Supermassive Black Holes (SMBHs) have been established to be at the center of all massive galaxies.Some of these are known to be accreting matter from their host galaxies, dubbed as Active GalacticNuclei (AGN). It is now known that AGN and their host galaxies coevolve. However, a clear concisedoes not exist if this coevolution is causal or casual.This thesis explores the coevolution of these AGN and their host galaxies from largest to the smallestscales. First, utilizing data from the Galaxy and Mass Assembly (GAMA) survey, we compare the largescale environments of 205 Quasars at z < 0.35 against a robust Markov chain Monte Carlos (MCMC)sample of 205,000 inactive galaxies matched in terms of both stellar mass and redshift. The resultsassert that there is no significant difference between the environment of active and inactive galaxies,implying that stochastic processes are the dominant triggers of AGN at low redshift.Second, we compare the global and spatially resolved star formation rates (SFR) and specific starformation rates (sSFR) of AGN and non-AGN host galaxies. We compare the properties of 32 X-rayselected AGN using data from the Chandra X-ray Observatory and XMM-Newton survey against amass matched control sample. Stellar masses and SFR are obtained by fitting Spectral EnergyDistributions (SED) of galaxies with 60 optical narrow-band multi-wavelength data from the miniJPASSurvey, which is a 1 deg2 preview of the upcoming Javalambre-Physics of the Accelerated UniverseAstrophysical Survey (J-PAS) survey. Our results show that while there are no differences between theglobal properties of X-ray AGN and non-AGN host galaxies, their sSFR profiles exhibit the exactopposite trend. This suggests that X-ray AGN quench their host galaxies in the central regions, whilesimultaneously pushing gas to the outskirts of their host galaxy where star formation takes place, forexample by compression of gas due to positive feedback.Following up on the results of our X-ray AGN host galaxies, we examine the radial profiles of RadioAGN host galaxies in the third part of this thesis. We use 12 band optical data from the JavalambrePhotometric Local Universe Survey (J-PLUS), which is another prelude to the J-PAS survey covering3,192 deg2 of the northern sky. Then, we use data from the Low-Frequency Array (LOFAR) survey tocross-match and select a sample of 441 Radio AGN hosts in the J-PLUS field at z < 0.15 and comparetheir radial profiles against a Baldwin, Phillips & Terlevich (BPT) diagram selected star forming sample.The results corroborate our findings for X-ray AGN, which posit a radially increasing sSFR for RadioAGN host galaxies. This reaffirms the result that AGN quench their hosts in the center, while enhancingtheir sSFR on the outskirts of galaxies. Moreover, examining the M¿¿MBH scaling relation, we find thathighly star forming galaxies lie above scaling relation observed for local galaxies, whereas quenchedgalaxies like below the local relation, with the average Eddington rate (¿Edd) being~2%.

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