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Fanaroff and Riley classification of radio galaxies groups them into two major categories FR-I and FR-II. The two categories are based on whether radio-galaxies have edge-darkened (FR-I) morphologies or edge-brightened (FR-II) morphologies. (http://arxiv.org/pdf/1206.6893v1.pdf) believes that these morphologies arose from the interaction of jets (as depicted in Figure 4)and the material in their surrounding environment. Spectroscopy observations further reveal that FR-I radio galaxy hosts exhibit optical spectra with only absorption lines, while FR-II hosts display mixed characteristics. Some FR-II hosts are similar to FR-Is in that they only exhibit absorption lines ,but some others have spectra with strong high ionization emission lines.  (http://arxiv.org/pdf/1212.0667v3.pdf) \cite{Singal_2014}  states that the morphology of galaxies is closely related to their luminosities. It is said that Fanaroff and Rilley noted that the morphology of radio galaxies is dependent on their luminosities. Since luminosity is in turn related to redshift, it is easy to confuse the effects due to luminosity as those due to redshift. http://arxiv.org/pdf/1212.0667v3.pdf \cite{Singal_2014}  further discovered that FR-I and FR-II morphology is dependent only on luminosity and not redshift. Fanaroff and Riley observed that the luminosity of FR-I galaxies falls below a threshold luminosity$ 2 \times 1025 10^{25}  W Hz^{-1}sr^{−1}$ . Studies have also shown that through optical observations we find most FR-II sources at find that at redshift ∼ 0.2 − 0.3 FR-II sources (\cite{Belsole_2007} , and references therein). From this we can conclude that the data we will be using in this study falls in the FR-I category - see Figures 9, 10 and 12.