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Spitzer 24 Micron Observations of Optical/Near‐Infrared–Selected Extremely Red Galaxies: Evidence for Assembly of Massive Galaxies at z ∼ 1–2?

Yan, Lin and Choi, Philip I. and Fadda, D. and Marleau, F. R. and Soifer, B. T. and Im, M. and Armus, L. and Frayer, D. T. and Storrie‐Lombardi, L. J. and Thompson, D. J. and Teplitz, H. I. and Helou, G. and Appleton, P. N. and Chapman, S. and Fang, F. and Heinrichsen, I. and Lacy, M. and Shupe, D. L. and Squires, G. K. and Surace, J. and Wilson, G. (2004) Spitzer 24 Micron Observations of Optical/Near‐Infrared–Selected Extremely Red Galaxies: Evidence for Assembly of Massive Galaxies at z ∼ 1–2? Astrophysical Journal Supplement Series, 154 (1). pp. 75-79. ISSN 0067-0049.

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We carried out direct measurement of the fraction of dusty sources in a sample of extremely red galaxies with (R - K_s) ≥ 5.3 mag and K_s < 20.2 mag, using 24 μm data from the Spitzer Space Telescope. Combining deep 24 μm Ks- and R-band data over an area of ~64 arcmin^2 in ELAIS N1 of the Spitzer First Look Survey (FLS), we find that 50% ± 6% of our extremely red object (ERO) sample have measurable 24 μm flux above the 3 σ flux limit of 40 μJy. This flux limit corresponds to a star formation rate (SFR) of 12 M_⊙ yr^(-1) at z ~ 1, much more sensitive than any previous long-wavelength measurement. The 24 μm-detected EROs have 24 μm/2.2 μm and 24 μm/0.7 μm flux ratios consistent with infrared luminous, dusty sources at z ≥ 1, and are an order of magnitude too red to be explained by an infrared quiescent spiral or a pure old stellar population at any redshift. Some of these 24 μm-detected EROs could be active galactic nuclei; however, the fraction among the whole ERO sample is probably small, 10%-20%, as suggested by deep X-ray observations as well as optical spectroscopy. Keck optical spectroscopy of a sample of similarly selected EROs in the FLS field suggests that most of the EROs in ELAIS N1 are probably at z ~ 1. The mean 24 μm flux (167 μJy) of the 24 μm-detected ERO sample roughly corresponds to the rest-frame 12 μm luminosity, νL_ν(12 μm), of 3 × 10^(10) L_⊙ at z ~ 1. Using the correlation between IRAS νL_ν(12 μm) and infrared luminosity LIR(8-1000 μm), we infer that the 〈L_(IR)〉 of the 24 μm-detected EROs is 3 × 10^(11) and 1 × 10^(12) L_⊙ at z = 1.0 and 1.5, respectively, similar to that of local luminous infrared galaxies (LIRGs) and ultraluminous infrared galaxies (ULIRGs). The corresponding SFR would be roughly 50-170 M_⊙ yr^(-1). If the timescale of this starbursting phase is on the order of 10^8 yr as inferred for the local LIRGs and ULIRGs, the lower limit on the masses of these 24 μm-detected EROs is 5 × 10^9 to 2 × 10^(10) M_⊙. It is plausible that some of the starburst EROs are in the midst of a violent transformation to become massive early type galaxies at the epoch of z ~ 1-2.

Item Type:Article
Related URLs:
URLURL TypeDescription
Yan, Lin0000-0003-1710-9339
Fadda, D.0000-0002-3698-7076
Im, M.0000-0002-8537-6714
Armus, L.0000-0003-3498-2973
Frayer, D. T.0000-0003-1924-1122
Teplitz, H. I.0000-0002-7064-5424
Helou, G.0000-0003-3367-3415
Appleton, P. N.0000-0002-7607-8766
Lacy, M.0000-0002-3032-1783
Shupe, D. L.0000-0003-4401-0430
Squires, G. K.0000-0002-1977-5717
Surace, J.0000-0001-7291-0087
Wilson, G.0000-0002-6572-7089
Additional Information:© 2004 American Astronomical Society. Received 2004 April 5. Accepted 2004 May 25. 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 NASA contract 1407. Support for this work was provided by NASA. The spectroscopic data presented herein were 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. We also wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:galaxies: bulges; galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20170324-082411883
Persistent URL:
Official Citation:Lin Yan et al 2004 ApJS 154 75
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75374
Deposited By: Ruth Sustaita
Deposited On:24 Mar 2017 17:27
Last Modified:09 Mar 2020 13:19

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