  We investigate the clustering properties and close neighbour counts for
galaxies with different types of bulges and stellar masses. We select samples
of "classical" and "pseudo" bulges, as well as "bulge-less" disk galaxies,
based on the bulge/disk decomposition catalog of SDSS galaxies provided by
Simard et al. (2011). For a given galaxy sample we estimate: the projected
two-point cross-correlation function with respect to a spectroscopic reference
sample, w_p(r_p), and the average background-subtracted neighbour count within
a projected separation using a photometric reference sample, N_neighbour(<r_p).
We compare the results with the measurements of control samples matched in
color, concentration and redshift. We find that, when limited to a certain
stellar mass range and matched in color and concentration, all the samples
present similar clustering amplitudes and neighbour counts on scales above
~0.1h^{-1}Mpc. This indicates that neither the presence of a central bulge, nor
the bulge type is related to intermediate-to-large scale environments. On
smaller scales, in contrast, pseudo-bulge and pure-disk galaxies similarly show
strong excess in close neighbour count when compared to control galaxies, at
all masses probed. For classical bulges, small-scale excess is also observed
but only for M_stars < 10^{10} M_sun; at higher masses, their neighbour counts
are similar to that of control galaxies at all scales. These results imply
strong connections between galactic bulges and galaxy-galaxy interactions in
the local Universe, although it is unclear how they are physically linked in
the current theory of galaxy formation.
