below).

In Figure \[critical\], we also show a preliminary SDSS [*Morphology–Radius*]{} ([[$T$–R]{}]{}) relation based on the work of Goto et al. (in prep). The morphological classifications used in this figure are based on new, and improved, concentration index ($C_{in}$; see Shimasaku et al. 2001) measurement of Yamauchi et al. (in prep). Briefly, Yamauchi et al. (in prep) compute their concentration index within two–dimensional, elliptical isotopes, which account for the observed ellipticity and orientation of the galaxy on the sky. This improvement helps prevent low inclination galaxies ([*e.g.*]{}, edge–on spirals) from being mis–classified as early-type galaxies. Furthermore, Yamauchi et al. (in prep) computes the “coarseness” of each galaxy, which is a measure of the residual variance after the best fit 2–D galaxy model has been subtracted. This coarseness measurement can therefore detect the presense of spiral arms in a galaxy. These two measurements of the morphology are re–normalized (by their rms) and added to produce a final morphological parameter called [[$T_{auto}$]{}]{}. Yamauchi et al. (in prep) has tested their algorithm extensively and have demonstrated that [[$T_{auto}$]{}]{}is more strongly correlated with visual morphological classifications than the normal [[$C_{in}$]{}]{}parameter, with a correlation coefficient with the visual morphologies of 0.89.

Using the [[$T_{auto}$]{}]{}classification, Goto 