First Results on Shear-selected Clusters from the Deep Lens Survey: Optical Imaging, Spectroscopy, and X-Ray Follow-up
We present the first sample of galaxy clusters selected on the basis of their weak gravitational lensing shear. The shear induced by a cluster is a function of its mass profile and its redshift relative to the background galaxies being sheared; in contrast to more traditional methods of selecting clusters, shear selection does not depend on the cluster's star formation history, baryon content, or dynamical state. Because mass is the property of clusters that provides constraints on cosmological parameters, the dependence on these other parameters could induce potentially important biases in traditionally selected samples. Comparison of a shear-selected sample with optically and X-ray-selected samples is therefore of great importance. Here we present the first step toward a new shear-selected sample: the selection of cluster candidates from the first 8.6 deg^2 of the 20 deg^2 Deep Lens Survey (DLS), and tabulation of their basic properties such as redshifts and optical and X-ray counterparts.
Additional Information© 2006 The American Astronomical Society. Received 2005 July 23; accepted 2006 January 18. We thank Matt Auger and Chris Fassnacht for assistance in reducing LRIS spectroscopy, Perry Gee for providing the redshift of CXOU J105535-045930, and Jim Bosch for assistance with preparing figures. The DLS has received generous support from Lucent Technologies and from NSF grants AST 04-41072 and AST 01-34753. Support for this work was also provided by the National Aeronautics and Space Administration through Chandra awards GO3-4173A and GO3-4173B issued to Rutgers and University of California at Davis by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. We also thank NOAO for supporting survey programs, and the 2dFGRS project for making data publicly available. Observations were obtained at Cerro Tololo Inter-American Observatory and the W. M. Keck Observatory. CTIO is a division of the National Optical Astronomy Observatory (NOAO), which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. This work also made use of the Image Reduction and Analysis Facility (IRAF), the NASA/IPAC Extragalactic Database (NED), the NASA Astrophysics Data System (ADS), and SAOImage DS9, developed by the Smithsonian Astrophysical Observatory.
Published - WITapj06.pdf
Accepted Version - 0507606.pdf