Discovery of a High-Redshift (z = 0.96) Cluster of Galaxies Using a FIRST Survey Wide-Angle-Tailed Radio Source*

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© 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation Elizabeth L. Blanton et al 2003 AJ 125 1635 DOI 10.1086/368140

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Author affiliations

1 Chandra Fellow

2 Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903

3 Visiting Astronomer, Kitt Peak National Observatory (KPNO), National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation

4 Department of Physics, University of California, Davis, 1 Shields Avenue, Davis, CA 95616

5 Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, L-413, P.O. Box 808, Livermore, CA 94550

6 Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027

7 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218

Dates

  1. Received 2002 November 8
  2. Accepted 2002 December 17
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1538-3881/125/4/1635

Abstract

Using a combination of near-infrared and optical photometry, along with multiobject spectroscopy, we have confirmed the existence of a high-redshift cluster of galaxies at z = 0.96. The cluster was found using a wide-angle–tailed radio source selected from the VLA FIRST survey as a cluster signpost. These types of radio sources are often found in clusters and are thought to attain their C-shaped morphologies from the relative motion between the radio source host galaxy and the intracluster medium. We present optical/near-infrared color-magnitude diagrams that show a concentration of cluster galaxies in color space. We also include spectroscopic results obtained from the Keck II Low Resolution Imaging Spectrometer. Ten galaxies are confirmed at the cluster redshift, with a line-of-sight velocity dispersion of σ∥ = 530 km s-1, typical of an Abell richness class 0 cluster. Using data from the ROSAT public archive, we limit the X-ray luminosity for the cluster to LX,bol ≲ 3 × 1044 ergs s-1, consistent with the value expected from the LX-σ relation.

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Footnotes

  • * 

    Based in part on observations obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

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10.1086/368140