EDP Sciences
Free Access
Volume 434, Number 2, May I 2005
Page(s) 433 - 448
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361:20041643
Published online 11 April 2005

A&A 434, 433-448 (2005)
DOI: 10.1051/0004-6361:20041643

A CFH12k lensing survey of X-ray luminous galaxy clusters

I. Weak lensing methodology
S. Bardeau1, J.-P. Kneib1, 2, O. Czoske3, 1, G. Soucail1, I. Smail4, H. Ebeling5 and G. P. Smith2

1  Observatoire Midi-Pyrénées, UMR5572, 14 Avenue Edouard Belin, 31400 Toulouse, France
    e-mail: bardeau@ast.obs-mip.fr
2  Caltech, Astronomy, 105-24 Pasadena, CA 91125, USA
3  Institut für Astrophysik und Extraterrestrische Forschung, Auf dem Hügel 71, 53121 Bonn, Germany
4  Institute for Computational Cosmology, University of Durham, South Road, Durham DH1 3LE, UK
5  Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr, Honolulu, HI 96822, USA

(Received 12 July 2004 / Accepted 9 January 2005 )

We describe the weak lensing methodology we have applied to multi-colour CFH12k imaging of a homogeneously-selected sample of luminous X-ray clusters at $z\sim 0.2$. The aim of our survey is to understand the variation in cluster structure and dark matter profile within rich clusters. The method we describe converts a fully reduced CFH12k image into constraints on the cluster mass distribution in two steps: (1) determination of the "true" shape of faint (lensed) galaxies, including object detection, point spread function (PSF) determination, galaxy shape measurement with errors; (2) conversion of the faint galaxy catalogue into reliable mass constraints using a range of 1D and 2D lensing techniques. Mass estimates are derived independently from each of the three images taken in separate filters to quantify the systematic uncertainties. Finally, we compare the cluster mass model to the light distribution of cluster members as derived from our imaging data. To illustrate the method, we apply it to the well-studied cluster Abell 1689 (z=0.184). In this cluster, we detect the gravitational shear signal out to ~3 Mpc at >3-$\sigma$ significance. The two-dimensional mass reconstruction has a ~10-$\sigma$ significance peak centered on the brightest cluster galaxy. The weak lensing profile is well fitted by a NFW mass profile with M200 = 14.1+6.3-4.7 $\times$ $10^{14}~M_{\odot}$, and c = 3.5+0.5-0.3 ( $\chi^2=0.33$), or by a power law profile with q=0.75 $\pm$ 0.07 and $\theta_{\rm E} = 14\farcs6$ $\pm$ $0\farcs3$ ( $\chi^2=0.64$). The mass-to-light ratio is found to be almost constant with radius with a mean value of $M/L_R = 150\,h\,(M/L)_{\odot}$. We compare these results to other weak lensing analyses of Abell 1689 from the literature and find good agreements in terms of the shear measurement as well as the final mass estimate.

Key words: gravitational lensing -- galaxies: clusters: general -- galaxies: clusters: individual: Abell 1689

SIMBAD Objects

© ESO 2005

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