Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth

By E. Daddi, Mark Dickinson, G. Morrison, R. Chary, A. Cimatti, D. Elbaz, D. Frayer, A. Renzini, Adrian Pope, D. M. Alexander and 5 more. 2007

1,245 citations recorded by the source corpus.

Examining a sample of massive galaxies at 1.4 < z < 2.5 with KVega < 22 from GOODS, we compare photometry from Spitzer at mid- and far-IR to submillimeter, radio, and rest-frame UV wavelengths, to test the agreement between different tracers of star formation rates (SFRs) and to explore the implications for galaxy assembly. For z ~ 2 galaxies with moderate luminosities (L8 μm < 1011 L☉), we find that the SFR can be estimated consistently from the multiwavelength data based on local luminosity correlations. However, 20%-30% of massive galaxies, and nearly all those with L8 μm > 1011 L☉, show a mid-IR excess that is likely due to the presence of obscured active nuclei, as shown in a companion paper. There is a tight and roughly linear correlation between stellar mass and SFR for 24 μm-detected galaxies. For a given mass, the SFR at z = 2 was larger by a factor of ~4 and ~30 relative to that in star-forming galaxies at z = 1 and 0, respectively. Typical ultraluminous infrared galaxies (ULIRGs) at z = 2 are relatively "transparent" to ultraviolet light, and their activity is long lived (≳400 Myr), unlike that in local ULIRGs and high-redshift submillimeter-selected galaxies. ULIRGs are the common mode of star formation in massive galaxies at z = 2, and the high duty cycle suggests that major mergers are not the dominant trigger for this activity. Current galaxy formation models underpredict the normalization of the mass-SFR correlation by about a factor of 4 and the space density of ULIRGs by an order of magnitude but give better agreement for z > 1.4 quiescent galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6a38b69473d16abe665578e5b04131f33e6eca58

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. Volker Springel
6. A. Dekel
7. D. M. Alexander
8. C. Conroy

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. A. Dekel
6. P. V. van Dokkum
7. C. Conroy
8. Volker Springel

Citations in the corpus

• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, background): “The amplitude of the MS reflects the evolution of the cosmic SFR density from the peak activity at z ∼ 1 − 2.5 to the “winding down” epochs at z < 1 (e.g. Noeske et al. 2007; Daddi et al. 2007a; Elbaz et al. 2007; Rodighiero et al. 2011; Whitaker et al. 2014).”
• STAR FORMATION AND DUST OBSCURATION AT z ≈ 2: GALAXIES AT THE DAWN OF DOWNSIZING (2009, methodology): “We extend the results of Daddi et al. (2007a) that UV light, appropriately corrected, is a reliably tracer of SFR atz∼ 2.”
• Vigorous Star Formation with Low Efficiency in Massive Disk Galaxies at z = 1.5 (2007, background): “…the Chary and Elbaz 2001 luminosity dependent templates) also agrees within this factor, while for BzK − 21000 the 24µm estimate of SFR is 2-2.5 larger than the radio and UV ones, mild evidence for possible mid-IR excess usually linked to obscured AGN activity (Daddi et al. 2007b; D07b hereafter).”
• Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, background): “Atz∼ 2 and atL24µm/(1+z) = 8× 1010 and 3.5× 1011 L⊙, Daddi et al. (2007b) find thatL70µm/(1+z) would be overestimated by a factor∼ 2 and∼ 10 using the CE01 library respectively, while we find a factor 2.3 and 12 respectively.”
• DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES (2008, background): “The high duty cycle of star formation in these objects (Daddi et al. 2007) would point in the same direction.”
• simba: Cosmological simulations with black hole growth and feedback (2019, background): “During Cosmic Noon, it has long been seen that cosmological models tend to underpredict the main sequence amplitude (Daddi et al. 2007; Davé 2008; Narayanan et al. 2012; Sparre et al. 2015; Somerville & Davé 2015), typically by a factor of 2− 3.”
• CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, positive): “The individual SFRs in star-forming galaxies correlate closely with their stellar masses in a narrow “star-forming main sequence” seen at z < 3 (Brinchmann et al. 2004; Noeske et al. 2007; Daddi et al. 2007b; Pérez-González et al. 2008).”
• 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): “Several other correlations between SFR and stellar mass have been published, including most recently by Reddy et al. (2006b) and Daddi et al. (2007).”
• A mature cluster with X-ray emission at z = 2.07 (2010, background): “On the other hand, the 24µm emission (which atz ∼ 2 corresponds to 8µm rest-frame) might be due to extremely obscured AGN activity (Fiore et al. 2009, Daddi et al. 2007b), an interpretation supported by the presence among the MIPS 24 µm sources of the Chandra-detected AGN.”
• The n ature of submillimetre galaxies in cosmological hydrodynamic simulations (2009, neutral): “As pointed out in Davé (2008), this would reconcile the observed values of αsf in BzK galaxies (Daddi et al. 2007) with the simulated αsf .”
• On the origin of the galaxy star‐formation‐rate sequence: evolution and scatter (2009, background): “…7.5∗ 0.67 10.0-11.3 Chabrier Noeske et al. (2007a) 1.0 0.80-1.20 6.80 0.90 9.3-11.1 Salpeter Elbaz et al. (2007) 1.9 1.4-2.5 23.77 0.90 9.5-11.1 Salpeter Daddi et al. (2007) 3.8 3.1-4.4 29.3 0.90 9.9-10.6 Chabrier Daddi et al. (2009) 3.96 3.67-4.25 14.3∗ 0.8∗ 8.8-10.3 Salpeter Stark et al. (2009)…”
• Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschel observations (2012, background): “The first reason is that, given their strong MIR emission (e.g. Daddi et al. 2007a; Fiore et al. 2008), AGN hosts are more represented in the 24µm prior list compared to inactive galaxies (for a given FIR host’s luminosity, they have a larger probability of being detected at 24µm).”
• Ionization state of inter-stellar medium in galaxies: evolution, SFR-M * -Z dependence, and ionizing photon escape (2013, background): “This tendency is consistent with the evolution of the star formation main sequence (e.g. Daddi et al. 2007).”
• GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, background): “…(SFR) and its stellar mass (M⋆) are tightly correlated and that the bulk of star forming galaxies follow a “main sequence” relation that evolves with redshift (e.g., Brinchmann et al. 2004; Noeske et al. 2007; Daddi et al. 2007; Elbaz et al. 2007, 2011; Rodighiero et al. 2011; Wuyts et al. 2011).”
• A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “Also shown is the original ‘main-sequence’ (MS) of star-forming galaxies at z ' 2 derived by Daddi et al. (2007) (SFR ∝ M0.”
• SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS (2009, background): “…evidence is growing that the majority of the high-z ULIRGs are fed by continuous gas accretion, and only about one third are gas-rich (“wet”) mergers (Daddi et al. 2007; Shapiro et al. 2008; Genzel et al. 2006, 2008; Förster Schreiber et al. 2006, 2009; Genel et al. 2008; Dekel & Birnboim 2008;…”
• AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, background): “…of the same stellar mass at the same redshift, implying that these intense starbursts have to be powered by extreme events such as major merger (Daddi et al. 2007; Engel et al. 2010; Hainline et al. 2011; Magnelli et al. 2012), while some cosmological simulations establish SMGs simply as the…”
• BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, background): “This relation has been dubbed the ’main sequence’ (MS) of starforming galaxies (Noeske et al. 2007; Elbaz et al. 2007; Daddi et al. 2007; Rodighiero et al. 2011).”