Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey

doi:10.1086/590105

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The Astrophysical Journal Volume 684 Number 2 Create an alert RSS this journal

Peter R. M. Eisenhardt et al. 2008 ApJ 684 905 doi:10.1086/590105

Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey

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Peter R. M. Eisenhardt¹, Mark Brodwin², Anthony H. Gonzalez³, S. Adam Stanford^4,5, Daniel Stern¹, Pauline Barmby⁶, Michael J. I. Brown⁷, Kyle Dawson⁸, Arjun Dey², Mamoru Doi⁹, Audrey Galametz^1,10, B. T. Jannuzi², C. S. Kochanek¹¹, Joshua Meyers^8,12, Tomoki Morokuma^9,13 and Leonidas A. Moustakas¹

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peter.eisenhardt@jpl.nasa.gov

¹ Jet Propulsion Laboratory, California Institute of Technology, MS 169-327, 4800 Oak Grove Drive, Pasadena, CA 91109
² National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719
³ Department of Astronomy, University of Florida, Gainesville, FL 32611
⁴ University of California, Davis, CA 95618
⁵ Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, CA 94550
⁶ Department of Physics and Astronomy, University of Western Ontario, 1151 Richmond Street, London, ON N6A 3K7, Canada
⁷ School of Physics, Monash University, Clayton, Victoria 3800, Australia
⁸ E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720
⁹ Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
¹⁰ Observatoire Astronomique de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France
¹¹ Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210
¹² Department of Physics, University of California, Berkeley, CA 94720
¹³ National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

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Abstract References Cited By

We have identified 335 galaxy cluster and group candidates, 106 of which are at z > 1, using a 4.5 μm-selected sample of objects from a 7.25 deg² region in the Spitzer Infrared Array Camera (IRAC) Shallow Survey. Clusters were identified as three-dimensional overdensities using a wavelet algorithm, based on photometric redshift probability distributions derived from IRAC and NOAO Deep Wide-Field Survey data. We estimate only ~10% of the detections are spurious. To date 12 of the z > 1 candidates have been confirmed spectroscopically, at redshifts from 1.06 to 1.41. Velocity dispersions of ~750 km s⁻¹ for two of these argue for total cluster masses well above 10¹⁴ M, as does the mass estimated from the rest-frame near-infrared stellar luminosity. Although not selected to contain a red sequence, some evidence for red sequences is present in the spectroscopically confirmed clusters, and brighter galaxies are systematically redder than the mean galaxy color in clusters at all redshifts. The mean I − [ 3.6] color for cluster galaxies up to z ~ 1 is well matched by a passively evolving model in which stars are formed in a 0.1 Gyr burst starting at redshift z_f = 3. At z > 1, a wider range of formation histories is needed, but higher formation redshifts (i.e., z_f > 3) are favored for most clusters.

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