Near-Infrared Bright Galaxies at z ≃ 2. Entering the Spheroid Formation Epoch?

By E. Daddi, A. Cimatti, A. Renzini, J. Vernet, Christopher J. Conselice, L. Pozzetti, M. Mignoli, P. Tozzi, T. Broadhurst, S. di Serego Alighieri and 4 more. 2003

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Spectroscopic redshifts have been measured for nine K-band luminous galaxies at 1.7 < z < 2.3, selected with Ks < 20 in the K20 survey region of the Great Observatories Origins Deep Survey (GOODS) area. Star formation rates (SFRs) of ~100-500 M☉ yr-1 are derived when dust extinction is taken into account. The fitting of their multicolor spectral energy distributions indicates stellar masses of M ≳ 1011 M☉ for most of the galaxies. Their rest-frame UV morphology is highly irregular, suggesting that merging-driven starbursts are going on in these galaxies. Morphologies tend to be more compact in the near-IR, a hint for the possible presence of older stellar populations. Such galaxies are strongly clustered, with seven out of nine belonging to redshift spikes, which indicates a correlation length of r0 ~ 9-17 h-1 Mpc (1 σ range). Current semianalytical models of galaxy formation appear to underpredict by a large factor (≳30) the number density of such a population of massive and powerful starburst galaxies at z ~ 2. The high masses and SFRs, together with the strong clustering, suggest that at z ~ 2 we may have started to explore the major formation epoch of massive early-type galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

