XMM-Newton Studies of the Supernova Remnant G350.0$-$2.0
  We report the results of XMM-Newton observations of the Galactic
mixed-morphology supernova remnant G350.0$-$2.0. Diffuse thermal X-ray emission
fills the north-western part of the remnant surrounded by radio shell-like
structures. We did not detect any X-ray counterpart of the latter structures,
but found several bright blobs within the diffuse emission. The X-ray spectrum
of the most part of the remnant can be described by a collisionally-ionized
plasma model VAPEC with solar abundances and a temperature of $\approx 0.8$
keV. The solar abundances of plasma indicate that the X-ray emission comes from
the shocked interstellar material. The overabundance of Fe was found in some of
the bright blobs. We also analysed the brightest point-like X-ray source 1RXS
J172653.4$-$382157 projected on the extended emission. Its spectrum is well
described by the two-temperature optically thin thermal plasma model MEKAL
typical for cataclysmic variable stars. The cataclysmic variable source nature
is supported by the presence of a faint ($g\approx21$) optical source with
non-stellar spectral energy distribution at the X-ray position of 1RXS
J172653.4$-$382157. It was detected with the XMM-Newton optical/UV monitor in
the $U$ filter and was also found in the archival H$\alpha$ and
optical/near-infrared broadband sky survey images. On the other hand, the X-ray
spectrum is also described by the power law plus thermal component model
typical for a rotation powered pulsar. Therefore, the pulsar interpretation of
the source cannot be excluded. For this source, we derived the upper limit for
the pulsed fraction of 27 per cent.
