The Dependence on Environment of the Color-Magnitude Relation of Galaxies

By David W. Hogg, M. Blanton, J. Brinchmann, Daniel J. Eisenstein, David Schlegel, James E. Gunn, T. McKay, Hans-Walter Rix, N. Bahcall, J. Brinkmann and 1 more. 2003

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The distribution in color and absolute magnitude is presented for 55,158 galaxies taken from the Sloan Digital Sky Survey in the redshift range 0.08 < z < 0.12, as a function of the galaxy number overdensity in a cylinder of transverse radius 1 h-1 Mpc and line-of-sight half-length 8 h-1 Mpc. In all environments, bulge-dominated galaxies (defined to be those with radial profiles best fitted with large Sérsic indices) have a color-magnitude diagram dominated by red galaxies for which the mode of the color distribution at fixed absolute magnitude depends linearly on absolute magnitude. Although the most luminous galaxies reside preferentially in high-density regions and blue galaxies reside preferentially in low-density regions, there is only a barely detectable variation with overdensity in the color (zero point) or slope of the linear relation between the mode color and luminosity [<0.02 mag in 0.1 or (B-V)]. These results constrain variations with environmental density in the ages or metallicities of typical bulge-dominated galaxies to be under 20%.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “The mean color and dispersion of these two (red and blue) distributions depend on luminosity, but little on galaxy environment (Blanton et al. 2003; Balogh et al. 2004; Hogg et al. 2004).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, background): “…South Ellis Avenue, Chicago, IL 60637 13 North American ALMA Science Center, NRAO Headquarters, 520 Edgemont Road, Charlottesville, VA 22903 (e.g., Hogg et al. 2004; Park et al. 2007), it is clear that the mean properties of galaxies we measure depend strongly on the type of environment they…”
The Tully-Fisher Relation and its Residuals for a Broadly Selected Sample of Galaxies (2006, result): “In accord with the usual trends for luminosity-environment correlations (e.g., Hogg et al. 2004), the high-luminosity galaxies are predominantly in overdense regions, while the lower luminosity galaxies are found in less dense regions.”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “…range of galaxy properties, including morphology, star-formation rate, and color, depend on local density (Gómez et al. 2003; Balogh et al. 2004a,b; Hogg et al. 2004; Kauffmann et al. 2004; Tovmassian et al. 2004; Blanton et al. 2005a; Christlein & Zabludoff 2005; Croton et al. 2005; Rojas et al.…”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, background): “They found that the ridgeline slope is nearly independent of cluster richness, consistent with findings that the slope is independent of environment (Hogg et al. 2004).”
GEMS: Galaxy Fitting Catalogs and Testing Parametric Galaxy Fitting Codes: GALFIT and GIM2D (2007, background): “…authors have used a constant value of n = 2.5 or n = 2.0 to crudely distinguish earlytype (bulge-dominated) from late-type (disk-dominated) galaxies (e.g., Blanton et al. 2003; Shen et al. 2003; Hogg et al. 2004; Bell et al. 2004; Barden et al. 2005; McIntosh et al. 2005; Ravindranath et al. 2004).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “This relies on the assump- tion that the color-redshift relation does not vary with environment (Hogg et al. 2004; Gruen & Brimioulle 2017).”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, methodology): “This dependence on galaxy luminosity/mass and environment is also observed in local samples (Hogg et al. 2004; Bernardi et al. 2005; McIntosh et al. 2005; Gallazzi et al. 2006).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, background): “It is not clear how it can explain dependencies on environment even if galaxies are selected with the same r-band luminosity or the same stellar mass (Hogg et al. 2004; van der Wel 2008).”
Evolution and Environment of Early-Type Galaxies (2005, background): “For instance, the Mg-σ relation shows only a weak dependence on environment (Bernardi et al. 1998), and recent work with the SDSS indicates that the color-magnitude relation also shows little dependence on environment (Bernardi et al. 2003d; Hogg et al. 2004; Balogh et al. 2004; Wake et al. 2005).”
Spectroscopic Identification of a Protocluster at z = 2.300: Environmental Dependence of Galaxy Properties at High Redshift (2005, background): “…while highly significant at z = 2.30, would be relatively subtle by z ∼ 0, where (average) age differences of <∼ 1 Gyr relative to ages in the range 11−12 Gyr would probably be “in the noise” of spectroscopic or photometric age dating for local earlytype galaxies (e.g., Hogg et al. 2004).”
Ages and metallicities of early-type galaxies in the SDSS: new insight into the physical origin of the colour-magnitude and the Mg2-sigmaV relations (2006, background): “While the slope of the CMR in low-density environments is not significantly different from that found for cluster early-type galaxies, the scatter about the relation appears to increase from highto low-density environments (Larson et al. 1980; Hogg et al. 2004).”
A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, methodology): “The tines of the tuningfork diagram correspond roughly to the red sequence and blue cloud in the SDSS color-magnitude diagram (Strateva et al. 2001; Bernardi et al. 2003; Hogg et al. 2002, 2004; Blanton et al. 2003, 2005; Baldry et al. 2004).”
Red Galaxy Growth and the Halo Occupation Distribution (2008, background): “The Red Galaxy Sample The distribution of galaxy colors is bimodal (e.g., Hogg et al. 2004), and selection criteria for red galaxies typically fall near the minimum between the red and blue galaxy populations (e.g., Madgwick et al. 2002; Bell et al. 2004;Willmer et al. 2006).”
Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “1 Mpc) environment, with little-to-no additional dependence on larger scale environment (Hogg et al. 2004; Kauffmann et al. 2004; Blanton et al. 2005).”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, background): “Many authors in the past have investigated the relations between environment and galaxy properties (Lewis et al. 2002; Gómez et al. 2003; Goto et al. 2003a; Balogh et al. 2004a, 2004b; Hogg et al. 2004; Tanaka et al. 2004; Kuehn & Ryden 2005; Desroches et al. 2006).”
Ongoing assembly of massive galaxies by major merging in large groups and clusters from the SDSS (2007, background): “This selection effectleads to a slight systematic under representation in regions of high galaxy number density (Hogg et al. 2004), such as in massive groups and clusters.”
A CATALOG OF DETAILED VISUAL MORPHOLOGICAL CLASSIFICATIONS FOR 14,034 GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2010, methodology): “Column 45 : Environmental over-density (rho) estimated by NYU-VAGC group (Hogg et al. 2004; Blanton et al. 2005a).”