The size distribution of galaxies in the Sloan Digital Sky Survey

By S. Shen, H. Mo, Simon D. M. White, M. Blanton, G. Kauffmann, Wolfgang Voges, J. Brinkmann, István Csabai. 2003

937 citations recorded by the source corpus.

We use a complete sample of about 140,000 galaxies from the Sloan Digital Sky Survey (SDSS) to study the size distribution of galaxies and its dependence on their luminosity, stellar mass, and morphological type. The large SDSS database provides statistics of unprecedented accuracy. For each type of galaxy, the size distribution at given luminosity (or stellar mass) is well described by a log-normal function, characterized by its median ¯

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/be1300e32352c3d2e0418655664ff8bbbe85b270

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Citations in the corpus

Structure and Star Formation in Galaxies out to z = 3: Evidence for Surface Density Dependent Evolution and Upsizing (2008, background): “This is comparable to the scatter in the relation for the SDSS sample for galaxies with masses lower than 4 1010 M⊙ (Shen et al. 2003).”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, methodology): “…galaxies, which are more centrally concentrated, are expected to have larger values of Cr, and two values are in common use: a more conservative Cr ≥ 2.86 (e.g. Nakamura et al. 2003; Shen et al. 2003) and a more cavalier Cr ≥ 2.6 (e.g. Strateva et al. 2001; Bell et al. 2003; Kauffmann et al. 2003).”
The Dramatic Size Evolution of Elliptical Galaxies and the Quasar Feedback (2008, background): “Since similarly superdense massive galaxies are extremely rare or absent at z ≃ 0 (Shen et al. 2003) a strong size evolution, by a factor ∼ 3 or more, is indicated.”
Ultradiffuse galaxies: the high-spin tail of the abundant dwarf galaxy population (2016, background): “We do not distinguish galaxies according to their morphology, implicitly assuming that the initial spin sets the size of stellar spheroids as it does for disks (Shen et al. 2003; Kravtsov 2013).”
Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging (2008, methodology): “Barden et al. 2005, ApJ, 635, 959 Bernardi M., Sheth R. K., Nichol R. C. et al., 2006, ApJ, 640, 241 Bertin E. & Arnouts S., 1996, A&AS, 117, 393 Boylan-Kolchin M., Ma C-P., Quataert E., 2006, MNRAS, 369, 1081 Bruzual G., Charlot S., 2003, MNRAS, 344, 1000 Bundy K. et al., 2006, ApJ, 651, 120 Chabri”
An Observed Fundamental Plane Relation for Supermassive Black Holes (2007, background): “0±0.4 (ignoring the log-quadratic and higher order terms, which are not significant), similar to that found for all SDSS galaxies by Shen et al. (2003), and M∗ ∝ σ3.”
The Morphological Diversities among Star-forming Galaxies at High Redshifts in the Great Observatories Origins Deep Survey (2006, methodology): “We adopt then > 2.5 criteria to distinguish spheroid-like galaxies from disk-like galaxies, which is al o the classification used for low-z galaxies in the SDSS (Shen et al. 2003).”
A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “However, we note that the difference between the E+bulge and Sph+disk sequences is also seen in an SDSS study of 140,000 galaxies by Shen et al. (2003).”
Red mergers and the assembly of massive elliptical galaxies: the fundamental plane and its projections (2006, neutral): “This difference is comparable to the observed scatter in the relation, σ ln r ≈ 0.3 (Shen et al. 2003).”
Pre-Processing of Galaxies before Entering a Cluster (2003, neutral): “Shen et al. (2003) showed that the typical radius and mass of late-type galaxies have the relation R∝M0.”
Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology (2006, methodology): “…(n > 2.5) galaxies (“late” and “early” type, respectively), consistent with the analysis conducted by the Sloan Digital Sky Survey (SDSS; see Shen et al. 2003), and more recently the Galaxy Evolution by Morphology…”
Strong-lensing optical depths in a ΛCDM universe – II. The influence of the stellar mass in galaxies (2007, background): “Shen et al. (2003)4 studied the size distribution of 140 000 galaxies in the Sloan Digital Sky Survey (SDSS) and found a relation R̄e ∝M0.”
The Millennium Galaxy Catalogue : morphological classification and bimodality in the colour-concentration plane (2006, background): “The size distribution shows no bimodality but a broadening towards lower luminosity as found by Shen et al. (2003) and Driver et al. (2005).”
CONNECTING ANGULAR MOMENTUM AND GALACTIC DYNAMICS: THE COMPLEX INTERPLAY BETWEEN SPIN, MASS, AND MORPHOLOGY (2015, background): “This is done to account for the fact that, for a given mass, disk galaxies have a larger effective radius than spheroids (Shen et al. 2003), and to better resemble the radius ranges studied in FR13.”
MINOR MERGERS AND THE SIZE EVOLUTION OF ELLIPTICAL GALAXIES (2009, background): “The galaxy is slightly more compact than typical SDSS early-type galaxies at this mass but lies within the observed distribution (Shen et al. 2003, see also Franx et al. 2008).”
The Kinematic Structure of Merger Remnants (2006, background): “To check the absolute size of our merger remnants, we note that the size-mass relationship found in the Sloan Digital Sky Survey (SDSS) for early-type galaxies suggests a typical size of 3.4 kpc for galaxies of equivalent stellar mass (∼ 8 × 1010M⊙) to our simulated remnants (Shen et al. 2003).”
The ATLAS3D project – I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria (2010, methodology): “SimilarRe − L relations were derived by Shen et al. (2003) for early-type and late-type galaxies, defined as those having a Sersic (1968) index larger or smaller thann = 2.5 respectively.”
The Millennium Galaxy Catalogue: the B-band attenuation of bulge and disc light and the implied cosmic dust and stellar mass densities (2007, background): “Indeed, recent observational studies have produced evidence that the size distribution of galaxies, at fixed luminosity, is broader than that predicted from hierarchical simulations (see Shen et al. 2003; Driver et al. 2005).”
An Explanation for the Observed Weak Size Evolution of Disk Galaxies (2006, methodology): “The observational relationship between radial size (effective radius or disk scale length) and luminosity or stellar mass for disks at low redshift has now been wellcharacterized by studies based on the Sloan Digital Sky Survey (SDSS; e.g. Shen et al. 2003, hereafter S03).”