The Gemini Deep Deep Survey: I. Introduction to the Survey, Catalogs and Composite Spectra

By R. Abraham, Karl Glazebrook, P. McCarthy, D. Crampton, R. Murowinski, I. Jørgensen, K. Roth, I. Hook, S. Savaglio, Hsiao-Wen Chen and 2 more. 2004

225 citations recorded by the source corpus.

The Gemini Deep Deep Survey (GDDS) is an ultra-deep (K<20.6 mag, I<24.5 mag) redshift survey targeting galaxies in the"redshift desert"between 1<z<2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely-separated 30 arcmin^2 fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K vs. I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8<z<1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. Typical exposures times were 20-30 hours per field (in Nod&Shuffle mode), and the resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. The infrared selection underlying the survey means that the GDDS is observing not only star-forming galaxies, as in most high-redshift galaxy surveys, but also quiescent evolved galaxies. The median redshift of the whole GDDS sample is z=1.1. Together with the data and catalogs, we present a summary of the criteria for selecting the GDDS fields, the rationale behind our mask designs, an analysis of the completeness of the survey, and a description of the data reduction procedures used. All data from the GDDS are publicly available. (ABRIDGED)

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8559222f5c66629209802af81eb12cc0aecfd466

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The VIMOS VLT deep survey - First epoch VVDS-deep survey: 11 564 spectra with 17.5 $\leq$ I$_\textit{\textbf{\small AB}}$ $\leq$ 24, and the redshift distribution over 0 $\leq$ z $\leq$ 5 (2004, unknown): “…(Lilly et al. 1995a; Le Fèvre et al. 1995; Steidel et al. 1996; Steidel et al. 1998; Lilly et al. 1996; Madau et al. 1998; Cimatti et al. 2002; Abraham et al. 2004; Wolf et al. 2003) the samples remain too small, incomplete, affected by large and sometimes degenerate errors from photometric…”
First Measurement of the Clustering Evolution of Photometrically Classified Quasars (2005, background): “At even higher redshifts (z > 1:5), our knowledge of galaxies is limited by the redshifting of the bulk of their luminosity to infrared and submillimeter wavelengths (e.g., the Gemini Deep Deep survey [GDDS]; Abraham et al. 2004).”
A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, methodology): “The Gemini Deep Deep Survey (GDDS; Abraham et al. 2004) performed spectroscopy of galaxies selected toK < 20.6 (Vega).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, methodology): “One dimensional spectra were extracted using the iGDDS software (Abraham et al. 2004).”
IMACS: The Inamori-Magellan Areal Camera and Spectrograph on Magellan-Baade (2011, background): “Figure 8 shows a even deeper probe of field galaxies at z ∼ 1 from Patrick J. McCarthy, part of the Gemini Deep Deep Survey (Abraham et al. 2004).”
THE COSMOS-WIRCam NEAR-INFRARED IMAGING SURVEY. I. BzK-SELECTED PASSIVE AND STAR-FORMING GALAXY CANDIDATES AT z ≳ 1.4 (2009, background): “More recentK-selected surveys include the K20 survey (Cimatti et al. 2002) reachingKs ≃ 21.8 and the GDDS survey (Abraham et al. 2004) which reachedKs ≃ 22.4 provide further evidence for this picture.”
Evidence for Solar Metallicities in Massive Star-forming Galaxies at z ≳ 2 (2004, methodology): “In the SSA22a field, there are three spectroscopically confirmed GDDS galaxies with 1:6 z 2:0, and four with uncertain redshifts of 2:0 < z < 2:2 (Abraham et al. 2004).”
Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation (2007, methodology): “The sample consists of 11 Ks < 20 galaxies meeting the s-BzK color criterion of Daddi et al. (2004a), taken from the GOODS-S (Daddi et al. 2004b) and Deep 3a (Kong et al. 2006) fields, and 8 galaxies from the Gemini Deep Deep Survey (GDDS; Abraham et al. 2004) with Ks F 20:5 and I F 24:5.”
THE GEMINI CLUSTER ASTROPHYSICS SPECTROSCOPIC SURVEY (GCLASS): THE ROLE OF ENVIRONMENT AND SELF-REGULATION IN GALAXY EVOLUTION AT z ∼ 1 (2011, methodology): “As a test, we drew an additional field sample of galaxies in the same redshift range from the GDDS survey (Abraham et al. 2004).”
Ultraviolet to Mid-Infrared Observations of Star-forming Galaxies at z ~ 2: Stellar Masses and Stellar Populations (2005, background): “…rest-frame far–UV colors (Adelberger et al. 2004b; Steidel et al. 2004), their high luminosity in the observed K band (Daddi et al. 2004b), red rest-frame optical colors (van Dokkum et al. 2003; Franx et al. 2003), or some combination of the above (e.g., Abraham et al. 2004; Shapley et al. 2004).”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, background): “More recently, the K20 survey (Cimatti et al. 2002) reachingKs ≈ 21.8 and the GDDS survey (Abraham et al. 2004) reachingK ≈ 22.4 provided further observations to test the existing knowledge and understanding of the galaxy formation process.”
Cosmic chronometers: constraining the equation of state of dark energy. I: H(z) measurements (2009, unknown): “Additional spectra came from the Gemini Deep Deep Survey (GDDS; [24]), which had typical exposure times of 20 − 30 hours obtained in the highest quality conditions at Gemini Observatory.”
Cosmic Star Formation History and Its Dependence on Galaxy Stellar Mass (2004, unknown): “We take advantage of the near-IR selection of the Gemini Deep Deep Survey (GDDS, Abraham et al. 2004, hereafter Paper I) to study directly the evolutin of the SFRD as a function of stellar mass at the epoch of observation.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “…photometries in deep fields and follow-up spectroscopic observations, such as the K20 Survey (Cimatti et al. 2002b), GOODS (Giavalisco et al. 2004), and the Gemini DeepDeep Survey (GDDS;Abraham et al. 2004), it is now possible to identify a large number of bright galaxies at high redshifts.”
Calibrating Redshift Distributions beyond Spectroscopic Limits with Cross-Correlations (2008, methodology): “Despite integration times of more than thirty hours per object, the Gemini Deep Deep Survey (GDDS) only succeeded in measuring spectroscopic redshifts for ∼ 15% of their targets with 24 < I < 24.5, and < 50% of objects with 23 < I < 24 (Abraham et al. 2004).”
A Highly Complete Spectroscopic Survey of the GOODS-N Field (2008, background): “They also checked their criteria on two deeper samples, a spectroscopic sample to Ks,AB = 22.4 from the Gemini Deep Deep Survey (GDDS; Abraham et al. 2004) and a photometric sample to Ks,AB = 23.8 from ISAAC imaging of the same GOODS-S region covered by the K20 survey.”
THE HOST GALAXIES OF GAMMA-RAY BURSTS. II. A MASS–METALLICITY RELATION FOR LONG-DURATION GAMMA-RAY BURST HOST GALAXIES (2010, background): “Savaglio et al. (2005) found that this correlation extended to higher redshifts, based on observations of galaxies from the Gemini Deep Deep Survey (GDDS; Abraham et al. 2004) at 0.4 < z < 1.”