The Overdensities of Galaxy Environments as a Function of Luminosity and Color

By David W. Hogg, M. Blanton, Daniel J. Eisenstein, James E. Gunn, David Schlegel, Idit Zehavi, N. Bahcall, J. Brinkmann, István Csabai, D. Schneider and 2 more. 2002

259 citations recorded by the source corpus.

We study the mean environments of galaxies in the Sloan Digital Sky Survey (SDSS) as a function of rest-frame luminosity and color. Overdensities in galaxy number are estimated in 8 and 1 h-1 Mpc spheres centered on 115,000 galaxies taken from the SDSS spectroscopic sample. We find that, at constant color, overdensity is independent of luminosity for galaxies with the blue colors of spirals. This suggests that at fixed star formation history, spiral-galaxy mass is a very weak function of environment. Overdensity does depend on luminosity for galaxies with the red colors of early types; both low-luminosity and high-luminosity red galaxies are found to be in highly overdense regions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/841dbd1bda349be3181e962f77f687eef5ce2d48

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

Citations in the corpus

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1 (2009, background): “…Kauffmann et al. 2004) suggest that observables such as morphology, stellar masses, colours and star formation histories in addition to be correlated among them are also all correlated to the environment (Hogg et al. 2003; Kauffmann et al. 2003, 2004; Blanton et al. 2005a; Baldry et al. 2006).”
Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, background): “They confirm the increase in the fraction of red, bulge-dominated galaxies with galaxy density and clustercentric distance (Goto et al. 2003a; Hogg et al. 2003; Balogh et al. 2004; De Propris et al. 2004) that was known to exist in rich, nearby clusters.”
Spectroscopic Identification of a Protocluster at z = 2.300: Environmental Dependence of Galaxy Properties at High Redshift (2005, background): “…universe, regions that were over-dense on ∼ 10 Mpc scales at high redshift have virialized to become rich galaxy clusters, harboring much more than their fair share of galaxies with the largest stellar masses and (apparently) the oldest luminosity-weighted stellar ages (e.g., Hogg et al. 2003).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, background): “…et al. 2004), morphology (e.g., Dressler 1980; Goto et al. 2003; Park et al. 2007), stellar mass (e.g., Kauffmann et al. 2004), color (e.g., Hogg et al. 2003; Balogh et al. 2004; Blanton et al. 2005), and luminosity (e.g., Croton et al. 2005; Park et al. 2007) are all strongly correlated…”
The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, result): “It also nicely explains why broad-band colours are more predictive of environment than morphology, as noted by Hogg et al. (2003) and Blanton et al. (2005b), and is in good agreement with the results of Hester (2006b).”
The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties (2007, background): “On the other hand, the luminosity of blue sequence galaxies is nearly independent of environment, while both luminous and faint red galaxies are found on average in higher density environments than intermediate luminosity red galaxies (Hogg et al. 2003).”
THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, background): “The bimodal color distribution separates red early-type galaxies from blue late-type star forming galaxies (Strateva et al. 2001; Hogg et al. 2003; Baldry et al. 2004; Willmer et al. 2006).”
Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, background): “However, many studies have also established the view that the evolution of galaxies is a strong function of environment, both observationally (e.g. Hogg et al. 2003; Kauffmann et al. 2004; Blanton et al. 2005a; Baldry et al. 2006; Peng et al. 2010) and theoretically (e.g. Crain et al. 2009), based…”
The Optical and Near-Infrared Properties of Galaxies. I. Luminosity and Stellar Mass Functions (2003, background): “The red sequence of galaxies from the field environment is known to contain predominantly early-type galaxies (Schweizer & Seitzer 1992; Hogg et al. 2003).”
Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies (2005, background): “The clustering bias of LRGs is known to be a strong function of luminosity (Hogg et al. 2003; Eisenstein et al. 2004; Zehavi et al. 2004a) and while the LRG sample is nearly volume-limited out to z ∼ 0.36, the flux cut does produce a varying luminosity cut at higher redshifts.”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “In the Sloan Digital Sky Survey (SDSS - see York et al. 2000), Hogg et al. (2003) find that for the blue cloud in the colour-magnitude diagram, the environment density correlates with colour (redder galaxies lie in denser environments) (see also Balogh et al. 2004; Blanton et al. 2005a; Baldry et…”
The physical properties of star-forming galaxies in the low-redshift universe (2003, background): “Number distributions as function of many photometric properties and as a function of local density have been discussed in detail by Blanton et al. (2003b) and by Hogg et al. (2003).”
The Dependence on Environment of the Color-Magnitude Relation of Galaxies (2003, background): “…massive of these bulge-dominated galaxies reside preferentially in the most dense environments and especially in rich clusters of galaxies (Dressler 1980; Postman & Geller 1984); indeed the most massive red galaxy populations have the highest average environmental overdensities (Hogg et al. 2003).”
What Aspects of Galaxy Environment Matter? (2006, methodology): “For example, we can measure as a function of galaxy properties the mean environments around galaxies (Hogg et al. 2003; Blanton et al. 2005a) or their correlation functions (Davis & Geller 1976; Santiago & Strauss 1992; Hermit et al. 1996; Norberg et al. 2002; Zehavi et al. 2004).”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, background): “…play a part in the observed trend that dim red galaxies are substantiallymore clustered than their intermediate-luminosity counterparts (e.g., Norberg et al. 2002; Hogg et al. 2003), although the basic effect can be explained if the majority of these galaxies are satellites (Berlind et al. 2005).”
Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey (2003, background): “The dependence of overdensity on color and luminosity takes an interesting form, as noted previously by Hogg et al. (2003).”