Spitzer Observations of Massive, Red Galaxies at High Redshift

By C. Papovich, L. A. Moustakas, Mark Dickinson, É. Le Floc'h, G. Rieke, E. Daddi, D. M. Alexander, F. E. Bauer, W. N. Brandt, T. Dahlén and 23 more. 2005

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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 Ks-selected galaxies in the ≃130 arcmin2 GOODS-S field, we identify 153 distant red galaxies (DRGs) with (J - Ks)Vega ≥ 2.3. This sample is approximately complete in stellar mass for passively evolving galaxies above 1011 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 zmed ~ 2.5), and the others are galaxies whose light is dominated by heavily reddened (A1600 ≳ 4-6 mag) starbursts (at zmed ~ 1.7). Very few DRGs (≲10%) have no indication of current star formation. DRGs at z ~ 1.5-3 with stellar masses ≥1011 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 ≥ 1011 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 ≥ 1011 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.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

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Citations in the corpus

MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, unknown): “2007b,a; Papovich et al. 2006; Martin et al. 2007; Bell et al. 2005; Damen et al. 2009).”
EMU: Evolutionary Map of the Universe (2011, background): “There is now evidence that star formation depends both on galaxy stellar mass (Feulner et al. 2005; Juneau et al. 2005; Papovich et al. 2006; Mobasher et al. 2009, see Figure.”
A STEEP FAINT-END SLOPE OF THE UV LUMINOSITY FUNCTION AT z ∼ 2–3: IMPLICATIONS FOR THE GLOBAL STELLAR MASS DENSITY AND STAR FORMATION IN LOW-MASS HALOS (2008, background): “Including ULIRGs — those galaxies whose UV slopes tend to under-predict their bolometric luminosities (e.g., Papovich et al. 2006, 2007; Reddy et al. 2006b) — does not change the fact that a large portion of the bolometric luminosity density arises from faint galaxies, either those that are fainter…”
Deep Spitzer 24 μm COSMOS Imaging. I. The Evolution of Luminous Dusty Galaxies—Confronting the Models (2009, background): “…tremendous progress in our understanding of the bolometric properties of distant sources (e.g., Huang et al. 2005; Yan et al. 2005; Daddi et al. 2005; Papovich et al. 2006; Webb et al. 2006; Reddy et al. 2006; Menéndez-Delmestre et al. 2007; Sajina et al. 2007; Lutz et al. 2008; Pope et al. 2008).”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, methodology): “Comparing the specific star formation rate distributions as a function of stellar mass, age, and redshift from our simulations and observed in Bauer et al. (2005), Feulner et al. (2005), Pérez-González et al. (2005), and Papovich et al. (2006) yields a similar self-consistent ‘‘downsizing.’’”
THE EVOLUTIONARY HISTORY OF LYMAN BREAK GALAXIES BETWEEN REDSHIFT 4 AND 6: OBSERVING SUCCESSIVE GENERATIONS OF MASSIVE GALAXIES IN FORMATION (2009, background): “The addition of Spitzer photometry (e.g., Labbé et al. 2005; Webb et al. 2006; Papovich et al. 2006; Reddy et al. 2006) and very deep spectra (van Dokkum et al. 2004; Kriek et al. 2006) has enabled the passively evolving subset of DRGs to be separated from the dusty subset, providing more robust…”
The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift (2011, background): “…stellar populations and remarkably small sizes relative to their local counterparts (e.g. Daddi et al. 2005; Labbé et al. 2005; Kriek et al. 2006; Papovich et al. 2006; Trujillo et al. 2006, 2007; Zirm et al. 2007; van Dokkum et al. 2008; Damjanov et al. 2009, 2011; Toft et al. 2009; Taylor…”
Cosmic X-ray surveys of distant active galaxies (2015, background): “…from the initial studies, the majority of the distant X-ray AGNs were found to be hosted by massive galaxies (> 3 × 1010 M ; e.g., Akiyama 2005; Papovich et al 2006; Alonso-Herrero et al 2008; Bundy et al 2008; Brusa et al 2009b; Xue et al 2010; Mainieri et al 2011; Lusso et al 2011), with…”
Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging (2008, methodology): “These galaxies consist of Distant Red Galaxies from Papovich et al. (2006), IEROs from Yan et al. (2004), and BzK galaxies from Daddi et al. (2007).”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, background): “…(we obtain <z>=2.4±0.9 just in this field) published by Reddy et al. (2005), the median and rms photometric values z=2.6±0.7 published by Franx et al. (2003), the median photometric redshift z=2.2 from Papovich et al. (2006), and the median photometric redshift z∼2.5 from Quadri et al. (2007).”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “…at the 5− 10µJy level at all redshifts (indicating SF/AGN activity a factor of> 10 lower than typical star-forming galaxies at that redshift; see also Papovich et al. 2006 for an early discussion of star formation in red-selectd galaxies; these measurements are not shown as they fall off of…”
The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission (2006, background): “The typical source in deep MIPS 24µm surveys has total infrared luminosity LTIR & 10 11L⊙ (Papovich et al. 2006; Yan et al. 2004), and may therefore exibit a much different contribution of PAH emission in the 8µm rest frame compared to star-forming galaxies of lower luminosity.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “As early as z ≈ 3, star formation begins to shut down rapidly in massive galaxies (e.g., Juneau et al. 2005; Papovich et al. 2006), leading to the formation of a quenched “red sequence” that grows with time (Bell et al. 2004; Faber et al. 2007; Brown et al. 2007).”
UV Star Formation Rates in the Local Universe (2007, background): “While most current studies observe an overall shift towards higher specific SFRs, the slope does not appear to change much (e.g., Noeske et al. 2007; Papovich et al. 2006).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “Furthermore, studies show that a high fraction of massive galaxies atz > 2 have high levels of star formation (e.g., Kriek et al. 2006; Papovich et al. 2006), and these are likely consistent with the evolution of the cluster galaxies.”
EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…with previous findings in the literature, although statistical uncertainties are obviously large (e.g., Kauffmann et al. 2003b; Reddy et al. 2005; Papovich et al. 2006; Daddi et al. 2007; Brusa et al. 2009; Xue et al. 2010; Hainline et al. 2012; Bongiorno et al. 2012; Rosario et al. 2013a).”
Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies (2018, background): “…based on a single color (such as color-magnitude diagrams) were very suc- Article number, page 2 of 41 cessful in the local Universe, but suffer from high contamination at higher redshifts owing to the increasing prevalence of dusty red galaxies (e.g., Labbé et al. 2005; Papovich et al. 2006).”
Kinemetry of SINS High-Redshift Star-Forming Galaxies: Distinguishing Rotating Disks from Major Mergers (2008, background): “…103 M yr 1 in submillimeter-selected galaxies (SMGs; e.g., Blain et al. 2002; Smail et al. 2002; Tacconi et al. 2006), and correspondingly large variations in morphology, stellar populations, excitation properties, and dust content (e.g., Reddy et al. 2005; Papovich et al. 2006; Kriek et al. 2007).”
THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4 (2015, background): “Furthermore, the ratio of IR to UV flux (infrared excess: IRX ≡ LIR/LUV) is strongly correlated with mass (e.g. Papovich et al. 2006; Whitaker et al. 2014), therefore, the completeness in ΨUV+IR will also be a function of stellar mass.”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, background): “Subpopulations of dusty, IR-luminous galaxies at low and high redshift are known to deviate from the original starburst relation with a higher IRX for a given slope β (Goldader et al., 2002; Chapman et al., 2005; Howell et al., 2010; Papovich et al., 2006).”