XMM-Newton's Views of Clusters from the REFLEX-DXL Sample
Minimum credit line: Image courtesy of Hans Boehringer (Max-Planck-Institut fuer Extraterrestrische Physik) and ESA. (for details, see Conditions of Use).
Credit: ESA/XMM-Newton, CC BY-SA 3.0 IGO
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XMM-Newton's EPIC cameras' views of REFLEX-DXL galaxy clusters, with contours superimposed. The investigators composed a sample of distant, X-ray luminous galaxy clusters in the redshift range z=0.26 to 0.31, with X-ray luminosities greater than 1.e+45 erg/s for the 0.1-2.4 keV band (the REFLEX-DXL sample) to investigate the scaling relations of massive galaxy clusters. The panels shows merged images from the MOS1, MOS2 and pn cameras of the clusters as seen in the 0.5-2 keV energy band. The cosmic evolution of large-scale structure (LSS) can be probed using the number density of clusters of galaxies, and hence studies of number density can be used to test cosmological models. The largest clusters are anticipated to demonstrate the largest evolutionary effects and therefore are particularly important in tracing LSS evolution. Since the REFLEX-DXL cluster galaxies are X-ray luminous they can be inferred to be very massive. The structure of the X-ray emitting intracluster plasma depends primarily on gravitational effects and shock heating for the most massive clusters (this dependence weakens as cluster mass decreases). Therefore hierarchical modelling should describe more massive clusters better, making them the most useful for comparisons of observations with theory.
Investigator(s): H. Boehringer, Y.-Y. Zhang, A. Finoguenov, Y. Ikebe, K. Matsushita, P. Schuecker, L. Guzzo, C. A. Collins
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- Read the Journal article
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http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2006A%26A...456...55Z&am - Detailed description of this image
- For unfamiliar terms, visit the XMM-Newton Astronomical Glossary
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