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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 358774.0, MPI für Astronomie / Publikationen_mpia
Scaling relations of spiral galaxies
Authors:Courteau, S.; Dutton, A. A.; van den Bosch, F. C.; MacArthur, L. A.; Dekel, A.; McIntosh, D. H.; Dale, D. A.
Date of Publication (YYYY-MM-DD):2007
Title of Journal:The Astrophysical Journal
Start Page:203
End Page:225
Audience:Not Specified
Abstract / Description:We construct a large data set of global structural parameters for 1300 field and cluster spiral galaxies and explore the joint distribution of luminosity L, optical rotation velocity V, and disk size R at I and 2MASS K bands. The I- and K-band velocity-luminosity (VL) relations have log slopes of 0.29 and 0.27, respectively, with sigmaln(VL)~0.13, and show a small dependence on color and morphological type in the sense that redder, earlier type disk galaxies rotate faster than bluer, later type disk galaxies for most luminosities. The VL relation at I and K bands is independent of surface brightness, size, and light concentration. The log slope of the I- and K-band size-luminosity (RL) relations is a strong function of morphology and varies from 0.25 to 0.5, with a mean of 0.32 for all Hubble types. At most luminosities, early-type disk galaxies have shorter scale lengths than later type ones. The average dispersion sigmaln(RL) decreases from 0.33 at I band to 0.29 at K, likely due to the 2MASS selection bias against lower surface brightness galaxies. The VL and RL residuals are largely uncorrelated with each other with a correlation coefficient r=-0.16 and DeltalogV|L/DeltalogR|L=-0.07+/-0.01 the RV-RL residuals show a weak positive correlation with r=0.53. These correlations suggest that scatter in luminosity is not a significant source of the scatter in the
Free Keywords:Cosmology: Dark Matter; Galaxies: Formation; Galaxies: Kinematics and Dynamics; Galaxies: Spiral; Galaxies: Structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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