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It was in the late 1940s when the connection between cosmic radio waves and synchrotron emission was established. Synchrotron emission in AGN is due to the presence of magnetic fields. Electrons moving at near relativistic speeds spiral around magnetic field lines. Synchrotron emission is observable as polarized emission. Astrophysical objects emit intense radio waves through the synchrotron emission. It is widely held that radio sources in the Universe emit by the synchrotron process at lower radio frequencies in the meter and centimeter wavelength range.\cite{Wielebinski_2006}   The radio core of an AGN emits synchrotron radiation emitted through particle acceleration and collimation into a double lobed structure. These are typical traits of radio galaxies. AGN also have a pair of jets of material ejected from their core. The structure of a radio source is also determined by the interaction of its energetic jets with ionized gas which surround the host galaxy. \cite{Krawczynski_2013} also observe that the black holes in AGN accrete matter and convert the gravitational energy of the accreted matter (and possibly also the rotational energy of the black hole) into mechanical and electromagnetic energy. We also have that inside the accretion disk, a fraction of the gravitational energy of the accreted material is converted to heat and electromagnetic radiation which is then radiated away by the accretion disk. The jets are formed from a portion of the material processed through the accretion disk which escapes the accretion system as collimated and uncollimated outflows. Jet plasma velocity can be denoted by v where $v = \beta_{jet}*c \approx c $ ,and c represents the speed of light. $\Gamma_{jet}$ , the bulk Lorentz factor of the plasma is given by $ \Gamma_{jet} \eq =  (1 - (\Gamma_{jet})^2 )^{-1/2} (\beta_{jet})^2 )^{-1/2}$  . Emissions from the jets can be red or blue-shifted as a result of the relativistic Doppler factor $\delta_{jet} = \Frac{1}{\Gamma_{jet} \times (1- \beta_{jet}\times\cos{\theta})} \beta_{jet}\times\cos{\theta})}$  Where \theta is the angle between the jet axis and the line of sight as measured in the observer frame \cite{Krawczynski_2013}. The lobes as seen in Figure 5 develop when the jets are stopped by pressure from the gas surrounding the host galaxy. The lobe structure is fairly symmetrical when viewed closer to the nucleus of the galaxy.