We present a study of a young ( few years old ) supernova remnant 2003lx which was first discovered in X-ray through two serendipitous Swift observations in 2008 January and the corresponding merged image revealed a 7 \sigma source detection at 2.1 \pm 1.2 arcsec ( 0.9 \pm 0.5 Swift pixels ) from the optical position of the supernova .
The X-ray luminosity L _ { x } = 4.8 _ { -1.7 } ^ { +1.8 } \times 10 ^ { 41 } ergs s ^ { -1 } of band 0.3 - 2.0 keV is estimated by a redshift z = 0.0377 power law which can infer a companion star with a mass-loss rate of \dot { M } \sim 10 ^ { -4 } M _ { \sun } yr ^ { -1 } ( with assumption of wind velocity v _ { w } = 10 km s ^ { -1 } ) in the white dwarf binary system .
Thermal Model fitting suggests the temperature of the shock wave front is kT \sim 0.4 keV which is consistent with the typical reverse shock temperate .
The X-ray emission allows us to probe the interaction between the fast moving debris of the exploded star and the circumstellar medium ( CSM ) .
This in turns provides footprints of the mass-loss history of the exploded system , and may allow us to learn about the nature of the progenitor and its companion .