  Kn-band images, unsharp-masked images, as well as major-axis and vertically-
summed surface brightness profiles are presented for 30 edge-on spiral
galaxies, most with a boxy or peanut-shaped (B/PS) bulge. Such galaxies have
more complex morphologies than galaxies of other bulge types, more often
showing (off-)centered X structures, secondary major-axis maxima and
spiral-like structures. Those features are also observed in N-body simulations
of barred discs and may trace the main bar orbit families. The surface
brightness profiles of galaxies with a B/PS bulge are also more complex, with
typically 3 or more clearly separated regions, including a flat intermediate
region (Freeman Type II profiles). Those radial breaks offer evidence for
bar-driven transfer of angular momentum and radial redistribution of material.
The profiles also suggest a rapid variation of the scaleheight of the disc
material, contrary to conventional wisdom but again as expected from vertical
resonances and instabilities in barred discs. The steep inner region of the
surface brightness profiles is often shorter than the isophotally thick part of
the galaxies, itself always shorter than the flat region of the profiles.
Contrary to the standard `bulge + disc' model, we thus propose that galaxies
with a B/PS bulge are composed of a thin concentrated disc (a disc-like bulge)
contained within a partially thick bar (the B/PS bulge) and a thin outer disc.
The inner disc likely formed secularly through bar-driven processes and is
responsible for the steep inner region of the surface brightness profiles,
while the bar is responsible for the flat region and the thick complex
morphological structures observed. Those components are strongly coupled
dynamically and are formed mostly of the same (disc) material. [Abridged]
