A Spectroscopic Survey of Redshift 1.4 ≲ z ≲ 3.0 Galaxies in the GOODS-North Field: Survey Description, Catalogs, and Properties

By Naveen A. Reddy, C. Steidel, D. Erb, A. Shapley, M. Pettini. 2006

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We present the results of a spectroscopic survey with LRIS-B on Keck of more than 280 star-forming galaxies and AGNs at redshifts 1.4 ≲ z ≲ 3.0 in the GOODS-N field. Candidates are selected by their UnGℛ colors using the ``BM/BX'' criteria to target redshift 1.4 ≲ z ≲ 2.5 galaxies and the LBG criteria to target redshift z ~ 3 galaxies; combined these samples account for ~25%-30% of the ℛ and Ks band counts to ℛ = 25.5 and Ks(AB) = 24.4, respectively. The 212 BM/BX galaxies and 74 LBGs constitute the largest spectroscopic sample of galaxies at z > 1.4 in GOODS-N. Extensive multiwavelength data allow us to investigate the stellar populations, stellar masses, bolometric luminosities (Lbol), and extinction of z ~ 2 galaxies. Deep Chandra and Spitzer data indicate that the sample includes galaxies with a wide range in Lbol (≃1010 to >1012 L☉) and 4 orders of magnitude in dust obscuration (Lbol/LUV). The sample includes galaxies with a large dynamic range in evolutionary state, from very young galaxies (ages ≃50 Myr) with small stellar masses (M* ≃ 109 M☉) to evolved galaxies with stellar masses comparable to the most massive galaxies at these redshifts (M* > 1011 M☉). Spitzer data indicate that the optical sample includes some fraction of the obscured AGN population at high redshifts: at least 3 of 11 AGNs in the z > 1.4 sample are undetected in the deep X-ray data but exhibit power-law SEDs longward of ~2 μm (rest frame) indicative of obscured AGNs. The results of our survey indicate that rest-frame UV selection and spectroscopy presently constitute the most timewise efficient method of culling large samples of high-redshift galaxies with a wide range in intrinsic properties, and the data presented here will add significantly to the multiwavelength legacy of GOODS.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/784d4052b30d460e1200e772b2f57825f4843b5f

