Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-25T17:30:27.884Z Has data issue: false hasContentIssue false
  • English
  • Français

X-raying the Hubble Frontier Fields cluster Abell 2744

Published online by Cambridge University Press:  27 October 2016

Dominique Eckert
Dominique Eckert*
Affiliation:
Department of Astronomy, University of Geneva, Ch. dEcogia 16, 1290 Versoix, Switzerland 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.

Abell 2744 was the first HFF cluster completed. It displays a fascinating complexity in its distribution of dark and luminous matter, which led to its nickname of the Pandora cluster. In late 2014 we obtained a deep (110 ks) observation of this cluster with XMM-Newton, with the aim of making a detailed comparison between the optical, X-ray and lensing properties of this system. The new X-ray observation unveiled the presence of three hot gas filaments extending on scales of several Mpc and connected to the cluster core. The X-ray structures coincide spatially with the distribution of galaxies and dark matter and provide strong evidence for the existence of the elusive warm-hot intergalactic medium (WHIM). The new observation also reveals the complexity of the thermodynamic structure of the cluster core and a probable shock front associated with the radio relic located 1 Mpc NW of the cluster core.

Keywords

galaxies: clusters: individual (Abell 2744)X-rays: galaxies: clustersgravitational lensinglarge-scale structure of universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 760 - 763
Copyright
Copyright © International Astronomical Union 2016 

References

Bonafede, A., Brüggen, M., van Weeren, R., et al. 2012, MNRAS, 426, 40 Google Scholar
Boschin, W., Girardi, M., Spolaor, M., & Barrena, R. 2006, A&A, 449, 461 Google Scholar
Cen, R. & Ostriker, J. P. 1999, ApJ, 514, 1 Google Scholar
Davé, R., Cen, R., Ostriker, J. P., et al. 2001, ApJ, 552, 473 Google Scholar
Eckert, D., Jauzac, M., Shan, H. Y. et al. 2015, Nature, in pressGoogle Scholar
Jullo, E. & Kneib, J.-P. 2009, MNRAS, 395, 1319 Google Scholar
Merten, J., Coe, D., Dupke, R., et al. 2011, MNRAS, 417, 333 Google Scholar
Ogrean, G. A., Brüggen, M., van Weeren, R. J., et al. 2013, MNRAS, 433, 812 Google Scholar
Orrú, E., Murgia, M., Feretti, L., et al. 2007, A&A, 467, 943 Google Scholar
Owers, M. S., Randall, S. W., Nulsen, P. E. J., et al. 2011, ApJ, 728, 27 Google Scholar
Kempner, J. C. & David, L. P. 2004, MNRAS, 349, 385 Google Scholar
Ricker, P. M. & Sarazin, C. L. 2001, ApJ, 561, 621 Google Scholar
Springel, V., Frenk, C. S., & White, S. D. M. 2006, Nature, 440, 1137 Google Scholar
Vazza, F., Brunetti, G., Gheller, C., & Brunino, R. 2010, New Astronomy, 15, 695 Google Scholar
Vazza, F., Eckert, D., Brüggen, M., & Huber, B. 2015, MNRAS, 451, 2198 CrossRefGoogle Scholar