Mass and light in the supercluster of galaxies MS0302+17

Free access article

Issue		A&A Volume 422, Number 2, August I 2004


Page(s)		407 - 422
Section		Cosmology (including clusters of galaxies)
DOI		http://dx.doi.org/10.1051/0004-6361:20047109

A&A 422, 407-422 (2004)
DOI: 10.1051/0004-6361:20047109

Mass and light in the supercluster of galaxies MS0302+17

R. Gavazzi¹, Y. Mellier^{1, 2}, B. Fort¹, J.-C. Cuillandre³ and M. Dantel-Fort²

¹ Institut d'Astrophysique de Paris, UMR 7095, 98 bis Boulevard Arago, 75014 Paris, France
e-mail: gavazzi@iap.fr
² Observatoire de Paris, LERMA, UMR 8112, 61 Avenue de l'Observatoire, 75014 Paris, France
³ Canada-France-Hawaii Telescope, 65-1238 Mamalahoa Highway, Kamuela, HI 96743, USA

(Received 20 January 2004 / Accepted 8 April 2004 )

Abstract
We investigate the supercluster MS0302+17 ( $z \approx 0.42$ ) using weak lensing analysis and deep wide field $\it BVR$ photometry with the CFH12K camera. Using (B-V) vs. (V-R) evolution tracks we identify early-type members of the supercluster, and foreground ellipticals. We derive a R band catalogue of background galaxies for weak lensing analysis. We compute the correlation functions of light and mass and their cross-correlation and test if light traces mass on supercluster, cluster and galaxy scales.

We show that the data are consistent with this assertion. The $\zeta$ -statistic applied in regions close to cluster centers and global correlation analyses over the whole field converge toward the simple relation $M/L=300\pm30\,h_{70}\,({\it M/L})_\odot$ in the B band. This independently confirms the earlier results obtained by Kaiser et al. (1998).

If we model dark matter halos around each early-type galaxy by a truncated isothermal sphere, we find that a linear relation $M\propto L$ still holds. In this case, the average halo truncation radius is $s_* \la 200h^{-1}_{70}\,{\rm kpc}$ close to clusters cores whereas it reaches a lower limit of ~ $300h^{-1}_{70}\,{\rm kpc}$ at the periphery. This change of s_* as a function of radial distance may be interpreted as a result of tidal stripping of early type galaxies. Nevertheless the lack of information on the spatial distribution of late-type galaxies affects such conclusions concerning variations of s_*.

Though all the data at hand are clearly consistent with the assumption that mass is faithfully traced by light from early-type galaxies, we are not able to describe in detail the contribution of late type galaxies. We however found it to be small. Forthcoming wide surveys in UV, visible, and near infrared wavelengths will provide large enough samples to extend this analysis to late-type galaxies using photometric redshifts.

Key words: cosmology: large-scale structure of Universe -- gravitational lensing -- cosmology: dark matter

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