire d'astrophysique de Marseille, Université Aix-Marseille III 38 rue Frederic Joliot-Curie, 13388 Marseille cedex 13, France
Claude Carignan
Affiliation:
Département de physique, Université de Montréal C.P. 6128, succ. Centre-Ville, Montréal, H3C 3J7, Canada email: mmaude@astro.umontreal.ca Observatoire d'Astrophysique de l'Université de Ouagadougou (ODAUO), UFR/SEA, BP 7021, Ouagadougou 03, Burkina Faso Department of Astronomy, University of Cape Town, Privite Bag X3, Rondebosch 7701, South Africa
Olivier Hernandez
Affiliation:
Département de physique, Université de Montréal C.P. 6128, succ. Centre-Ville, Montréal, H3C 3J7, Canada email: mmaude@astro.umontreal.ca
Philippe Amram
Affiliation:
Laboratoire d'astrophysique de Marseille, Université Aix-Marseille III 38 rue Frederic Joliot-Curie, 13388 Marseille cedex 13, France
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.

The exact contribution of the stellar disk to the overall kinematics of a galaxy remains in most studies a free parameter of the mass models. With the help of chemospectrophotometric evolution models, it is now possible to have a coherent picture of the stellar population of a galaxy including its mass-to-luminosity ratio at every radius spanning a wide range of observable wavelengths. We will focus on discussing the consistency of the mass thus inferred in photometric bands ranging from the FUV to the NIR for individual galaxies and compare this to the maximum-disc hypothesis.

Keywords

galaxies: kinematics and dynamicsgalaxies: mass-to-light ratio
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 186 - 190
Copyright
Copyright © International Astronomical Union 2011

References

Bell, J. & deAAAAJong, E., 2001, ApJ, 550, 212CrossRefGoogle Scholar
Bershady, M. A., et al. 2010, ApJ 716, 198CrossRefGoogle Scholar
Boissier, S. & Prantzos, N., 1999, MNRAS, 307, 857CrossRefGoogle Scholar
Boissier, S. & Prantzos, N., 2000, MNRAS, 312, 398CrossRefGoogle Scholar
Daigle, O., et al. 2006, MNRAS, 367, 469CrossRefGoogle Scholar
Dicaire, I., et al. 2008, MNRAS, 385, 553CrossRefGoogle Scholar
GilAAAAdeAAAAPaz, A., et al. 2007 ApJS, 173, 185CrossRefGoogle Scholar
Hernandez, O., et al. 2005, MNRAS, 360, 1201CrossRefGoogle Scholar
Kennicutt, R. C., et al. 2003, PASP, 115, 928CrossRefGoogle Scholar
Mo, H.J., Mao, S., & White, S., 1998, MNRAS, 295, 319CrossRefGoogle Scholar
Muñoz-Matteos, J. C., et al. 2011, In preparationGoogle Scholar
Stark, D. V., McGaugh, S. S., & Swaters, R. A. 2009, AJ, 138, 392CrossRefGoogle Scholar
Walter, F., et al. 2008, AJ, 136, 2653CrossRefGoogle Scholar