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TOWARD THE STANDARD POPULATION SYNTHESIS MODEL OF THE X-RAY BACKGROUND: EVOLUTION OF X-RAY LUMINOSITY AND ABSORPTION FUNCTIONS OF ACTIVE GALACTIC NUCLEI INCLUDING COMPTON-THICK POPULATIONS (2014, methodology): “We basically refer to the redshift catalog provided by Trouille et al. (2008), which contains the results from previous works including Barger et al. (2003), Swinbank et al. (2004), Chapman et al. (2005), and Reddy et al. (2006).”
Photometric redshifts in the SWIRE Survey (2008, methodology): “Because the depth of our optical surveys is typically r ∼ 23.5-25, we do not sample the low-mass end of the galaxy distribution at these redshifts as well as Reddy et al (2006).”
EDDINGTON-LIMITED ACCRETION AND THE BLACK HOLE MASS FUNCTION AT REDSHIFT 6 (2010, background): “At z ∼ 2 − 3, about 3–5% of Lyman break galaxies contain evidence for weak AGN (Steidel et al. 2002; Reddy et al. 2006).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “Furthermore, the field has been the subject of numerous spectroscopic surveys (e.g. Steidel et al. 2003; Wirth et al. 2004; Treu et al. 2005; Strolger et al. 2005; Reddy et al. 2006; Barger et al. 2008; Yoshikawa et al. 2010; Daddi et al. 2010; Cooper et al. 2011).”
UV-CONTINUUM SLOPES AT z ∼ 4–7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR–MAGNITUDE RELATIONSHIP FOR z ⩾ 4 STAR-FORMING GALAXIES (2011, methodology): “…some change in the dust composition of galaxies as a result of the fact that dust from SNe would be expected to form much earlier in the lifetime of a galaxy than dust from AGB stars (e.g., Maiolino et al. 2004; Maiolino 2006; Reddy et al. 2006b; Gallerani et al. 2010; Finkelstein et al. 2012).”
PHYSICAL CONDITIONS IN A YOUNG, UNREDDENED, LOW-METALLICITY GALAXY AT HIGH REDSHIFT (2010, methodology): “From the G − R color, we find a UV continuum slope β = −2.1, placing BX418 at the extreme blue end of the β distribution of luminous z ∼ 2 galaxies (Reddy et al. 2006b, 2010).”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “Finally, the thin dotted-dashed line shows the relation used in Reddy et al. (2006a).”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, unknown): “The Cosmic Evolution of ULIRGs As already shown by D05b (see also Papovich et al. 2006; Reddy et al. 2006a; Caputi et al. 2007), the typical massive (M k 1011 M yr 1) star-forming galaxy at z ¼ 2 is a ULIRG, i.e., it appears to have LIR 1012 L or more.”
The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, background): “Various studies have derived stellar masses, M∗, for highredshift galaxies by modeling the rest-frame UV-to-near-IR data (e.g., Shapley et al. 2005; Papovich et al. 2005, 2006; Reddy et al. 2006; Stark et al. 2009; Finkelstein et al. 2010; Labbé et al. 2010a).”
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, methodology): “…suppressing star formation in high mass halos (Croton et al. 2006; Scannapieco et al. 2005; Granato et al. 2004), even after taking into account the saturation of UV light with respect to the total star formation rates of galaxies with large SFRs (Adelberger & Steidel 2000; Reddy et al. 2006b).”
ON THE STELLAR POPULATIONS AND EVOLUTION OF STAR-FORMING GALAXIES AT 6.3 < z ⩽ 8.6 (2009, methodology): “Figure 12 compares our observations to a number of studies from the literature, from 2≤ z ≤ 7 (Shapley et al. 2005; Reddy et al. 2006; Stark et al. 2009, all of which assumed a Salpeter IMF), and shows the evolution of the mass of an L∗ galaxy with redshift.”
THE GREATER IMPACT OF MERGERS ON THE GROWTH OF MASSIVE GALAXIES: IMPLICATIONS FOR MASS ASSEMBLY AND EVOLUTION SINCE z ≃ 1 (2009, background): “…redshifts13 initiated by the survey work in Cowie et al. (2004), as well as the 1.4 < z < 3.0 11 http://archive.stsci.edu/prepds/goods/ 12 http://tkserver.keck.hawaii.edu/tksurvey/ 13 http://www.ifa.hawaii.edu/ cowie/hhdf/acs.html spectroscopic survey undertaken by Reddy et al. (2006).”
THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H-SELECTED GALAXIES AT 1.37 ≤ z ≤ 3.8 ?> (2014, background): “Additional spectroscopic redshifts are included as well (Reddy et al. 2006; Barger et al. 2008; Coil et al. 2009, 2011; Cooper et al. 2012; Newman et al. 2013; van de Sande et al. 2013).”
GOODS-HERSCHEL MEASUREMENTS OF THE DUST ATTENUATION OF TYPICAL STAR-FORMING GALAXIES AT HIGH REDSHIFT: OBSERVATIONS OF ULTRAVIOLET-SELECTED GALAXIES AT z ∼ 2 (2011, methodology): “…other investigations targeting moderately luminous galaxies and using a variety of star formation tracers at z ∼ 2 (e.g., Reddy & Steidel 2004; Reddy et al. 2006b, 2010; Daddi et al. 2007; Pannella et al. 2009) and z ∼ 3 (e.g., Seibert et al. 2002; Nandra et al. 2002; Magdis et al. 2010a,b).”
The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “We use spectroscopic redshifts coming from a combination of various studies (Cohen et al. 2000; Wirth et al. 2004; Cowie et al. 2004; Le Fèvre et al. 2004; Mignoli et al. 2005; Vanzella et al. 2006; Reddy et al. 2006; Barger et al. 2008; Cimatti et al. 2008; Lilly et al. 2009).”
LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION (2009, unknown): “…(2006), Yoshida et al. (2006), Iye et al. (2006), Nagao et al. (2007), Hayashi et al. (2009), and Ly et al. (2009) for SDF, and Wirth et al. (2004), Reddy et al. (2006), Barger et al. (2008), Cohen et al. (2000); Cohen (2001), Steidel et al. (1996, 1999, 2003), Phillips et al. (1997), Lowenthal et…”
THE KILOPARSEC-SCALE KINEMATICS OF HIGH-REDSHIFT STAR-FORMING GALAXIES (2009, methodology): “Despite our growing knowledge of the broad global characteristics of high redshift galaxies (e.g., Erb et al. 2006c; Reddy et al. 2006a; Papovich et al. 2006; Cowie et al. 2008; and references therein), our understanding of their internal structure and dynamical evolution has been limited by their…”
A Highly Complete Spectroscopic Survey of the GOODS-N Field (2008, background): “Most of the redshifts are at z < 1.6 (2362 sources) where the [OII] 3727 Å line still lies in the DEIMOS spectroscopic range, 327 lie between z = 1.6−3.5, mostly from the LRIS observations of Reddy et al. (2006), and there are relatively few objects (only 21) with spectroscopic redshifts z > 3.5.”