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Clustering of dust-obscured galaxies at z ~ 2

Brodwin, Mark and Dey, Arjun and Brown, Michael J. I. and Pope, Alexandra and Armus, Lee and Bussmann, Shane and Desai, Vandana and Jannuzi, Buell T. and Le Floc'h, Emeric (2008) Clustering of dust-obscured galaxies at z ~ 2. Astrophysical Journal Letters, 687 (2). L65-L68. ISSN 2041-8205. http://resolver.caltech.edu/CaltechAUTHORS:BROapjl08

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Abstract

We present the angular autocorrelation function of 2603 dust-obscured galaxies (DOGs) in the Boötes field of the NOAO Deep Wide-Field Survey. DOGs are red, obscured galaxies, defined as having R−[24] ≥ 14 (F24/FR ≳ 1000). Spectroscopy indicates that they are located at 1.5 ≾ z ≾ 2.5. We find strong clustering, with r_0 = 7.40−(0.84+^1.27-0.84)h^−1 Mpc for the full F_(24 )> 0.3 mJy sample. The clustering and space density of the DOGs are consistent with those of submillimeter galaxies, suggestive of a connection between these populations. We find evidence for luminosity-dependent clustering, with the correlation length increasing to r_0 = 12.97_(−2.64)^(+4.26)h^−1 Mpc for brighter F_(24)> 0.6 mJy) DOGs. Bright DOGs also reside in richer environments than fainter ones, suggesting these subsamples may not be drawn from the same parent population. The clustering amplitudes imply average halo masses of log M = 12.2_(−0.2)^(+0.3) M⊙ for the full DOG sample, rising to log M = 13.0_(−0.3)6(+0.4) M⊙ for brighter DOGs. In a biased structure formation scenario, the full DOG sample will, on average, evolve into ~3L* present-day galaxies, whereas the most luminous DOGs may evolve into brightest cluster galaxies.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/593327DOIUNSPECIFIED
http://www.iop.org/EJ/abstract/1538-4357/687/2/L65/PublisherUNSPECIFIED
ORCID:
AuthorORCID
Brown, Michael J. I.0000-0002-1207-9137
Additional Information:© 2008. The American Astronomical Society. Received 2008 July 28; accepted 2008 September 22; published 2008 October 21. M. B. is grateful to M. Dickinson and NOAO for supporting this research. We thank M. White for providing his HaloFit code and halo correlation functions, and for a careful reading of the manuscript. We thank the anonymous referee for helpful comments. 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. We used data products from the NDWFS, which was supported by NOAO, AURA, Inc., and the NSF. NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation.
Funders:
Funding AgencyGrant Number
National Optical Astronomy ObservatoryUNSPECIFIED
Association of Universities for Research in Astronomy Inc.UNSPECIFIED
NSFUNSPECIFIED
NASAUNSPECIFIED
Subject Keywords:galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: statistics; large-scale structure of universe.
Record Number:CaltechAUTHORS:BROapjl08
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:BROapjl08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13575
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:27 May 2009 22:17
Last Modified:06 Oct 2017 00:14

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