The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data

By A. Coil, M. Davis, D. Madgwick, J. Newman, C. Conselice, M. C. Cooper, R. Ellis, S. Faber, Douglas P. Finkbeiner, P. Guhathakurta and 7 more. 2003

143 citations recorded by the source corpus.

We measure the two-point correlation function ξ(rp, π) in a sample of 2219 galaxies between z = 0.7 and 1.35 to a magnitude limit of RAB = 24.1 from the first season of the DEEP2 Galaxy Redshift Survey. From ξ(rp, π) we recover the real-space correlation function, ξ(r), which we find can be approximated within the errors by a power law, ξ(r) = (r/r0)-γ, on scales ~0.1-10 h-1 Mpc. In a sample with an effective redshift of zeff = 0.82, for a ΛCDM cosmology we find r0 = 3.53 ± 0.81 h-1 Mpc (comoving) and γ = 1.66 ± 0.12, while in a higher redshift sample with zeff = 1.14 we find r0 = 3.12 ± 0.72 h-1 Mpc and γ = 1.66 ± 0.12. These errors are estimated from mock galaxy catalogs and are dominated by the cosmic variance present in the current data sample. We find that red, absorption-dominated, passively evolving galaxies have a larger clustering scale length, r0, than blue, emission-line, actively star-forming galaxies. Intrinsically brighter galaxies also cluster more strongly than fainter galaxies at z ≃ 1. Our results imply that the DEEP2 galaxies have an effective bias b = 0.96 ± 0.13 if σ8DM = 1 today or b = 1.19 ± 0.16 if σ8DM = 0.8 today. This bias is lower than that predicted by semianalytic simulations at z ≃ 1, which may be the result of our R-band target selection. We discuss possible evolutionary effects within our survey volume, and we compare our results with galaxy-clustering studies at other redshifts, noting that our star-forming sample at z ≃ 1 has selection criteria very similar to the Lyman break galaxies at z ≃ 3 and that our red, absorption-line sample displays a clustering strength comparable to the expected clustering of the Lyman break galaxy descendants at z ≃ 1. Our results demonstrate that galaxy-clustering properties as a function of color, spectral type, and luminosity seen in the local universe were largely in place by z ≃ 1.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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Citations in the corpus

Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, methodology): “…redshifts and their error distributions determined using a sample of galaxies in the Groth strip with redshifts from DEEP2 (Davis et al. 2003; Madgwick et al. 2003; Coil et al. 2004; Davis et al. 2005), and require zs > zl + 0.1 to avoid contamination from physically-associated lens-source pairs.”
Galaxy halo masses and satellite fractions from galaxy–galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies (2005, methodology): “…redshifts and their error distributions determined using a sample of galaxies in the Groth strip with redshifts from DEEP2 (Davis et al. 2003; Madgwick et al. 2003; Coil et al. 2004; Davis et al. 2004), and require zs > zl + 0.1 to avoid contamination from physically-associated lens-source pairs.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, methodology): “For the EGS field, we use the Deep2 CFHT/12k mosaic imaging of the field (Coil et al. 2004; Davis et al. 2007), initially registered to the USNO-A2.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “With accurate multiband photometries andmedium-resolution spectra now available from large-redshift surveys such as the 2dFGRS, the SDSS, and the DEEP2 Galaxy Redshift Survey (Coil et al. 2004), it is now possible to study in detail a wide range of properties of the galaxy population, such as spatia”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, methodology): “…to detect absorption lines against the stellar continua in reasonable exposure times, we selected galaxies having BAB < 23, where B-band photometry was obtained from Capak et al. (2004, GOODS-N), Giavalisco et al. (2004, GOODS-S), and CFHT imaging of the EGS (Davis et al. 2003; Coil et al. 2004).”
DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “At redshift lower than 1.3, large-scale structures have been mapped by the DEEP2, 2dF and SDSS surveys (Coil et al. 2004; Peacock et al. 2001; Doroshkevich et al. 2004).”
Spectroscopic Identification of a Protocluster at z = 2.300: Environmental Dependence of Galaxy Properties at High Redshift (2005, background): “2 Carnegie Fellow 3 Miller Fellow ate (e.g., Coil et al. 2004) and high (e.g., Daddi et al. 2003; Adelberger et al. 2004a, 2005) redshift all indicate highly significant differences in clustering amplitude as a function of galaxy color and/or rest-frame optical luminosity, in the sense that redder…”
A COSMIC VARIANCE COOKBOOK (2010, background): “This may be particularly true at high redshift, where galaxies are expected to be much more strongly clustered than dark matter (Kauffmann et al. 1999; Baugh et al. 1999; Coil et al. 2004; Moster et al. 2010).”
The Spatial Clustering of Star-forming Galaxies at Redshifts 1.4 ≲ z ≲ 3.5 (2004, background): “By z 1 their correlation length will be similar to the correlation length of early-type (i.e., ‘‘absorption line’’) galaxies in the sample of Coil et al. (2004).”
GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 (2010, background): “…show stronger clustering and are thus associated with more massive halos, and the relationships between color and clustering seems to persist (Coil et al. 2004; Le Fèvre et al. 2005; Phleps et al. 2006; Coil et al. 2006; Pollo et al. 2006; Coil et al. 2008; Meneux et al. 2008; McCracken et…”
Galaxy bimodality due to cold flows and shock heating (2004, background): “Our model predicts a similar behavior of M/L(M) at z ∼ 1, to be revealed by spectroscopic surveys (such as the DEEP2/3 Madgwick et al. 2003; Coil et al. 2004), which have already confirmed the predicted invariance of the bi-modality mass in this redshift range (Fig.”
THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS (2012, methodology): “This “prewhitening” is done to reduce the impact of possible systematic color errors within a single CFHT 12K pointing, which are of order 0.02-0.04 mag (Coil et al. 2004b).”
Ultraviolet to Mid-Infrared Observations of Star-forming Galaxies at z ~ 2: Stellar Masses and Stellar Populations (2005, background): “…in numerical simulations, Adelberger et al. argue that the BX galaxies are consistent with typical total halo masses of > ∼ 10 12 M⊙ and that by z ∼ 1 they will have a clustering strength similar to that of galaxies with early type spectra in the DEEP2 redshift survey results of Coil et al. (2004).”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, background): “The current and upcoming large galaxy surveys (e.g., SDSS, Adelman-McCarthy et al. 2006; Deep Evolutionary Exploratory Probe [DEEP2], Coil et al. 2004; Dark Energy Survey [DES], Abbott et al. 2005; Large Synoptic Survey Telescope [LSST]; and Supernova/Acceleration Probe [SNAP], Aldering et al.…”
The DEEP2 Galaxy Redshift Survey: the relationship between galaxy properties and environment at z∼ 1 (2006, methodology): “…completeness of the DEEP2 survey, we scale the density measured about each galaxy according to the local value of the 2D survey completeness map, w(α, δ), which accounts for variations in targeting rate and redshift completeness from position to position within the survey (Coil et al. 2004b).”
THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1 (2009, methodology): “The spectra were reduced using an early version of the pipeline developed by the DEEP2 Redshift Survey Team (Coil et al. 2004; J. A. Newman et al. 2010, in preparation).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, methodology): “Measurements of Rest–frame Colors, Luminosities, and Environments Rest–frame (U −B) colors and absolute B–band magnitudes, MB, are calculated from CFHT B,R, I photometry (Coil et al. 2004b) using the K–correction procedure described in Willmer et al. (2006).”
Binary Quasars in the Sloan Digital Sky Survey: Evidence for Excess Clustering on Small Scales (2005, background): “Adelberger et al. (2003) and Coil et al. (2004) have measured the correlation function of galaxies at z 3 and z 1, respectively, down to scales as small as 100–200 h 1 kpc, and no small-scale excess clustering was found.”
Chemical Abundances of DEEP2 Star-forming Galaxies at z~1.0-1.5 (2005, methodology): “Photometric data were taken in B, R and I-bands with the CFH12k camera on the 3.6-m Canada-France-Hawaii telescope (see Coil et al. 2004b, for details).”