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We use bulge-type classifications of 809 representative SDSS galaxies byGadotti (2009) to classify a large sample of galaxies into real bulges(classical or elliptical) and pseudobulges using Random Forest. We usestructural and stellar population predictors that can easily be measuredwithout image decomposition. Multiple parameters such as the central massdensity with 1 kpc, concentration index, S\'{e}rsic index and velocitydispersion do result in accurate bulge classifications when combined together.We classify $\sim 44,500$ face-on galaxies above stellar mass of 10$^{10}$M$_\odot$ and redshift $ 0.02 < z < 0.07$ into real bulges or pseudobulges with$93 \pm 2$\% accuracy. We show that $\sim 75 - 90\%$ of AGNs identified by theoptical line ratio diagnostic are hosted by real bulges. The pseudobulgefraction significantly decreases with AGN signature as the line ratios changefrom indicating pure star formation ($\sim 54 \pm 4$ \%), to composite of starformation and AGN ($\sim 18 \pm 3$\%), and to AGN-dominated galaxies ($\sim 5\pm 3$\%). Using the dust-corrected [\ion{O}{3}] luminosity as an AGN accretionindicator, and the stellar mass and radius as proxies for a black hole mass, wefind that AGNs in real bulges have lower Eddington ratios than AGNs inpseudobulges. Real bulges have a wide range of AGN and star formationactivities, although most of them are weak AGNs. For both bulge-types, theirEddington ratios are correlated with specific star formation rates (SSFR). Realbulges have lower specific accretion rate but higher AGN fraction thanpseudobulges do at similar SSFRs.

The Activation of Galactic Nuclei and Their Accretion Rates are Linked to the Star Formation Rates and Bulge-types of Their Host Galaxies