  Inspecting all 1224 edge-on disk galaxies larger than 2' in the RC3 on DSS
images we have found several galaxies with extraordinary bulges meeting two
criteria: They are box shaped and large in respect to the diameters of their
galaxies. These bulges are often disturbed, show frequently prominent
irregularities and asymmetries, and some possess possible merger remnants or
merging satellites. For these bulges we have introduced the term "Thick Boxy
Bulges" (TBBs). About 2% of all disk galaxies (S0-Sd), respectively 4% of all
galaxies with box- and peanut-shaped (b/p) bulges, belong to this class of
galaxies. Using multicolour CCD and NIR data we have enlarged and followed up
our sample of nearly 20 galaxies with a TBB. The disturbed morphology of a
large fraction of these galaxies shows that many of the TBB galaxies are not
dynamically settled. For the TBBs the extent of the box shape seems to be too
large to result from a normal bar potential. Therefore we conclude that two
classes of b/p bulges exist with different origins. While most (~96%) b/p
bulges can be explained by bars alone, the extended boxy structures of TBBs
result most likely from accreted material by infalling satellite companions
(soft merging).
