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We have used the full radial extent of images from the Hubble SpaceTelescope's Advanced Camera for Surveys and Wide Field Planetary Camera 2 toextract surface brightness profiles from a sample of six, local lenticulargalaxy candidates. We have modelled these profiles using a core-Sersic bulgeplus an exponential disk model. Our lenticular disk galaxies with bulgemagnitudes M_V < ~ -21.30 mag have central stellar deficits, suggesting thatthese bulges may have formed from `dry' merger events involving supermassiveblack holes while their surrounding disk was subsequently built up, perhaps viacold gas accretion scenarios. The central stellar mass deficits M_def areroughly 0.5 to 2 M_BH (black hole mass), rather than ~ 10 to 20 M_BH as claimedfrom some past studies, which is in accord with core-Sersic model mass deficitmeasurements in elliptical galaxies. Furthermore, these bulges have Sersicindices n ~ 3, half light radii R_e < 2 kpc and masses > 10^11 M_sun, andtherefore appear to be descendants of the compact galaxies reported at z ~ 1.5to 2. Past studies which have searched for these local counterparts by usingsingle-component galaxy models to provide the z ~ 0 size comparisons haveover-looked these dense, compact and massive bulges in today's early-type diskgalaxies. This evolutionary scenario not only accounts for what are todaygenerally old bulges---which must be present in z ~ 1.5 images---residing inwhat are generally young disks, but it eliminates the uncomfortable suggestionof a factor of 3 to 5 growth in size for the compact, z ~ 1.5 galaxies that areknown to possess infant disks.

Central Stellar Mass Deficits in the Bulges of Local Lenticular Galaxies, and the Connection with Compact z ~ 1.5 Galaxies