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We present rest-frame $B$ and $I$ imaging of 35 low-redshift ($z < 0.5$)Palomar-Green quasars using the Hubble Space Telescope Wide Field Camera 3. Weperform multi-component two-dimensional image decomposition to separate thehost galaxy from its bright active nucleus, characterize its morphology, andmeasure its photometric properties. Special care is devoted to quantifying thestructural parameters of the galaxy bulge, determine its $B-I$ color, andestimate its stellar mass. Roughly half of the sample, comprising the lessluminous ($L_{5100} \lesssim 10^{45}\,\mathrm{erg\,s^{-1}}$) but most highEddington ratio quasars, reside in disk galaxies that are often barred andpossess pseudo bulges. The large stellar masses, large effective radii, andfaint surface brightnesses suggest that the host galaxies of the most luminousquasars are mostly ellipticals. Major mergers constitute only a minority($\lesssim 20\%$) of our sample. Our quasar sample roughly obeys the scalingrelations between black hole mass and host galaxy (bulge, core, total) stellarmass. Hosts with black holes more massive than $\sim 10^8\,M_\odot$ behavesimilarly to classical bulges and early-type galaxies, while those with lessmassive black holes, particular the narrow-line Seyfert 1s, are consistent withpseudo bulges in late-type galaxies. The host galaxy bulges, irrespective ofwhether they are classical or pseudo, follow the relatively tight inverserelation between effective radius and mean effective surface brightness ofinactive classical bulges and ellipticals. We argue that pseudo bulgesexperience recent or ongoing nuclear star formation.

The Diverse Morphology, Stellar Population, and Black Hole Scaling Relations of the Host Galaxies of Nearby Quasars