Structure of Brightest Cluster Galaxies and Intracluster Light
  Observations of 170 local ($z\lesssim0.08$) galaxy clusters in the northern
hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager
(WWFI). We correct for systematic effects such as point-spread function
broadening, foreground star contamination, relative bias offsets, and charge
persistence. Background inhomogeneities induced by scattered light are reduced
down to $\Delta {\rm SB} > 31~g'$ mag arcsec$^{-2}$ by large dithering and
subtraction of night-sky flats. Residual background inhomogeneities brighter
than ${\rm SB}_{\sigma}< 27.6~g'$ mag arcsec$^{-2}$ caused by galactic cirrus
are detected in front of 23% of the clusters. However, the large field of view
allows discrimination between accretion signatures and galactic cirrus. We
detect accretion signatures in the form of tidal streams in 22%, shells in
9.4%, and multiple nuclei in 47% of the Brightest Cluster Galaxies (BCGs) and
find two BCGs in 7% of the clusters. We measure semimajor-axis surface
brightness profiles of the BCGs and their surrounding Intracluster Light (ICL)
down to a limiting surface brightness of ${\rm SB} = 30~g'$ mag arcsec$^{-2}$.
The spatial resolution in the inner regions is increased by combining the WWFI
light profiles with those that we measured from archival \textit{Hubble Space
Telescope} images or deconvolved WWFI images. We find that 71% of the BCG+ICL
systems have surface brightness (SB) profiles that are well described by a
single S\'ersic (SS) function, whereas 29% require a double S\'ersic (DS)
function to obtain a good fit. We find that BCGs have scaling relations that
differ markedly from those of normal ellipticals, likely due to their
indistinguishable embedding in the ICL.