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The Multiwavelength Survey by Yale-Chile (MUSYC): Survey Design and Deep Public UBVRIz' Images and Catalogs of the Extended Hubble Deep Field-South (2005, background): “It has recently become clear that optical selection methods do not provide a full census of the galaxy population at z∼ 3, as they miss objects which are faint in the rest-frame ultraviolet (Franx et al. 2003; Daddi et al. 2004).”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, background): “…density of massive galaxies takes place in the cosmic time interval between z 3 and 1 (e.g., Dickinson et al. 2003; Rudnick et al. 2003, 2006; Fontana et al. 2004, 2006; Daddi et al. 2004a, hereafter D04a; van Dokkum et al. 2006; Franceschini et al. 2006; Pozzetti et al. 2007; Arnouts et al. 2007).”
THE SINS/zC-SINF SURVEY of z ∼ 2 GALAXY KINEMATICS: OUTFLOW PROPERTIES (2012, methodology): “They were selected either from their UnGR colors satisfying the ‘BX’ criteria (Steidel et al. 2004; Adelberger et al. 2004; Erb et al. 2006; Law et al. 2009) or based on K band imaging via the ‘BzK’ criterion for 1.4 <z <2.5 SFGs (Daddi et al. 2004).”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, background): “In this sequence, giant elliptical galaxies assembled at z 0:8Y2 from smaller progenitors whose stars formed at z 1:5Y5 (vanDokkum et al. 2003; Daddi et al. 2004a, 2005; Fontana et al. 2004; Stanford et al. 2004; Bundy et al. 2005; Labbé et al. 2005; Saracco et al. 2005; Longhetti et al. 2005;…”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, background): “Recently various groups have discovered massive galaxies at redshifts z > 1, which has been seen as potentially a problem for CDM based models (Franx et al. 2003; Daddi et al. 2004; Somerville et al. 2004; Glazebrook et al. 2004; cf. Nagamine et al. 2005).”
From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, methodology): “These selection criteria sample fairly luminous (L 1011Y1012:5 L ) galaxies with star formation rates of 10Y300 M yr 1, with a range of ages 10 Myr-3 Gyr and stellar masses M 109Y1011:5 M (Shapley et al. 2005; Förster Schreiber et al. 2004; Erb et al. 2006b, 2006c; Daddi et al. 2004a, 2004b).”
An interferometric CO survey of luminous submillimetre galaxies (2005, result): “Our estimate of the abundances of massive galaxies atz ∼ 2.8 is in good agreement with independent measurements at similar redshifts (Daddi et al. 2004; Saracco et al. 2004), and confirms the slow decline in the space density of massive galaxies as a function of redshift (Genzel et al. 2003;…”
Multiwavelength Study of Massive Galaxies at z ~ 2. II. Widespread Compton-thick Active Galactic Nuclei and the Concurrent Growth of Black Holes and Bulges (2007, methodology): “Stellar masses for our sample are estimated from the empirically calibrated relations presented in Daddi et al. (2004b), as discussed in Paper I, based on the observed photometry in theB-, z- andK- bands.”
Evolved Galaxies at z > 1.5 from the Gemini Deep Deep Survey: The Formation Epoch of Massive Stellar Systems (2004, background): “Similarly, the massiveK-bright galaxies at from the Great Obser-z ∼ 2 vatories Origins Deep Survey and K20 survey (Daddi et al. 2004) have high inferred star formation rates.”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, background): “Thus, spiral galaxies (and increasingly irregular galaxies at higher redshift; e.g., Cross et al. 2004; Daddi et al. 2004; Somerville et al. 2004b) dominate the SFR density at zP2, even assuming the most optimistic fgas ¼1:0 pure gaseous mergers, with the contribution from mergers rising to a…”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “K (sBzK; Daddi et al. 2004a (D04)) selection – and a bluer selection criteria in general – is biased towards more “active” SFGs (i.e. with higher (s)SFRs), excluding good portions of galaxies that are classified as SFGs via other selection mechanisms (NUV−r vs. r−J ; NUVrJ), and give steeper MS…”
Spectroscopic Identification of a Protocluster at z = 2.300: Environmental Dependence of Galaxy Properties at High Redshift (2005, background): “Obviously, such samples depend on galaxies having enough current (relatively unobscured) star formation to be identified as a candidate for spectroscopy, which will produce a bias against both passively evolving z > 2 galaxies and galaxies that are heavily reddened by dust (cf. Daddi et al. 2004).”
The K20 survey. VII. The spectroscopic catalogue: spectral properties and evolution of the galaxy population ⋆, ⋆⋆ (2005, methodology): “…technique for a joint selection of 2 For five galaxies the redshift has been obtained from ESO/GOODS data. star-forming and passive galaxies at z > 1.4 (Daddi et al. 2004b), and the study of the rest-frame B-band morphology as a function of redshift based on HST/ACS imaging of the CDFS field…”
The K20 survey. VI. The distribution of the stellar masses in galaxies up to z 2 (2004, methodology): “Second, we have found that the estimated star– formation rates obtained adopting a Calzetti law are consistent with the X–ray and radio luminosities of these objects (Daddi et al 2004b), suggesting that we are not missing a significant fraction of their star–formation activity.”
A Census of Optical and Near-Infrared Selected Star-forming and Passively Evolving Galaxies at Redshift z ~ 2 (2005, methodology): “Daddi et al. (2004a) show that the reddening vector is essentially parallel to the BzK limit defined by Equation 4, implying that BzK selection should be sensitive to galaxies with higher extinction (and presumably higher star formation rates) than found among BX/BM selected galaxies (i.e., E(B − V…”
The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, methodology): “The SINS BX/BM targets were more specifically taken from the near-IR longslit spectroscopic follow-up with NIRSPEC at the Keck II telescope of Erb et al. (2006b) and the SINS K20 objects comprised all five z > 2 sources discussed by Daddi et al. (2004).”
Lightcone mock catalogues from semi-analytic models of galaxy formation – I. Construction and application to the BzK colour selection (2012, methodology): “A popular photometric technique, designed to simultaneously identify populations of star-forming and passively evolving galaxies, is the BzK colour-criterion (Daddi et al. 2004a).”
The Assembly of Diversity in the Morphologies and Stellar Populations of High-Redshift Galaxies (2005, background): “The observed morphologies of galaxies at zk 2 are generally highly irregular or centrally compact (Giavalisco et al. 1996; Lowenthal et al. 1997; Dickinson 2000; Daddi et al. 2004), but some large disk-galaxy candidates exist (e.g., Labbé et al. 2003; Conselice et al. 2004).”
Vigorous Star Formation with Low Efficiency in Massive Disk Galaxies at z = 1.5 (2007, methodology): “Stellar masses of 0.5–0.8×1011M⊙ were derived from optical and UV rest frame photometry, following the method of Daddi et al. (2004b).”
The VIMOS VLT deep survey: the assembly history of the stellar mass in galaxies: from the young to the old universe (2007, unknown): “This population shows extremely red colours (MI − MK 0.8) and could be related to the appearance of the population of massive star forming dusty galaxies observed in previous surveys (Fontana et al. 2004; Daddi et al. 2004b).”