A Census of Optical and Near-Infrared Selected Star-forming and Passively Evolving Galaxies at Redshift z ~ 2

By Naveen A. Reddy, D. Erb, C. Steidel, A. Shapley, K. Adelberger, M. Pettini. 2005

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Using the extensive multiwavelength data in the GOODS-North field, including our ground-based rest-frame UV spectroscopy and near-IR imaging, we construct and draw comparisons between samples of optical and near-IR selected star-forming and passively evolving galaxies at redshifts 1.4 ≲ z ≲ 2.6. We find overlap at the 70%-80% level in samples of z ~ 2 star-forming galaxies selected by their optical (UnGℛ) and near-IR (BzK) colors when subjected to common K-band limits. Deep Chandra data indicate a ~25% AGN fraction among near-IR selected objects, much of which occurs among near-IR bright objects (Ks < 20; Vega). Using X-rays as a proxy for the bolometric star formation rate (SFR) and stacking the X-ray emission for the remaining (non-AGN) galaxies, we find that the SFR distributions of UnGℛ, BzK, and J - Ks > 2.3 galaxies (i.e., distant red galaxies; DRGs) are very similar as a function of Ks, with Ks < 20 galaxies having ⟨SFR⟩ ~ 120 M☉ yr-1, a factor of 2-3 higher than those with Ks > 20.5. The absence of X-ray emission from the reddest DRGs and BzK galaxies with (z - K)AB ≳ 3 indicates that they must have declining star formation histories to explain their red colors and low SFRs. While the M/L ratio of passively evolving galaxies may be larger on average, the Spitzer IRAC data indicate that their inferred stellar masses do not exceed the range spanned by optically selected galaxies, suggesting that the disparity in current SFR may not indicate a fundamental difference between optical and near-IR selected massive galaxies (M* > 1011 M☉). We consider the contribution of optical, near-IR, and submillimeter selected galaxies to the star formation rate density (SFRD) at z ~ 2, taking into account sample overlap. The SFRD in the interval 1.4 ≲ z ≲ 2.6 of UnGℛ and BzK galaxies to Ks = 22 and DRGs to Ks = 21 is ~0.10 ± 0.02 M☉ yr-1 Mpc-3. Optically selected galaxies to ℛ = 25.5 and Ks = 22.0 account for ~70% of this total. Greater than 80% of radio-selected submillimeter galaxies to S850 μm ~ 4 mJy with redshifts 1.4 < z < 2.6 satisfy either one or more of the BX/BM, BzK, and DRG criteria.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e09c6797ea624eb2ced87399ecc93a8d7662be5f

