We study nine S0–Sb galaxies with ( photometric ) bulges consisting of two distinct components .
The outer component is a flattened , kinematically cool , disklike structure : a “ disky pseudobulge ” .
Embedded inside is a rounder , kinematically hot spheroid : a “ classical bulge ” .
This indicates that pseudobulges and classical bulges are not mutually exclusive : some galaxies have both .

The disky pseudobulges almost always have an exponential disk ( scale lengths = 125–870 pc , mean \sim 440 pc ) with disk-related subcomponents : nuclear rings , bars , and/or spiral arms .
They constitute 11–59 % of the galaxy stellar mass ( mean PB / T = 0.33 ) , with stellar masses \sim 7 \times 10 ^ { 9 } – 9 \times 10 ^ { 10 } \mathrm { M } _ { \sun } .
Classical-bulge components have Sérsic indices of 0.9–2.2 , effective radii of 25–430 pc and stellar masses of 5 \times 10 ^ { 8 } – 3 \times 10 ^ { 10 } \mathrm { M } _ { \sun } ( usually < 10 % of the galaxy ’ s stellar mass ; mean B / T = 0.06 ) .
The classical bulges show rotation , but are kinematically hotter than the disky pseudobulges .
Dynamical modeling of three systems indicates that velocity dispersions are isotropic in the classical bulges and equatorially biased in the disky pseudobulges .

In the mass–radius and mass–stellar mass density planes , classical-bulge components follow sequences defined by ellipticals and ( larger ) classical bulges .
Disky pseudobulges also fall on this sequence ; they are more compact than similar-mass large-scale disks .
Although some classical bulges are quite compact , they are distinct from nuclear star clusters in both size and mass , and coexist with nuclear clusters in at least two galaxies .

Since almost all the galaxies in this study are barred , they probably also host boxy/peanut-shaped bulges ( vertically thickened inner parts of bars ) .
NGC 3368 shows evidence for such a zone outside its disky pseudobulge , making it a galaxy with all three types of “ bulge ” .