Physical properties and environments of nearby galaxies

By M. Blanton, John Moustakas. 2009

384 citations recorded by the source corpus.

We review the physical properties of nearby, relatively luminous galaxies, using results from newly available massive data sets together with more detailed observations. First, we present the global distribution of properties, including the optical and ultraviolet luminosity, stellar mass, and atomic gas mass functions. Second, we describe the shift of the galaxy population from "late" galaxy types in underdense regions to "early" galaxy types in overdense regions. We emphasize that the scaling relations followed by each galaxy type change very little with environment, with the exception of some minor but detectable effects. The shift in the population is apparent even at the densities of small groups and therefore cannot be exclusively due to physical processes operating in rich clusters. Third, we divide galaxies into four crude types -- spiral, lenticular, elliptical, and merging systems -- and describe some of their more detailed properties. We attempt to put these detailed properties into the global context provided by large surveys.

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

View Paper: https://www.semanticscholar.org/paper/080075c71f1634c2e857fdcd09031649a7d61298

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Citations in the corpus

Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey (2017, background): “Colors The optical colors of galaxies reveal their dominant stellar populations and thus correlate strongly with galaxy morphology, leading to the well-known separation of galaxies into red and blue sequences (e.g., Strateva et al. 2001; Blanton & Moustakas 2009).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “…color or star formation activity, such that disk-dominated galaxies are predominantly blue and star forming, while spheroid-dominated galaxies are largely red and quiescent, with nearly uniformly old stellar populations (e.g. Blanton & Moustakas 2009, Kauffmann et al. 2003, Roberts & Haynes 1994).”
The star formation history of CALIFA galaxies: Radial structures (2013, background): “This location correlates with stellar population properties (Kauffmann et al. 2003a,b; Baldry et al. 2004; Bell et al. 2004; Brinchmann et al. 2004; Gallazzi et al. 2005; Mateus et al. 2006, 2007; Blanton & Moustakas 2009).”
Theoretical Challenges in Galaxy Formation (2016, background): “…density profile (de Vaucouleurs 1948) and a flattened, rotationally supported disk/spiral component, which is typically somewhat larger (apart from the highest mass systems) and has a roughly exponential profile (e.g. Blanton & Moustakas 2009, Shen et al. 2003, van der Kruit & Freeman 2011).”
THE GEMINI CLUSTER ASTROPHYSICS SPECTROSCOPIC SURVEY (GCLASS): THE ROLE OF ENVIRONMENT AND SELF-REGULATION IN GALAXY EVOLUTION AT z ∼ 1 (2011, background): “In the last decade, the SDSS and other spectroscopic surveys have revolutionized this field, providing high-quality data that has quantified these correlations with high precision (see e.g., the review by Blanton & Moustakas 2009).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, background): “(The two classification schemes are certainly not identical, however; see, e.g., Choi, Park, & Vogeley 2007; Bamford et al. 2009; Blanton & Moustakas 2009; Skibba et al. 2009).”
A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies (2019, background): “M? space, a key parameter space for classifying galaxies (e.g., see Blanton & Moustakas 2009).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “But high-quality, multiband photometric and spectroscopic surveys have provided us with a different perspective (Blanton & Moustakas 2009).”
The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “…which discovered the clear and nearly universalT − Σ relation from a sample of about 6000 galaxies in 55 clusters,galaxy density has often been correlated to galaxy properties in large surveys to provide constraints on and test galaxy formationm dels (see Blanton & Moustakas 2009, for a review).”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, background): “The evidence based on such datasets suggests that the transformation from star-forming to quiescent galaxies is a smooth function of density, and happens in great part outside clusters (e.g. Dressler 1980; Lewis et al. 2002; Gómez et al. 2003; Blanton & Moustakas 2009).”
The Evolution of Galaxy Structure Over Cosmic Time (2014, background): “For nearby galaxy’s a few recent relevant reviews are Blanton & Moustakas (2009), van der Kruit & Freeman (2011), and Conroy (2013).”
Galaxy and mass assembly (GAMA): End of survey report and data release 2 (2015, background): “…recently, full hydrodynamical simulations (Vogelsberger et al. 2014; Schaye et al. 2015), advances in this field are to a significant extent driven by observationally exploring the physical properties of galaxies, their interdependences and their evolution with time (e.g. Blanton & Moustakas 2009).”
Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “Large-scale galaxy surveys, such as the Sloan Digital Sky Survey (SDSS; York et al. 2000), have enabled detailed examinations of the correlations between these galaxy properties and their environment at z ≈ 0 (see Blanton & Moustakas 2009, for a recent review).”
PRIMUS: THE DEPENDENCE OF AGN ACCRETION ON HOST STELLAR MASS AND COLOR (2011, background): “The fraction of the total stellar mass contained in the bulge will depend on the galaxy morphology, which in turn is related to both the color and stellar mass of the host galaxy (see Blanton & Moustakas 2009), introducing significant scatter to our Mbh estimates.”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, background): “…correlation between B-luminosity and slope using either calibration, although a noisy, but significant correlation appears if the slope is expressed in physical units, i.e., dex kpc−1, owing to the tendency for luminous disk galaxies to be larger (Garnett et al. 1997; Blanton & Moustakas 2009).”
The effect of the environment on the Hi scaling relations (2011, background): “…one of the main issues for environmental studies is to reconcile the evidence that the effects of the environment start at densities typical of poor groups (Blanton & Moustakas 2009 and references therein) with the fact that Hi-deficient objects are only observed in clusters of galaxies.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “For more general reviews, the reader is referred to Blanton & Moustakas (2009) and Kormendy & Bender (2012) for normal galaxies and to Boselli & Gavazzi (2014), for emphasis on the faint end of the galaxy luminosity.”
The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “Results show that most of the massive nearby galaxies are ellipticals, S0’s, or spirals (Blanton & Moustakas 2009) following the Hubble tuning fork diagram.”