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Title:
The WARPS Survey. VI. Galaxy Cluster and Source Identifications from Phase I
Authors:
Perlman, Eric S.; Horner, Donald J.; Jones, Laurence R.; Scharf, Caleb A.; Ebeling, Harald; Wegner, Gary; Malkan, Matthew
Affiliation:
AA(Guest Observer at the Canada-France-Hawaii Telescope. CFHT is operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.; Guest Observer at the W. M. Keck Observatory. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration.; Guest Observer at Lick Observatories. Lick Observatory is operated by the University of California.), AB(Guest Observer at Cerro Tololo Inter-American Observatory. CTIO is operated by the Association of University for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation.; Laboratory for High Energy Astrophysics, Code 662, Goddard Space Flight Center, Greenbelt, MD 20771.; Department of Astronomy, University of Maryland, College Park, MD 20742.), AC(Guest Observer at the W. M. Keck Observatory. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration.; Guest Observer at Lick Observatories. Lick Observatory is operated by the University of California.; School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK.), AD(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.; Guest Observer at Cerro Tololo Inter-American Observatory. CTIO is operated by the Association of University for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation.; Columbia Astrophysics Laboratory, Columbia University, Mail Code 5247, 550 West 120th Street, New York, NY 10027.), AE(Guest Observer at the W. M. Keck Observatory. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration.; Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822.; Observer at the University of Hawaii 2.2 m telescope on Mauna Kea.), AF(Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755.; Observer at the Michigan-Dartmouth-MIT Observatory.), AG(Guest Observer at Lick Observatories. Lick Observatory is operated by the University of California.; Department of Physics and Astronomy, University of California, Los Angeles, CA 90024.)
Publication:
The Astrophysical Journal Supplement Series, Volume 140, Issue 2, pp. 265-301. (ApJS Homepage)
Publication Date:
06/2002
Origin:
UCP
ApJ Keywords:
Surveys, X-Rays: Galaxies: Clusters, X-Rays: General
Abstract Copyright:
(c) 2002: The American Astronomical Society
DOI:
10.1086/339685
Bibliographic Code:
2002ApJS..140..265P

Abstract

We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06<z<0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5×2.0keV)=6.5×10-14ergcm-2s- 1. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160 deg2 survey.

Associated Articles

Part 1     Part  2     Part  3     Part  4     Part  5     Catalog Description     Part  6    


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