The fundamental plane of clusters of galaxies. Issue 4 (2nd May 2013)

• Record Type: Journal Article
• Authors: D'Onofrio, M.; Bettoni, D.; Bindoni, D.; Cava, A.; Fasano, G.; Marziani, P.; Moles, M.; Moretti, A.; Poggianti, B.M.; Varela, J.; Schartel, Norbert
• Is Part Of: Astronomische Nachrichten. Volume 334:Issue 4/5(2013)
• Page Start: 373
• Page End: 376
• Publication Date: 2013-05-02
• Subjects: Astronomy -- Periodicals; 520.5
• DOI: 10.1002/asna.201211860
• Languages: English
• ISSNs: 0004-6337

Abstract

<abstract abstract-type="main" xml:lang="en"> <title>Abstract</title> <p>We have analyzed the growth curves and the surface brightness light profiles of the clusters of the WINGS sample (Fasano et al. 2006) in the B and V bands, measuring the effective radii, the effective surface brightnesses and the total luminosities of our clusters. The similarly of the radial surface brightness profiles of early‐type galaxies (ETGs) and clusters indicate that within r200 almost all clusters are virialized structures. The total luminosities <italic>L</italic>_{<italic>B</italic>} of clusters are found to correlate with the X‐ray luminosity <italic>L</italic>_{<italic>X</italic>}, following approximately the same relation measured for galaxies by Eskridge et al. (1995). By coupling the photometric data with the central velocity dispersions, derived from the radial velocities of the galaxies measured by Cava et al. (2009), we were able to fit the fundamental plane (FP) of clusters of galaxies. We find that it has approximately the same slope of the FPs of early‐type galaxies (ETGs) and globular clusters (GCs), but differs from them in the zero‐point. This behavior can be easily explained in terms of a different contribution of dark matter (DM). (© 2013 WILEY‐VCH Verlag GmbH &amp; Co. KGaA, Weinheim)</p> </abstract>