Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-17T18:21:31.577Z Has data issue: false hasContentIssue false
  • English
  • Français

FUV Emission in Cool-Core Clusters

Published online by Cambridge University Press:  03 June 2010

J. B. R. Oonk ,
W. Jaffe ,
M. N. Bremer  and
N. Hatch
J. B. R. Oonk
Affiliation:
Leiden Observatory, Leiden University, Leiden, The Netherlands
W. Jaffe
Affiliation:
Leiden Observatory, Leiden University, Leiden, The Netherlands
M. N. Bremer
Affiliation:
H. H. Wills Physics Laboratory, University of Bristol, Bristol, UK
N. Hatch
Affiliation:
Leiden Observatory, Leiden University, Leiden, The Netherlands
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.

Far ultraviolet (FUV) emission is observed in the central regions of cool-core clusters with the Hubble Space Telescope (HST). It is traced out to 20 kpc from the nuclei of the brightest cluster galaxies and found to be distributed in clumps and filaments, as shown in Figure 1. The FUV emission matches the global structure of the ionized gas nebulae. If produced by stars, this emission can account for the ionization but not the temperature of the gas (Voit & Donahue 1997; Oonk et al. in preparation).

Keywords

galaxies: galaxies: cooling flowscDclusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 463
Copyright
Copyright © International Astronomical Union 2010

References

Voit, G. M. & Donahue, M. 1997, ApJ, 486, 242CrossRefGoogle Scholar
Oonk, J. B. R., Hatch, N., Jaffe, W., & Bremer, M. N., in preparationGoogle Scholar