Evolution and Color Dependence of the Galaxy Angular Correlation Function: 350,000 Galaxies in 5 Square Degrees

By A. Coil, J. Newman, N. Kaiser, M. Davis, Chung-Pei Ma, D. Kocevski, D. Koo. 2004

149 citations recorded by the source corpus.

When applied to deep photometric catalogs, the two-point angular correlation function, ω(θ), is a sensitive probe of the evolution of galaxy clustering properties. Here we present measurements of ω(θ) as a function of IAB magnitude and (R - I) color to a depth of IAB = 24 on scales θ = 7′′-3′, using a sample of ~350,000 galaxies covering 5 deg2 in total over five separate fields. Using redshifts of 2954 galaxies in early DEEP2 Galaxy Redshift Survey data, we construct robust galaxy redshift distributions as a function of IAB magnitude and (R - I) color for galaxies in the range 0 < z < 2. We constrain models of the redshift evolution of galaxy clustering and find that significant growth of clustering has occurred from z ≥ 1 to z = 0. A model in which the comoving scale length, x0, evolves linearly with redshift, x0(z) = x0(0)(1 - Bz), fits the data better than the ϵ model proposed by Groth & Peebles. The clustering properties depend strongly on observed (R - I) color, with both the reddest and bluest galaxies exhibiting large clustering amplitudes and steeper slopes. Different observed (R - I) color ranges are sensitive to very disparate redshift regimes. Red galaxies with (R - I) ~ 1.5 lie in a narrow redshift range centered at z ~ 0.85 and have a comoving scale length of clustering at z = 0.85 of x0 = 5.0 ± 0.3 h-1 Mpc. These galaxies have early-type spectra and are likely progenitors of massive local ellipticals. The bluest galaxies with (R - I) ~ 0 appear to be a mix of star-forming galaxies, both relatively local (z ~ 0.3-0.6) dwarfs and bright z > 1.4 galaxies, as well as broad-line active galactic nuclei. We find that local blue dwarfs are relatively unclustered, with x0 = 1.6 ± 0.2 h-1 Mpc. The z > 1.4 blue galaxies have a larger clustering scale length, x0 ≳ 5 h-1 Mpc.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f0cf723c2fd6ca2a1fa16ccd463f2fa9c1ffb0bb

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

In Statistical and Nonlinear Physics

Citations in the corpus

Systematic errors in weak lensing: application to SDSS galaxy-galaxy weak lensing (2005, methodology): “First, we note that as discussed in Coil et al. (2004a), redshifts z > 1.45 cannot be measured by the DEEP2 survey.”
The All-Wavelength Extended Groth Strip International Survey (AEGIS) Data Sets (2006, background): “Details of the data reduction, astrometry, star-galaxy separation, and catalog construction can be found in Coil et al. (2004); the resulting catalogs are available at http://deep.berkeley.edu/DR1.”
A NEW DIAGNOSTIC OF ACTIVE GALACTIC NUCLEI: REVEALING HIGHLY ABSORBED SYSTEMS AT REDSHIFT >0.3 (2011, methodology): “For galaxies outside of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) field-of-view, we use CFHT 12k BRI photometry from Coil et al. (2004).”
The Evolving Luminosity Function of Red Galaxies (2006, methodology): “DEEP2 photometry uses the larger of a 200 diameter aperture or a 6 aperture, where is defined by aGaussian fit to the object profile (Coil et al. 2004).”
The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift (2011, methodology): “For each galaxy in the DEEP2/DEEP3 sample, rest-frame U − B colours and absolute B-band magnitudes, MB, are calculated from Canada–France–Hawaii Telescope (CFHT) BRI photometry (Coil et al. 2004) using the K-correction procedure described in Willmer et al. (2006).”
Photometric redshifts for the SDSS Data Release 12 (2016, methodology): “…due to an underestimation of astrometric accuracy – DEEP2, the survey responsible for 71.4% of outliers in the non-PRIMUS set, uses the Canada France Hawaii Telescope, which quotes the USNOA 2.0 astrometric error of 0.5′′ (Coil et al. 2004), the highest value of all the external surveys.”
Strong size evolution of the most massive galaxies since z~2 (2007, methodology): “The details of the data reduction for this data is provided in Coil et al. (2004).”
THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, methodology): “BRI photometry was obtained by the DEEP2 team for these objects from imaging carried out using the 1 http://www.deep.berkeley.edu/DR3/ CFH12K camera on the 3.6 m Canada France Hawaii Telescope (Coil et al. 2004).”
Cosmological baryonic and matter densities from 600 000 SDSS luminous red galaxies with photometric redshifts (2006, background): “…by guest on 29 July 2018 Evolutionary Probe (DEEP2; Davis et al. 2003) and the VIRMOSVLT Deep Survey (VVDS; Le Fevre et al. 2003) have produced impressive measurements of the clustering pattern over an area of a few square degrees (e.g. Coil et al. 2004; Le Fevre et al. 2005).”
THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, methodology): “The BRI−band photometry was measured from images taken with the CFH12K camera on the 3.6 m CanadaFrance-Hawaii Telescope (Coil et al. 2004).”
THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “The data are complete to∼ 25.25 in B, 24.75 in R, and∼ 24.25 in I (see Coil et al. 2004 for more details).”
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).”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, background): “Separation between stars and galaxies is based on magnitude, size, and color, which were used to assign each object a probability of being a galaxy; star-galaxy separation efficiency is discussed in Coil et al. (2004) and Paper I.”
The DEEP2 Galaxy Redshift Survey: Color and Luminosity Dependence of Galaxy Clustering at z ∼ 1 (2007, methodology): “These results are consistent with those of Coil et al. (2004b), who use an early DEEP2 data sample of 2200 galaxies at 0.7 < z < 1.35 in ∼ 0.35 deg2 to determine that galaxies redward of the median color of the sample, (B − R)0 = 0.7, have a significantly higher correlation length and steeper slope…”
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).”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, methodology): “Our sample is limited to areas covered simultaneously by Spitzer MIPS 24µm photometry (Davis et al. 2007), CFHT BRI photometry (Coil et al. 2004), DEEP2 and DEEP3 spectroscopy (Davis et al. 2007; Cooper et al. 2011, 2012), Palomar K-band photometry (Bundy et al. 2006), and GALEX UV photometry…”
AEGIS-X: THE CHANDRA DEEP SURVEY OF THE EXTENDED GROTH STRIP (2008, methodology): “To do so, we first matched the Xray catalogs to the DEEP2 optical photometry catalog (Coil et al. 2004) and the median RA and DEC offsets were calculated.”