et al. 2003). This result, together with the finding that the black hole mass, M$_{\rm BH}$, and the host galaxy’s stellar velocity dispersion, $\sigma$, is strongly correlated (Gebhardt et al. 2000; Ferrarese & Merritt 2000), has led to the general consensus that black hole formation and growth is fundamentally connected to the build-up of galaxy bulges. Indeed, it has been proposed that feedback from the AGN regulates the surrounding star formation in the host galaxy (e.g. Silk & Rees 1998; Kauffmann & Haehnelt 2000). However, an important outstanding question remains unresolved: [*is a bulge in general a necessary ingredient for a black hole to form and grow*]{}? On the one hand, M33, the best studied nearby bulgeless galaxy, shows no evidence of a supermassive black hole (SBH), and the upper limit on the mass is significantly below that predicted by the M$_{\rm BH}$-$\sigma$ relation established in early-type galaxies (Gebhardt et al. 2001; Merritt et al. 2001). On the other hand, both NGC 4395 (Filippenko & Ho 2003) and POX52 (Barth et al. 2004) show no evidence for a bulge and yet do contain AGN. However, these two galaxies have remained isolated cases of bulgeless galaxies with accreting black holes, suggesting 