This section briefly outlines the future possibilities. These include projects that could not be done due to lack of appropriate data and projects that could not be undertaken in the time available. Of the many projects that can be put in these categories, we mention a few here.
The fundamental plane
(Djorgovski and Davies, 1987; Dressler et al., 1987)
for ellipticals is a two-dimensional manifold in the three-dimensional
space formed by the global structural parameters
(1) scale length, 
,
(2) velocity dispersion, 
, and
(3) mean effective surface brightness
. The fundamental plane is likely to be independent of
environment (Jørgensen, 1996). The face-on view of
the fundamental plane
provides information about formation processes and evolution.
Lack of availability of velocity dispersion for the radio and control
galaxies has prevented us from locating these galaxies on the
fundamental plane. However,
we hope to do this as part of a future study.
With the available data we could have positioned the galaxies on the photometric fundamental plane, as well as ranked the galaxies within the surrounding region. However, even the group membership of certain galaxies close to the radio galaxy was uncertain. We will pursue these lines in the near future.
We have shown that on the average radio galaxies tend to possess excess blue color in the central region as compared to control galaxies. It is likely that the excess blue has its origin in a star formation episode in the recent past. High resolution spectra will allow us to determine the age and strength of such a burst of star formation.
It is now known that nuclear density profiles of elliptical galaxies continue to rise upto the smallest observable radius. It has been debated whether there exist two types of galaxies viz. those with a core and those with a cusp (e.g. Ferrarese et al., 1994) or it is a continuous family (Merritt, 1997) or, an artifact, to some extent, due to selection effects like distance to the objects (Faber et al., 1997). Dynamical modeling based on light distribution of the radio galaxies in our sample will provide valuable information on their intrinsic shapes. In case of dust lane galaxies, we have information about the radio source orientation and the position angle of the dust lane thus providing us with an additional vector to study the 3D shape than is usually available. We would like to pursue dynamical modeling in the future.