Supermassive black holes do not correlate with galaxy disks or
  pseudobulges
  The masses of supermassive black holes are known to correlate with the
properties of the bulge components of their host galaxies. In contrast, they
appear not to correlate with galaxy disks. Disk-grown pseudobulges are
intermediate in properties between bulges and disks. It has been unclear
whether they do or do not correlate with black holes in the same way that
bulges do, because too few pseudobulges were classified to provide a clear
result. At stake are conclusions about which parts of galaxies coevolve with
black holes, possibly by being regulated by energy feedback from black holes.
Here we report pseudobulge classifications for galaxies with dynamically
detected black holes and combine them with recent measurements of velocity
dispersions in the biggest bulgeless galaxies. These data confirm that black
holes do not correlate with disks and show that they correlate little or not at
all with pseudobulges. We suggest that there are two different modes of black
hole feeding. Black holes in bulges grow rapidly to high masses when mergers
drive gas infall that feeds quasar-like events. In contrast, small black holes
in bulgeless galaxies and galaxies with pseudobulges grow as low-level
Seyferts. Growth of the former is driven by global processes, so the biggest
black holes coevolve with bulges, but growth of the latter is driven locally
and stochastically, and they do not coevolve with disks and pseudobulges.
