Cosmic shear analysis in 50 uncorrelated VLT fields. Implications for , ^*

¹ Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
² Observatoire de Paris, DEMIRM, 61 avenue de l'Observatoire, 75014 Paris, France
³ Universitá "La Sapienza", P.le Aldo Moro 2, 00185 Roma, Italy
⁴ Canadian Institute for Theoretical Astrophysics, 60 St George Street, Toronto, M5S 3H8 Ontario, Canada
⁵ Institut für Astrophysik und Extraterrestrische Forschung der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
⁶ Dept. of Physics, Johns Hopkins University, Baltimore, MD 21218, USA
⁷ Service de Physique Théorique, C.E. de Saclay, 91191 Gif-sur-Yvette Cedex, France
⁸ Max Planck Institut fur Astrophysiks, Karl-Schwarzschild-Str. 1, Postfach 1523, 85740 Garching, Germany

Corresponding author: Y. Mellier, mellier@iap.fr

Received: 14 November 2000
Accepted: 8 January 2001

Abstract

We observed with the camera FORS1 on the VLT (UT1, ANTU) 50 randomly selected fields and analyzed the cosmic shear inside circular apertures with diameter ranging from 0.5 to 5.0 arcmin. The images were obtained in optimal conditions using the Service Observing proposed by ESO on the VLT, which enabled us to a well-defined and homogeneous set of data. The 50 fields cover a 0.64 square-degrees area spread over more than 1000 square-degrees obtain which provides a sample ideal for minimizing the cosmic variance. Using the same techniques as in Van Waerbeke et al. ([CITE]), we measured the cosmic shear signal and investigated the systematics of the VLT sample. We find a significant excess of correlations between galaxy ellipticities on those angular scales. The amplitude and the shape of the correlation as function of angular scale are remarkably similar to those reported so far. Using our combined VLT and CFHT data and adding the results published by other teams we put the first joint constraints on and using cosmic shear surveys. From a deduced average of the redshift of the sources the combined data are consistent with (for a CDM power spectrum and ), in excellent agreement with the cosmological constraints obtained from the local cluster abundance. This is consistent with theoretical expectations if the density field grew from initial Gaussian conditions.