Traditionally, radio galaxies have been believed to be
ellipticals
consisting of a coeval population of old stars,
and almost no dust or gas. However, photometric studies
carried out over the past few years have demonstrated that
many elliptical galaxies not only have dust and gas, but also
possess fine structure indicating some amount of activity in
the past 
million years.
Radio galaxies host an active galactic nucleus (AGN) and are
associated with highly energetic phenomena like the radio
jets which transport a very large amount of energy over hundreds
of kiloparsecs.
Such phenomena are likely to be associated with morphological
features not found in normal elliptical galaxies.
In this chapter we present the results of fitting the 1D profiles
of galaxies as described in the previous chapter.
We show that the ratio 
of the bulge scale lengths in
filters, provides a measure of the color gradient in the galaxy.
The ratio is related to color gradients measured in the conventional way, but
is more robust: it can provide an estimate of the color gradient even
when the signal-to-noise ratio is not good enough for the gradient
to be measured unambiguously using conventional techniques. Using
the ratio we show that a large fraction of radio galaxies become bluer
towards the center. We compare in Chapter 
these results with
information obtained from color maps.
Our model fits indicate that radio galaxies tend to deviate from de Vaucouleurs' law near the center more often than control galaxies. We argue that the deviations are due to excess blue emission or dust absorption in the central region and obtain quantitative estimates.