2000A&A...356...33R

We present BeppoSAX observations of the Seyfert 1.8 galaxy NGC 1365 in the 0.1-100keV range. The source was 6 times brighter than during an ASCA observation 3 years earlier. The 4-10keV flux is highly variable during the BeppoSAX observation, while the soft (0.1-4keV) emission is constant within the errors. Both a cold and a warm reflector and a cold absorber are required to explain the observed spectrum. The comparison between ASCA and BeppoSAX spectra strongly suggests that the circumnuclear material has a more complex structure than a simple homogeneous torus, with quite different absorbing gas columns along different lines of sight. A broad iron Kα line is also present in the spectrum, with the peak energy significantly redshifted. This can be explained by means of a relativistic disk line model. Alternatively, a warm absorption Fe line system with N_H≃10²³cm^–2 could account for the observed line profile.