  We present the results of the Suzaku observation of the Seyfert 2 galaxy NGC
4507. This source is one of the X-ray brightest Compton-thin Seyfert 2s and a
candidate for a variable absorber. Suzaku caught NGC 4507 in a highly absorbed
state characterised by a high column density (NH \sim8 x10^23 cm^-2), a strong
reflected component (R\sim 1.9) and a high equivalent width Fe K alpha emission
line (EW\sim 500 eV). The Fe K alpha emission line is unresolved at the
resolution of the Suzaku CCDs (sigma < 30 eV or FWHM < 3000 km s^-1) and most
likely originates in a distant absorber. The Fe K beta emission line is also
clearly detected and its intensity is marginally higher than the theoretical
value for low ionisation Fe. A comparison with previous observations performed
with XMM-Newton and BeppoSAX reveals that the X-ray spectral curvature changes
on a timescale of a few months. We analysed all these historical observations,
with standard models as well as with a most recent model for a toroidal
reprocessor and found that the main driver of the observed 2-10 keV spectral
variability is a change of the line-of-sight obscuration, varying from
\sim4x10^23 cm^-2 to \sim9 x 10^23 cm^-2. The primary continuum is also
variable, although its photon index does not appear to vary, while the Fe K
alpha line and reflection component are consistent with being constant across
the observations. This suggests the presence of a rather constant reprocessor
and that the observed line of sight NH variability is either due to a certain
degree of clumpiness of the putative torus or due to the presence of a second
clumpy absorber.
