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Radiative cooling, star formation and supernova explosions processes that are also integral to the formation of a galaxy while processes such as accretion of gas, and galaxy mergers, govern the galaxy’s structure. These sets of processes together drive the formation and evolution of galaxies \cite{Ceverino_2009}.  \citet{Fanaroff_1974} Fanaroff et al. (1974)  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. \citet{Saripalli_2012} Saripalli et al. (2012)  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. \citet{Singal_2014} Singal et al. (2014)  states that the morphology of galaxies is closely related to their luminosities. It is said that \citet{Fanaroff_1974} Fanaroff et al. (1974)  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. \citet{Singal_2014} Singal et al. (2014)  further discovered that FR-I and FR-II morphology is dependent only on luminosity and not redshift. \citet{Fanaroff_1974} Fanaroff et al. (1974)  observed that the luminosity of FR-I galaxies falls below a threshold luminosity at 1.4 GHz $ L_{1.4} = 2 \times 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).