We report the first XMM detection of the SNR candidate G337.2+0.1 ( =AX J1635.9 - 4719 ) .
The object shows centrally filled and diffuse X-ray emission .
The emission peaks in the hard 3.0 - 10.0 keV band .
A spatially resolved spectral study confirms that the column density of the central part of the SNR is about N _ { H } \sim 5.9 ( \pm 1.5 ) \times 10 ^ { 22 } cm ^ { -2 } and its X-ray spectrum is well represented by a single power-law with a photon index \Gamma =0.96 \pm 0.56 .
The non-detection of line emission in the central spectrum is consistent with synchrotron radiation from a population of relativistic electrons .
Detailed spectral analysis indicates that the outer region is highly absorbed and quite softer than the inner region , with N _ { H } \sim 16.2 ( \pm 5.2 ) \times 10 ^ { 22 } cm ^ { -2 } and kT=4.4 ( \pm 2.8 ) keV .
Such characteristics are already observed in other X-ray plerions .
Based on the morphological and spectral X-ray information , we confirm the SNR nature of G337.2+0.1 , and suggest that the central region of the source is a pulsar wind nebula ( PWN ) , originated by an energetic though yet undetected pulsar , that is currently losing energy at a rate of \sim 10 ^ { 36 } erg s ^ { -1 } .