  Dwarf galaxies are dominated by dark matter even in the innermost regions
and, therefore, provide excellent probes for the investigation of dark halos.
To that purpose, we analyse ROSAT PSPC-data of the dwarf galaxy NGC 247. We
focus in particular on the diffuse X-ray emission in the $1/4 $keV band.
Assuming an isothermal density profile, we find that the mass of the hot
emitting gas is about $10^8 {\rm M_{\odot}}$, corresponding to $\lesssim 0.5%$
of the total dynamical mass of the galaxy. The total mass of NGC 247, as
derived from the X-ray data agrees quite well with the value obtained from the
measured rotation curve (Burlak). The X-ray profile in the $3/4 $keV and $1.5
$keV band shows an excess at a radial distance of about $15 $ arcmin from the
center. Such a ``hump'' in the radial X-ray profile can be explained by the
presence of a cluster of young low mass stars or brown dwarfs. Therefore, NGC
247 offers the possibility to observe the formation of a halo of MACHOs.
