Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-23T08:40:00.278Z Has data issue: false hasContentIssue false
  • English
  • Français

The growth of the red-sequence in clusters since ≃1

Published online by Cambridge University Press:  21 October 2010

Roberto P. Muñoz ,
L. F. Barrientos ,
B. P. Koester ,
D. G. Gilbank ,
M. D. Gladders  and
H. K. C. Yee
Roberto P. Muñoz
Affiliation:
Departamento de Astronomia y Astrofisica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Casilla 306, Santiago 22, Chile; email: [email protected] Departamento de Fisica y Astronomia, Universidad de Valparaiso
L. F. Barrientos
Affiliation:
Departamento de Astronomia y Astrofisica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Casilla 306, Santiago 22, Chile; email: [email protected]
B. P. Koester
Affiliation:
Department of Astronomy and Astrophysics, University of Chicago
D. G. Gilbank
Affiliation:
Department of Physics and Astronomy, University of Waterloo
M. D. Gladders
Affiliation:
Department of Astronomy and Astrophysics, University of Chicago
H. K. C. Yee
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto
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 use deep nIR imaging of 15 galaxy clusters at z ≃ 1 to study the build-up of the red-sequence in rich clusters since the Universe was half its present age. We measured, for the first time, the luminous-to-faint ratio of red-sequence galaxies at z=1 from a large ensemble of clusters, and found an increase of 100% in the ratio of luminous-to-faint red-sequence galaxies from z=0.45 to 1.0. The measured change in this ratio as function of redshift is well-reproduced by a simple evolutionary model developed in this work, that consists in an early truncation of the star formation for bright cluster galaxies and a delayed truncation for faint cluster galaxies.

Keywords

galaxies: clusters: generalgalaxies: evolutiongalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 88
Copyright
Copyright © International Astronomical Union 2010

References

Gladders, M. D. & Yee, H. K. C. 2005, ApJS 157, 1CrossRefGoogle Scholar
De Lucia, G., Poggianti, B. M., Aragón-Salamanca, A., White, S. D. M., Zaritsky, D., Clowe, D., Halliday, C., Jablonka, P., von der Linden, A., Milvang-Jensen, B., Pelló, R., Rudnick, G., Saglia, R. P., & Simard, L. 2007, MNRAS 374, 809CrossRefGoogle Scholar
Muñoz, R. P., Padilla, N. D., & Barrientos, L. F. 2009, MNRAS 392, 655CrossRefGoogle Scholar