The environmental dependence of the relations between stellar mass, structure, star formation and nuclear activity in galaxies

By G. Kauffmann, Simon D. M. White, T. Heckman, B. Ménard, J. Brinchmann, S. Charlot, Christy A. Tremonti, J. Brinkmann. 2004

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We use a complete sample of galaxies drawn from the Sloan Digital Sky Survey to study how structure, star formation and nuclear activity depend on local density and on stellar mass. Local density is estimated by counting galaxies above a fixed absolute magnitude limit within cylinders 2 Mpc in projected radius and ±500 km s -1 in depth. The stellar mass distribution of galaxies shifts by almost a factor of two towards higher masses between low-and high-density regions. At fixed stellar mass both star formation and nuclear activity depend strongly on local density, while structural parameters such as size and concentration are almost independent of it. Only for low-mass galaxies (M * 1-Gyr) time-scales. Since structure does not depend on environment for galaxies with masses greater than 3 x 10 10 M ○. , the trends in recent SFH, dust and nuclear activity in these systems cannot be driven by processes that alter structure, for example mergers or harassment. The SFH-density correlation is strongest for small-scale estimates of local density. We see no evidence that star formation history depends on environment more than 1 Mpc from a galaxy. Finally, we highlight a striking similarity between the changes in the galaxy population as a function of density and as a function of redshift. We use mock catalogues derived from N-body simulations to explain how this may be understood.

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

View Paper: https://www.semanticscholar.org/paper/8b12c33f29bacf4536d8aa1e0470dfaa211ea5e2

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Citations in the corpus

What drives the growth of black holes (2011, background): “…a radius of 2 Mpc, the fraction of galaxies hosting radio-quiet AGN activity is ≈ 2 times higher in low-density regions than in high-density regions (Kauffmann et al., 2004), while the local galaxy density of radio-loud AGNs is ≈ 2 higher than that found for radioquiet AGNs (Kauffmann et al.,…”
CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and Mass Profiles (2003, methodology): “…gradual reductions in star formation rates and supports those that lead to sudden truncation of star formation (see also van Dokkum et al. 1998; Balogh et al. 2004) or mechanisms (of any timescale) which operate only until moderate redshifts (timescales &1.5 Gyr, see §4 and Kauffmann et al. 2004).”
Galaxy Protoclusters as Drivers of Cosmic Star Formation History in the First 2 Gyr (2017, background): “Galaxy clusters today make a negligible contribution to the cosmic star-formation rate density (CSFRD) due to their low number density (Bahcall & Cen 1993), compact sizes (Girardi et al. 1995), and quenched galaxy populations (Kauffmann et al. 2004).”
First results from the IllustrisTNG simulations: the galaxy colour bimodality (2017, methodology): “Studying environment, Kauffmann et al. (2004) and Baldry et al. (2006) used SDSS to demonstrate that while the location of the two populations in the D4000/color-mass plane does not correlate with (projected neighbor density) environment, the relative fraction in each population does.”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “…optical emission-line AGN is generally found to be lower in denser environments and in groups and clusters, than in the field (Miller et al. 2003, Kauffmann et al. 2004, von der Linden et al. 2007): the fraction of AGN among galaxies of given stellar mass decreases by a factor of two from the…”
THE CLUSTERING CHARACTERISTICS OF H i-SELECTED GALAXIES FROM THE 40% ALFALFA SURVEY (2012, background): “…the clustering of HI-selected galaxies are in agreement with pre- vious results, particularly with our understanding that ALFALFA galaxies tend to be blue, spiral, and late type galaxies which are already known to be weakly clustered (Norberg et al. 2002; Kauffmann et al. 2004; Zehavi et al. 2005).”
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Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology (2006, methodology): “The morphological parameters in our catalog may be used, for example, to address questions of “Nature vs. Nurture”, including the well-studied morphology-density relation (e.g., Kauffmann et al. 2004).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “…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. 2005; Cooper et…”
The 2dF Galaxy Redshift Survey: Luminosity functions by density environment and galaxy type (2004, methodology): “Only with the recent emergence of large galaxy redshift surveys such as the 2dFGRS and also the Sloan Digital Sky Survey (SDSS) can such a study be undertaken with any reasonable kind of precision (for the SDSS, see recent work by Hogg et al. 2003, Hoyle et al. 2003, and Kauffmann et al. 2004).”
Passively Evolving Early-Type Galaxies at 1.4 ≲ z ≲ 2.5 in the Hubble Ultra Deep Field (2005, neutral): “Similarly, the stellar surface mass density of the four galaxies, defined as ¼ M /(2r2e ), is more than a factor 10 higher than that of local galaxies with similar stellar masses (Kauffmann et al. 2004).”
WINGS: a WIde-field Nearby Galaxy-cluster Survey. I. Optical imaging (2005, background): “Results based on these surveys have highlighted the strong correlation between star formation properties in galaxies and local galaxy density, and that such a correlation exists both inside and outside of clusters (Lewis et al. 2002; Gómez et al. 2003; Kauffmann et al. 2004; Balogh et al. 2004).”
Metallicities and Physical Conditions in Star-forming Galaxies at z ~ 1.0-1.5 (2008, methodology): “In terms of environment, we find that 90%-95% of objects in the Main, Offset-SF, and Offset-AGN samples have zero or one neighbor, the lowest density bin in Kauffmann et al. (2004).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, result): “A similar result is found by Park et al. (2007) and Kauffmann et al. (2004).”
Modelling the galaxy bimodality: shutdown above a critical halo mass (2006, background): “Star forming galaxies are mainly confined to haloes below this mass and most galaxies in haloes above this threshold are evolving passively (Kauffmann et al. 2004).”
Physical properties and environments of nearby galaxies (2009, background): “It appears that among all these properties, the controlling variables are those related to mass and star-formation history — not those having to do with structure (Kauffmann et al. 2004; Blanton et al. 2005a; Christlein & Zabludoff 2005; Quintero et al. 2006).”
The Environmental Dependence of Galaxy Properties in the Local Universe: Dependences on Luminosity, Local Density, and System Richness (2004, background): “Kauffmann et al. (2004) reported that, at a fixed stellar mass, star formation and nuclear activity depend strongly on local density, while morphology is almost independent of local density.”
CONVERTING FROM 3.6 AND 4.5 μm FLUXES TO STELLAR MASS (2012, background): “We are increasingly realizing that M∗ is intricately connected to other galaxy properties, such as current star formation rate and morphology (Kauffmann et al. 2004).”