We report the results of a search for a point X-ray source ( stellar remnant ) in the southwest protrusion of the supernova remnant G 315.4 - 2.30 ( MSH 14 - 6 3 , RCW 86 ) using the archival data of the Chandra X-ray Observatory .
The search was motivated by a hypothesis that G 315.4 - 2.30 is the result of an off-centered cavity supernova explosion of a moving massive star , which ended its evolution just near the edge of the main-sequence wind-driven bubble .
This hypothesis implies that the southwest protrusion in G 315.4 - 2.30 is the remainder of a pre-existing bow shock-like structure created by the interaction of the supernova progenitor ’ s wind with the interstellar medium and that the actual location of the supernova blast center is near the center of this hemispherical structure .
We have discovered two point X-ray sources in the “ proper ” place .
One of the sources has an optical counterpart with the photographic magnitude 13.38 \pm 0.40 , while the spectrum of the source can be fitted with an optically thin plasma model .
We interpret this source as a foreground active star of late spectral type .
The second source has no optical counterpart to a limiting magnitude \sim 21 .
The spectrum of this source can be fitted almost equally well with several simple models ( power law : photon index = 1.87 ; two-temperature blackbody : kT _ { 1 } = 0.11 keV , R _ { 1 } = 2.34 km and kT _ { 2 } = 0.71 keV , R _ { 2 } = 0.06 km ; blackbody plus power law : kT = 0.07 keV , photon index = 2.3 ) .
We interpret this source as a candidate stellar remnant ( neutron star ) , while the photon index and non-thermal luminosity of the source ( almost the same as those of the Vela pulsar and the recently discovered pulsar PSR J 0205 + 6449 in the supernova remnant 3C 58 ) suggest that it can be a young “ ordinary ” pulsar .