This paper presents a BeppoSAX observation of NGC 7582 made during 1998 November and an optical spectrum taken in 1998 October .
The new X-ray data reveal a previously unknown hard X-ray component in NGC 7582 , peaking close to 20 keV .
Rapid variability is observed with correlated changes in the 5-10 and 13-60 keV bands indicating that a single continuum component , produced by the active nucleus , provides the dominant flux across both bands .
Comparison between RXTE and BeppoSAX data reveals changes in the 2 – 10 keV flux on timescales of months .
Changes in the nuclear X-ray flux appear unrelated to the gradual decline in optical flux noted since the high-state in 1998 July .
The 0.5 – 2 keV flux of NGC 7582 is not significantly variable within the BeppoSAX observation , but has brightened by a factor of \sim 2 since the ASCA observation of 1994 .
While there is some concern about contamination from spatially-unresolved sources , the long-term variability in soft X-ray flux seems most likely associated with the nucleus or an event within the host galaxy of NGC 7582 .

The 2 – 100 keV spectrum is well fit by a powerlaw of photon index \Gamma = 1.95 ^ { +0.09 } _ { -0.18 } , steeper by \Delta \Gamma \simeq 0.40 than the index during the 1994 ASCA observation .
The X-ray continuum is attenuated by a thick absorber of N _ { H } \sim 1.6 \times 10 ^ { 24 } { cm ^ { -2 } } covering \sim 60 ^ { +10 } _ { -14 } \% of the nucleus plus a screen with N _ { H } \sim 1.4 \times 10 ^ { 23 } { cm ^ { -2 } } covering the entire nucleus .
Comparison of the BeppoSAX and ASCA spectra shows an increase in the full screen by \Delta N _ { H } \simeq 7 \times 10 ^ { 22 } { cm ^ { -2 } } since 1994 , confirming the absorption variability found by Xue et al .
The increase in soft X-ray flux between 1994 and 1998 is consistent with the appearance of holes in the full screen allowing \mathrel { \hbox { \raise 2.15 pt \hbox { $ < $ } \hbox to 0.0 pt { \lower 2.15 pt \hbox { $ \sim$% } } } } 1 % of the nuclear flux to escape , and producing some clear lines-of-sight to the broad-line-region .
The data are also consistent with the scenario suggested by Aretxaga et al , of the radiative onset of a type IIn supernova causing the observed optical change in NGC 7582 .