  In this paper we present a new method for obtaining the optical
wavelength-dependent reddening function of planetary nebulae, using the nebular
and stellar continuum. The data used was a spectrum of NGC 6302 obtained with a
mean signal to noise of >10^2 A^-1 in the nebular continuum. With such a high
S/N the continuum can be accurately compared with a theoretical model nebular
plus stellar continuum. The nebular electron temperature and density used in
the model are determined using ratios of prominent emission lines. The
reddening function can then be obtained from the ratio of the theoretical and
the observed continuum. We find that for NGC 6302, the visible to IR extinction
law is indistinguishable from `standard' interstellar reddening, but that the
UV extinction curve is much steeper than normal, suggesting that more small
dust grains had been ejected into the nebula by the PN central star. Finally,
using the extinction law that we have determined, we present a complete
de--reddened line list of nearly 600 emission lines, and report on the
detection of the He(2-10) and He(2-8) Raman Features at 4331 A and 4852 A, and
the detection of Raman-Scattered OVI features at 6830 and 7087 AA.
