  In recent years it has become clear that understanding the absorption present
in AGN is essential given its bearing on unification models. We present the
most recent XMM-Newton observation of Mrk 6, with the goal of understanding the
nature and origin of the complex absorption intrinsic to this source. X-ray
spectral fitting shows that a simple warm absorption model provides an equally
good statistical representation of the CCD data as a partial covering model.
Furthermore, once the RGS data are included in the spectral fitting, the simple
warm absorber model provides a very good fit to the data, without increasing
the complexity of the model, in contrast with the partial covering model which
requires the addition of either a low metalicity (<0.03 solar) thermal plasma
or low temperature blackbody emission in order to provide a similar quality
fit. The warm absorber is also a considerably more natural way to explain the
variability observed in the X-ray absorbing column density between the previous
XMM-Newton observation and this one, requiring only a second, higher column
density, higher ionisation, absorber to be present during the previous
XMM-Newton observation. In comparison, the partial covering models which
requires moving, clumpy, material relatively close to the source that result in
two distinct lines of sight, with separate absorbing columns that each vary
considerably without any associated change in their covering fractions, in
order to explain the observed variability. We associate the warm absorber
either with an accretion disk wind with densities of ~10^9 /cm^3, or with an
ionised `skin' or atmosphere of the molecular torus with densities of ~10^3 -
10^5 /cm^3.
