We examine the physical properties of 173 cluster members in CL 1358+62 ( z = 0.3283 ) from HST WFPC2 imaging taken in the F606W ( \sim rest-frame B ) and F814W ( \sim rest-frame V ) filters over a 2.2 \times 2.2 Mpc ^ { 2 } field ( H _ { 0 } = 100 km s ^ { -1 } Mpc ^ { -1 } , \Omega _ { M } = 0.3 , \Omega _ { \Lambda } = 0.7 ) .
Structural parameters are measured for each galaxy by fitting a PSF-convolved , two component model to their 2D surface brightness distribution .
We examine bulge+disk models using three different bulge profiles ( de Vaucouleurs , Sérsic , and exponential ) , and rigorously test the robustness of our results by analyzing several thousand artificial galaxies in the same manner as the cluster data .
The measured physical properties from the best-fit profile of the cluster galaxies are combined with ground-based spectroscopy to test for correlations between morphological characteristics , current star formation , total galaxy colors , and cluster substructure .
We find that : ( 1 ) Bulge-to-total ratio [ ( B / T ) _ { deV } ] and Hubble type ( -5 \leq T \leq 8 ) are strongly correlated ( 99 % confidence ) , but the scatter is large and early-type spirals are not reliably distinguished from ellipticals and S0 ’ s based on ( B / T ) _ { deV } .
( 2 ) From comparison of their physical properties , the low luminosity ( -17.3 \geq MB _ { z } -5 \log h \geq - 19.3 ) ellipticals in our sample are likely to be face-on S0 galaxies .
( 3 ) High galaxy asymmetry and strong [ OII ] \lambda 3727 emission are strongly correlated for disk-dominated members [ ( B / T ) _ { deV } < 0.4 ] .
( 4 ) There exists a small population ( \sim 5 % ) of bulge-dominated members whose significant [ OII ] \lambda 3727 emission ( < -5 Å ) suggest they harbor active galactic nuclei .
( 5 ) At these redshifts , determining the correct Sérsic index n can be highly unreliable .