Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published September 2004 | Published
Journal Article Open

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

Abstract

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.

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.

Attached Files

Published - Yan_2004_ApJS_154_75.pdf

Files

Yan_2004_ApJS_154_75.pdf
Files (303.2 kB)
Name Size Download all
md5:593550baaffc47c7c8d1af3478d86467
303.2 kB Preview Download

Additional details

Created:
August 22, 2023
Modified:
October 25, 2023