SpitzerObservations of Massive, Red Galaxies at High Redshift

2005/11/09 by Casey Papovich, L. A. Moustakas, Leonidas A. Moustakas +33 · 44 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Cosmic Phenomena #Galaxies: Formation, Evolution, Phenomena #astro-ph

paper · pdf · doi:10.1086/499915

published as Astrophys.J.640:92-113,2006 · Accepted for publication in the Astrophysical Journal. 25 pages, 14 figures

arxiv created 2005/11/09 · openalex publication_date 2006/03/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31

Abstract

We study massive galaxies at z ~ 1-3.5 using HST optical imaging, ground-based near-IR imaging, and Spitzer observations at 3-24 μm. From K s -selected galaxies in the ≃130 arcmin 2 GOODS-S field, we identify 153 distant red galaxies (DRGs) with ( J - K s ) Vega ≥ 2.3. This sample is approximately complete in stellar mass for passively evolving galaxies above 10 11 M ☉ and z ≤ 3. Roughly half of the DRGs are objects whose optical and near-IR rest-frame light is dominated by evolved stars combined with ongoing star formation (at z med ~ 2.5), and the others are galaxies whose light is dominated by heavily reddened ( A 1600 ≳ 4-6 mag) starbursts (at z med ~ 1.7). Very few DRGs (≲10%) have no indication of current star formation. DRGs at z ~ 1.5-3 with stellar masses ≥10 11 M ☉ have specific star formation rates (SFRs per unit mass) including the reradiated far-IR emission that range from 0.2 to 10 Gyr -1 . Based on the X-ray luminosities and rest-frame near-IR colors, roughly one-quarter of the DRGs contain AGNs, implying that the growth of supermassive black holes coincides with the formation of massive galaxies. At 1.5 ≤ z ≤ 3, the DRGs with M ≥ 10 11 M ☉ have an integrated specific SFR comparable to the global value of all galaxies. In contrast, galaxies at z ~ 0.3-0.75 with M ≥ 10 11 M ☉ have an integrated specific SFR less than the global value and more than an order of magnitude lower than that for massive DRGs. At z ≲ 1, lower mass galaxies dominate the overall cosmic mass assembly. This suggests that the bulk of star formation in massive galaxies occurs at early cosmic epochs and is largely complete by z ~ 1.5. Further mass assembly in these galaxies takes place with low specific SFRs.

Citations

• A high abundance of massive galaxies 3–6 billion years after the Big Bang
• STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE

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