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Citations in the corpus

A study of the gas–star formation relation over cosmic time (2010, methodology): “…uncertainties and given the intrinsic scatter of the z ∼ 2 ‘main sequence’, the ‘BX’ sample provides a fair census of the highmass end of the entire UV/optically selected SFG population in this redshift and mass range (Reddy et al. 2005; Erb et al. 2006b; Förster Schreiber et al. 2009).”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “Then there appears to be a sharp drop of passive BzKs beyond z = 2, which in part may be due to the available B-band data being not deep enough (Reddy et al. 2005) Further candidate ETGs with masses up to a few 1011M⊙ have been identified at even higher redshifts, such as six objects within the…”
The Mass-Metallicity Relation at z≳2 (2006, background): “Specifically, Reddy et al. (2005) find that only 3% of UV-selected galaxies at z ∼ 2 have X-ray detections in the ultra-deep 2Ms Chandra Deep Field North.”
UV Luminosity Functions at z~4, 5, and 6 from the Hubble Ultra Deep Field and Other Deep Hubble Space Telescope ACS Fields: Evolution and Star Formation History (2007, background): “We refer our readers to Franx et al. (2003), Reddy et al. (2005), and van Dokkum et al. (2006) for an excellent discussion of these issues at slightly lower redshifts (z ∼ 2 − 3).”
THE STRUCTURE AND KINEMATICS OF THE CIRCUMGALACTIC MEDIUM FROM FAR-ULTRAVIOLET SPECTRA OF z ≃ 2–3 GALAXIES (2010, background): “…particular objects in the present sample, drawn from a spectroscopic survey of “BX” UV-color-selected galaxies, have been well-characterized in terms of their spatial clustering (Adelberger et al. 2005b) and stellar population parameters (Erb et al. 2006c; Shapley et al. 2005; Reddy et al. 2005).”
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): “This has been shown to be valid for moderately luminous galaxies (i.e., LIRGs; Reddy et al. 2005, 2006b).”
THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, background): “These represent the bulk of the cosmic star formation activity and stellar mass density at these redshifts (Reddy et al. 2005; Rudnick et al. 2006; Grazian et al. 2007, Caputi et al. 2007).”
A Spectroscopic Survey of Redshift 1.4 ≲ z ≲ 3.0 Galaxies in the GOODS-North Field: Survey Description, Catalogs, and Properties (2006, methodology): “…allows us to very efficiently follow up galaxies spanning over 2 orders of magnitude in age and stellar mass at redshifts z k 1:4, other techniques are required to assess the total stellar mass budget at these redshifts (e.g., Rudnick et al. 2006; van Dokkum et al. 2006; Reddy et al. 2005).”
Submillimeter Galaxies at z ~ 2: Evidence for Major Mergers and Constraints on Lifetimes, IMF, and CO-H2 Conversion Factor (2008, background): “Significant progress has been made in elucidating the physical properties of high-z star-forming galaxies, as well as the relations of different populations to each other (e.g., Reddy et al. 2005; Grazian et al. 2007; Bouché et al. 2007).”
The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, result): “…in AGN fraction with higher galaxy mass is however fully consistent with the trends observed from much larger multiwavelength and spectroscopic surveys at z ∼ 2 (e.g., Reddy et al. 2005; Daddi et al. 2007; Brusa et al. 2009; Hainline et al. 2012; Bongiorno et al. 2012; Mancini et al. 2015).”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, methodology): “Several recent surveys have used the 24 m emission in 1 < z < 3 galaxies in order to estimate their ongoing SFRs and related quantities (e.g., Pérez-González et al. 2005; Reddy et al. 2005; D05b, Papovich et al. 2006; Caputi et al. 2006a, 2006b).”
The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, background): “For the latter case, Reddy et al. (2005) found that the cosmic SFR has a relatively minor contribution from such severely extincted systems that escape BzK/Lyman Break Galaxy selection at z ∼ 2, so they are not likely to be the dominant growth mode for galaxies.”
Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation (2007, unknown): “The BX/BM and s-BzK criteria select largely overlapping populations (at least down to Ks < 20), in excellent agreement with Reddy et al. (2005) and Grazian et al. (2007).”
The first appearance of the red sequence of galaxies in proto-clusters at 2 <~ z <~ 3 (2007, background): “The galaxies that satisfy this criterion were named Distant Red Galaxies (DRGs) and they have been shown to correspond to 2 < z < 3 galaxies with a high completeness rate when followed up spectroscopically (e.g., van Dokkum et al. 2003, Förster Schreiber et al. 2004, Reddy et al. 2005).”
EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…in good agreement 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…”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, background): “Still, Reddy et al. (2005) noted a 70%Y80% overlap in the identification of star-forming galaxies selected by visible and near-IR surveys at z 2, so our ACS survey should not miss a high fraction of the high-tb luminous galaxies at that redshift.”
PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z ∼ 1–3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES (2012, background): “…masses and star formation rates considered here, the BX/MD sample provides a reasonably fair census of the entire UV-/optically selected SFG population in this red-shift and mass range (Daddi et al. 2007, Reddy et al. 2005), although the UV-selection is naturally biased against dusty galaxies.”