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Identification of a Complete 160 μm Flux-limited Sample of Infrared Galaxies in the ISO Lockman Hole 1 deg^2 Deep Fields: Source Properties and Evidence for Strong Evolution in the FIR Luminosity Function for ULIRGs

Jacobs, B. A. and Sanders, D. B. and Rupke, D. S. N. and Aussel, H. and Frayer, D. T. and Ilbert, O. and Kartaltepe, J. S. and Kawara, K. and Kim, D.-C. and Le Floc’h, E. and Murayama, T. and Smolčić, V. and Surace, J. A. and Taniguchi, Y. and Veilleux, S. and Yun, M. S. (2011) Identification of a Complete 160 μm Flux-limited Sample of Infrared Galaxies in the ISO Lockman Hole 1 deg^2 Deep Fields: Source Properties and Evidence for Strong Evolution in the FIR Luminosity Function for ULIRGs. Astronomical Journal, 141 (4). Art. No. 110. ISSN 0004-6256.

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We have identified a complete, flux-limited (S_(160) > 120 mJy) sample of 160 μm selected sources from Spitzer observations of the 1 deg^2 Infrared Space Observatory (ISO) Deep Field region in the Lockman Hole (LH). Ground-based UV, optical, and near-infrared (NIR) photometry and optical spectroscopy have been used to determine colors, redshifts, and masses for the complete sample of 40 galaxies. Spitzer-IRAC+MIPS photometry, supplemented by ISOPHOT data at 90 μm and 170 μm, has been used to calculate accurate total infrared luminosities, L_(IR)(8-1000 μm), and to determine the IR luminosity function (LF) of luminous infrared galaxies (LIRGs). The maximum observed redshift is z ~ 0.80 and the maximum total infrared luminosity is log (L_(IR)/L_⊙) = 12.74. Over the luminosity range log (L_(IR)/L_⊙)) = 10-12, the LF for LIRGs in the LH Deep Field is similar to that found previously for local sources at similar infrared luminosities. The mean host galaxy mass, log (M/M_⊙ ) = 10.7, and dominance of H_(II)-region spectral types, is also similar to what has been found for local LIRGs, suggesting that intense starbursts likely power the bulk of the infrared luminosity for sources in this range of L_(IR). However for the most luminous sources, log (L_(IR)/L_⊙ ) > 12.0, we find evidence for strong evolution in the LF ∝ (1 + z)^(6±1), assuming pure number density evolution. These ultraluminous infrared galaxies (ULIRGs) have a larger mean host mass, log (M/M_⊙) = 11.0, and exhibit disturbed morphologies consistent with strong interactions/mergers, and they are also more likely to be characterized by starburst-active galactic nucleus (AGN) composite or AGN spectral types.

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Surace, J. A.0000-0001-7291-0087
Additional Information:© 2011 American Astronomical Society. Received 2010 September 10; accepted 2010 November 17; published 2011 February 24. We benefited from the published data and preliminary analyses of S. Oyabu. V.S. acknowledges support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST-0838260, and also received funding from the European Union’s Seventh Framework programme under grant agreement 229517. Y.T. was financially supported in part by the Ministry of Education, Culture, Sports, Science and Technology (Nos. 10044052 and 10304013), and by the JSPS (Nos. 15340059, 17253001, and 19340046). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The participating institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck- Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Owens Valley Radio Observatory UNSPECIFIED
European Research Council (ERC)229517
Ministry of Education, Culture, Sports, Science and Technology (MEXT)10044052
Ministry of Education, Culture, Sports, Science and Technology (MEXT)10304013
Japan Society for the Promotion of Science (JSPS)15340059
Japan Society for the Promotion of Science (JSPS)17253001
Japan Society for the Promotion of Science (JSPS)19340046
Alfred P. Sloan Foundation UNSPECIFIED
Participating Institutions UNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:galaxies: evolution – infrared: galaxies
Classification Code:PACS: 98.54.Cm, 98.62.Ai, 98.62.Qz, 98.62.Py, 98.62.Ck, 95.85.Hp
Record Number:CaltechAUTHORS:20110328-142023974
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Official Citation:B. A. Jacobs et al. 2011 The Astronomical Journal 141 110 doi: 10.1088/0004-6256/141/4/110
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23140
Deposited By: Benjamin Perez
Deposited On:28 Mar 2011 22:35
Last Modified:18 May 2017 21:56

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