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Photometric redshifts in the Irac shallow survey

Brodwin, M. and Brown, M. J. I. and Ashby, M. L. N. and Bian, C. and Brand, K. and Dey, A. and Eisenhardt, P. R. and Eisenstein, D. J. and Gonzalez, A. H. and Huang, J.-S. and Jannuzi, B. T. and Kochanek, C. S. and McKenzie, E. and Murray, S. S. and Pahre, M. A. and Smith, H. A. and Soifer, B. T. and Stanford, S. A. and Stern, D. and Elston, R. J. (2006) Photometric redshifts in the Irac shallow survey. Astrophysical Journal, 651 (2). pp. 791-803. ISSN 0004-637X.

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Accurate photometric redshifts are calculated for nearly 200,000 galaxies to a 4.5 μm flux limit of ~13 μJy in the 8.5 deg^2 Spitzer IRAC Shallow Survey. Using a hybrid photometric redshift algorithm incorporating both neural net and template-fitting techniques, calibrated with over 15,000 spectroscopic redshifts, a redshift accuracy of σ = 0.06(1 + z) is achieved for 95% of galaxies at 0 < z < 1.5. The accuracy is σ = 0.12(1 + z) for 95% of active galactic nuclei (AGNs) at 0 < z < 3. Redshift probability functions, central to several ongoing studies of the galaxy population, are computed for the full sample. We demonstrate that these functions accurately represent the true redshift probability density, allowing the calculation of valid confidence intervals for all objects. These probability functions have already been used to successfully identify a population of Spitzer-selected high-redshift (z > 1) galaxy clusters. We present one such spectroscopically confirmed cluster at <z> = 1.24, ISCS J1434.5+3427. Finally, we present a measurement of the 4.5 μm-selected galaxy redshift distribution.

Item Type:Article
Related URLs:
URLURL TypeDescription
Brodwin, M.0000-0002-4208-798X
Brown, M. J. I.0000-0002-1207-9137
Ashby, M. L. N.0000-0002-3993-0745
Dey, A.0000-0002-4928-4003
Gonzalez, A. H.0000-0002-0933-8601
Jannuzi, B. T.0000-0002-1578-6582
Kochanek, C. S.0000-0001-6017-2961
Stern, D.0000-0003-2686-9241
Additional Information:© 2006 The American Astronomical Society. Received 2006 April 26; accepted 2006 July 13. We are grateful and indebted to the teams who built the instruments used in this project. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This paper made use of data from the NOAO Deep Wide-Field Survey (NDWFS), which was supported by NOAO, AURA, Inc., and the National Science Foundation. We thank the entire NDWFS survey team and those who operate and maintain Kitt Peak National Observatory, whose facilities were used to obtain the NDWFS Bootes field images. Spectroscopic redshifts that contributed to the training of our photometric redshift algorithms were obtained by numerous groups. In addition to the vast number of redshifts from the AGES survey described in the text, redshifts were contributed by various projects, including ones led by Hyron Spinrad, Steve Dawson, Richard Green, James Rhoads, Sangeeta Malhotra, and George Djorgovski. We are grateful to them for generously sharing their redshifts with us. We are grateful to the staff of the MMT Observatory, W. M. Keck Observatory, and KPNO for their help with obtaining the various spectroscopic data. A. H. G. and E. M. acknowledge support from an NSF Small Grant for Exploratory Research under award AST 04-36681. S. A. S.’s work was performed under the auspices of the US Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract W-7405-Eng-48.
Funding AgencyGrant Number
NSFAST 04-36681
Department of Energy (DOE)W-7405-ENG-48
Subject Keywords:galaxies: clusters: general; galaxies: clusters: individual (ISCS J1434.5+3427); galaxies: distances and redshifts; galaxies: evolution; galaxies: photometry; methods: statistical
Issue or Number:2
Record Number:CaltechAUTHORS:20110218-082815155
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Official Citation:Photometric Redshifts in the IRAC Shallow Survey M. Brodwin, M. J. I. Brown, M. L. N. Ashby, C. Bian, K. Brand, A. Dey, P. R. Eisenhardt, D. J. Eisenstein, A. H. Gonzalez, J.-S. Huang, B. T. Jannuzi, C. S. Kochanek, E. McKenzie, S. S. Murray, M. A. Pahre, H. A. Smith, B. T. Soifer, S. A. Stanford, D. Stern, and R. J. Elston doi: 10.1086/507838
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22367
Deposited By: Ruth Sustaita
Deposited On:18 Feb 2011 17:00
Last Modified:04 Nov 2019 05:45

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