We present the results of the first XMM-Newton observation of the interacting type IIn supernova 1995N , performed in July 2003 .
We find that the 0.2–10.0 keV unabsorbed flux dropped at a value of \simeq 1.8 \times 10 ^ { -13 } erg cm ^ { -2 } s ^ { -1 } , almost one order of magnitude lower than that of a previous ASCA observation of January 1998 .
From all the available X-ray measurements , an interesting scenario emerges where the X-ray light emission may be produced by a two-phase ( clumpy/smooth ) CSM .
The X-ray spectral analysis shows statistically significant evidence for the presence of two distinct components , that can be modeled with emission from optically thin , thermal plasmas at different temperatures .
The exponent of the ejecta density distribution inferred from these temperatures is n \simeq 6.4 .
From the fluxes of the two spectral components we derive an estimate of the mass loss rate of the supernova progenitor , { \dot { M } } \sim 2 \times 10 ^ { -4 } M _ { \odot } { yr } ^ { -1 } , at the upper end of the interval exhibited by red super-giants .
Coordinated optical and infrared observations allow us to reconstruct the simultaneous infrared to X-ray flux distribution of SN 1995N .
We find that , at \sim 9 years after explosion , the direct X-ray thermal emission due to the wind/ejecta interaction is \sim 5 times larger than the total reprocessed IR/optical flux .