Demographics of Bulge Types within 11 Mpc and Implications for Galaxy
  Evolution
  We present an inventory of galaxy bulge types (elliptical galaxy, classical
bulge, pseudobulge, and bulgeless galaxy) in a volume-limited sample within the
local 11 Mpc volume using Spitzer 3.6 micron and HST data. We find that whether
counting by number, star formation rate, or stellar mass, the dominant galaxy
type in the local universe has pure disk characteristics (either hosting a
pseudobulge or being bulgeless). Galaxies that contain either a pseudobulge or
no bulge combine to account for over 80% of the number of galaxies above a
stellar mass of 10^9 M_sun. Classical bulges and elliptical galaxies account
for ~1/4, and disks for ~3/4 of the stellar mass in the local 11 Mpc. About 2/3
of all star formation in the local volume takes place in galaxies with
pseudobulges. Looking at the fraction of galaxies with different bulge types as
a function of stellar mass, we find that the frequency of classical bulges
strongly increases with stellar mass, and comes to dominate above 10^{10.5}
M_sun. Galaxies with pseudobulges dominate at 10^{9.5}-10^{10.5} M_sun. Yet
lower-mass galaxies are most likely to be bulgeless. If pseudobulges are not a
product of mergers, then the frequency of pseudobulges in the local universe
poses a challenge for galaxy evolution models.
