  A Chandra observation of the Large Magellanic Cloud supernova remnant DEM
L241 reveals an interior unresolved source which is probably an
accretion-powered binary. The optical counterpart is an O5III(f) star making
this a High-Mass X-ray Binary (HMXB) with orbital period likely to be of order
tens of days. Emission from the remnant interior is thermal and spectral
information is used to derive density and mass of the hot material. Elongation
of the remnant is unusual and possible causes of this are discussed. The
precursor star probably had mass > 25 solar masses
