Hostname: page-component-78c5997874-m6dg7 Total loading time: 0 Render date: 2024-11-05T05:01:55.832Z Has data issue: false hasContentIssue false
  • English
  • Français

The UV upturn phenomenon in the hierarchical universe

Published online by Cambridge University Press:  17 August 2012

Jaehyun Lee  and
Sukyoung K. Yi
Jaehyun Lee
Affiliation:
Department of Astronomy & Yonsei University Observatory, Yonsei University, Seoul 120-749, Republic of Korea email: [email protected]
Sukyoung K. Yi
Affiliation:
Department of Astronomy & Yonsei University Observatory, Yonsei University, Seoul 120-749, Republic of Korea email: [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.

Recent studies show that an old stellar population with high metallicity in the monolithic paradigm can explain the UV upturn. Numerical simulations and empirical studies however point out that massive early-type galaxies have evolved hierarchically with an extended star formation history. This obviously has an impact on our traditional understanding on the UV upturn and requires a new investigation on its origin. We report on our investigation on the evolutionary history of model galaxy SEDs in the hierarchical scenario. The use of conventional population models (calibrated to the monolithic picture) in combination with merger trees and extended star formation fails to reproduce the observed UV upturn. If a hierarchical picture is thought to be more realistic than a monolithic one, new calibration on the population models is required.

Keywords

galaxies: evolutionultraviolet: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 56 - 58
Copyright
Copyright © International Astronomical Union 2012

References

Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Buzzoni, A. 2007, ASPC, 374, 311Google Scholar
Greggio, L. & Renzini, A. 1990, ApJ, 364, 35CrossRefGoogle Scholar
Negroponte, J. & White, S. D. M. 1983, MNRAS, 205, 1009CrossRefGoogle Scholar
Toomre, A. & Toomre, J. 1972, BAAS, 4, 214Google Scholar
van Dokkum, P. G. 2005, AJ, 130, 2647CrossRefGoogle Scholar
White, S. D. M. & Frenk, C. S. 1991, ApJ, 379, 52CrossRefGoogle Scholar
Yi, S. K., Demarque, P., & Oemler, A. Jr. 1998, ApJ, 492, 480CrossRefGoogle Scholar
Yi, S. K. 2003, ApJ, 572, 202CrossRefGoogle Scholar
Yi, S. K. et al. 2005, AJ, 619, 111CrossRefGoogle Scholar
Yi, S. K., Lee, J., Sheen, Y.-K., Jeong, H., Suh, H., & Oh, K. 2011, ApJS, 195, 22CrossRefGoogle Scholar