Science Objectives and Early Results of the DEEP2 Redshift Survey

By M. Davis, S. Faber, J. Newman, A. Phillips, Richard S. Ellis, C. Steidel, Christopher J. Conselice, A. Coil, Douglas P. Finkbeiner, D. Koo and 11 more. SPIE Astronomical Telescopes + Instrumentation, 2002

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The DEIMOS spectrograph has now been installed on the Keck-II telescope and commissioning is nearly complete. The DEEP2 Redshift Survey, which will take approximately 120 nights at the Keck Observatory over a three year period and has been designed to utilize the power of DEIMOS, began in the summer of 2002. The multiplexing power and high efficiency of DEIMOS enables us to target 1000 faint galaxies per clear night. Our goal is to gather high-quality spectra of ≈ 60,000 galaxies with z>0.75 in order to study the properties and large scale clustering of galaxies at z ≈ 1. The survey will be executed at high spectral resolution, R=λ/Δλ ≈ 5000, allowing us to work between the bright OH sky emission lines and to infer linewidths for many of the target galaxies (for several thousand objects, we will obtain rotation curves as well). The linewidth data will facilitate the execution of the classical redshift-volume cosmological test, which can provide a precision measurement of the equation of state of the Universe. This talk reviews the project, summarizes our science goals and presents some early DEIMOS data.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, methodology): “Data taken with the DEep Imaging and Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) at the Keck observatory were processed with version 1.1.4 of spec2d, the pipeline developed for the DEEP2 galaxy redshift survey (Davis et al. 2003).”
The VIMOS Public Extragalactic Survey (VIPERS) - First Data Release of 57 204 spectroscopic measurements (2013, methodology): “…on 10 m class telescopes, significant clustering studies of the general galaxy population at z ∼ 1 became feasible as notably exploited by the VVDS (Le Fèvre et al. 2005) and the DEEP2 (Davis et al. 2003) surveys, followed by the zCOSMOS follow-up of the COSMOS HST field (Lilly et al. 2009).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, methodology): “%) project designed to study the galaxy population and large–scale structure at z ∼ 1 (Davis et al. 2003; Faber et al. 2006).”
Metallicities and Physical Conditions in Star-forming Galaxies at z ~ 1.0-1.5 (2008, methodology): “…Sample and Near-IR Spectroscopy The high-redshift galaxies presented in this paper are drawn from the DEEP2 Galaxy Redshift Survey (hereafter DEEP2; Davis et al. 2003; Faber et al. 2007), which contains> 30,000 galaxies with high-confidence redshifts at 0.7≤ z≤ 1.5 down to a limiting magnitude…”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “In the DEEP2 galaxy survey (Davis et al. 2003), just as the colour bimodality persists out to z ∼ 1 (Lin et al. 1999; Im et al. 2001; Bell et al. 2004; Willmer et al. 2006; Faber et al. 2007), the mean colour-density relation (Cooper et al. 2006) and the SSFR-density (Cooper et al. 2008) relation…”
CLUSTERING OF LOW-REDSHIFT (z ⩽ 2.2) QUASARS FROM THE SLOAN DIGITAL SKY SURVEY (2008, positive): “Coil et al. (2007) calculate the cross-correlation between ∼ 30 000 redshift 0.7 < z < 1.4 galaxies observed as part of the DEEP2 galaxy redshift survey (Davis et al. 2001, 2003), and quasars over the same redshift range.”
Number Counts at 3 μm < λ < 10 μm from the Spitzer Space Telescope (2004, background): “The DEEP2 survey (Davis et al. 2003) has produced complementary visible and nearinfrared data for this field.”
Photometric redshifts for the CFHTLS T0004 deep and wide fields (2008, methodology): “It includes theDEEP2 redshift survey (Davis et al. 2003 and Davis et al. 2007), the newVVDS “wide” sample (Garilli et al. 2008) and the “zCOSMOS” sample (Lilly et al. 2007).”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, background): “Luminous Blue Galaxies at 0.7 < z < 1.7: Studies from the second Deep Extragalactic Evolutionary Probe (DEEP2; Davis et al. 2003) reveal that the most luminous, star-forming blue galaxies at z ∼ 1 appear to be a population that evolves into massive red galaxies at lower redshifts (Cooper et al.…”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, methodology): “…we perform our correction using spectroscopic redshifts in the overlap with the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al. 2005; Garilli et al. 2008), the DEEP2 galaxy redshift survey (Davis et al. 2003, 2007; Newman et al. 2013) and the SDSS (Eisenstein et al. 2001; Strauss et al. 2002).”
Galaxies–intergalactic medium interaction calculation – I. Galaxy formation as a function of large-scale environment (2009, background): “Alongside studies of the evolution of cosmic gas, realistic modelling of the low-redshift evolution of galaxies is essential to connect the snapshots of cosmic evolution provided by galaxy surveys at different epochs, for example DEEP2 (Davis et al. 2003), VVDS (Le Fèvre et al. 2005) and COMBO-17 (”
THE NATURE OF LINER-LIKE EMISSION IN RED GALAXIES (2011, background): “In surveys of much more distant galaxies, such as most galaxies in SDSS, or surveys at high redshifts, such as DEEP2 (Davis et al. 2003), zCOSMOS (Lilly et al. 2007), BOSS (Eisenstein et al. 2011), and distant cluster surveys (e.g. Lubin et al. 2009), the spectra obtained usually covers a much…”
First Measurement of the Clustering Evolution of Photometrically Classified Quasars (2005, background): “In the distant universe (z ’ 1), the distribution of galaxies is less constrained, as it requires extensive investments of telescope time on 8 m class telescopes (e.g., DEEP2 [Deep Extragalactic Evolutionary Probe 2]; Davis et al. 2003).”
SIMULATION OF THE COSMIC EVOLUTION OF ATOMIC AND MOLECULAR HYDROGEN IN GALAXIES (2009, background): “While such large scale surveys are currently dominated by the optical and higher frequency bands [e.g. Spitzer (Fang et al. 2005), SDSS (Eisenstein et al. 2005), DEEP2 (Davis et al. 2003), 2dFGRS (Cole et al. 2005), GALEX (Milliard et al. 2007), Chandra (Gilli et al. 2003)], they may well be overtak”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, methodology): “On the Keck telescopes LRIS has enabled the first large survey of Lyman-Break Galaxies (Steidel et al. 1996), and has been followed by DEIMOS in 2002 used e.g. for the DEEP2 survey (Davis et al. 2003).”