Volume 403, Number 1, May III 2003
|Page(s)||11 - 27|
|Section||Cosmology (including clusters of galaxies)|
|Published online||29 April 2003|
A radial mass profile analysis of the lensing cluster MS 2137.3–2353 *
Institut d'Astrophysique de Paris, UMR 7095, 98bis boulevard Arago, 75014 Paris, France
2 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
3 Observatoire Midi-Pyrénées, UMR 5572, 14 Av. E. Belin, 31400 Toulouse, France
Corresponding author: R. Gavazzi, firstname.lastname@example.org
Accepted: 21 February 2003
We reanalyze the strong lens modeling of the cluster of galaxies MS 2137.3–2353 using a new UBVRIJK data set obtained with the ESO Very Large Telescope. We infer the photometric redshifts of the two main arc systems which are both found to be at . After subtraction of the central cD star light in the previous F702/HST imaging we found only one object lying underneath. This object has the expected properties of the fifth image associated to the tangential arc. It lies at the right location, shows the right orientation and has the expected signal-to-noise ratio. We improve the previous lens modelings of the central dark matter distribution of the cluster, using two density profiles: an isothermal model with a core, and the NFW-like model with a cusp. Without the fifth image, the arc properties together with the shear map profile are equally well fit by the isothermal model and by a sub-class of generalized-NFW mass profiles having inner slope power index in the range . Adding new constrains on the center lens position provided by the fifth image favors isothermal profiles that better predict the fifth image properties. A detailed model including nearby cluster galaxy perturbations or the effect of the stellar mass distribution to the total mass inward does not change our conclusions but imposes the of the cD stellar component is below 10 at a 99% confidence level. Using our new detailed strong+weak lensing model together with Chandra X-ray data and the cD stellar component we finally discuss intrinsic properties of the gravitational potential. Whereas X-ray and dark matter have a similar orientation and ellipticity at various radius, the cD stellar isophotes are twisted by . The sub-arc-second azimuthal shift we observe between the radial arc position and the predictions of elliptical models correspond to what is expected from a mass distribution twist. This shift may result from a projection effect of the cD and the cluster halos, thus revealing the triaxiality of the mass components.
Key words: dark matter / galaxies: clusters: individual: MS 2137.3–2353 / gravitational lensing
© ESO, 2003
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