  Using a deep Chandra AO-1 observation of the face-on spiral galaxy M101, we
examine three of five previously optically-identified X-ray sources which are
spatially correlated with optical supernova remnants (MF54, MF57, and MF83).
The X-ray fluxes from these objects, if due to diffuse emission from the
remnants, are bright enough to require a new class of objects, with the
possible attribution by Wang to diffuse emission from hypernova remnants. Of
the three, MF83 was considered the most likely candidate for such an object due
to its size, nature, and close positional coincidence. However, we find that
MF83 is clearly ruled out as a hypernova remnant by both its temporal
variability and spectrum. The bright X-ray sources previously associated with
MF54 and MF57 are seen by Chandra to be clearly offset from the optical
positions of the supernova remnants by several arc seconds, confirming a result
suggested by the previous work. MF54 does have a faint X-ray counterpart,
however, with a luminosity and temperature consistent with a normal supernova
remnant of its size. The most likely classifications of the sources are as
X-ray binaries. Although counting statistics are limited, over the 0.3--5.0 keV
spectral band the data are well fit by simple absorbed power laws with
luminosities in the 10^38 to 10^39 ergs/s range. The power law indices are
softer than those of Milky Way LMXB of similar luminosities, and are more
consistent with those of the Large Magellanic Cloud. Both the high luminosity
and the soft spectral shape favor these being accreting black hole binaries in
high soft states.
