We identify the radio-emitting shell-type supernova remnant G15.9+0.2 as a relatively young remnant containing an X-ray point source that may be its associated neutron star .
The integrated spectrum of the remnant shell obtained from our 30 ks exploratory Chandra observation shows very strong lines that require elevated element abundances from ejecta , in particular of sulfur .
A plane-shock model fit gives a temperature kT = 0.9 ( 0.8 , 1.0 ) keV , an ionization timescale n _ { e } t = 6 ( 4 , 9 ) \times 10 ^ { 10 } cm ^ { -3 } s , and a sulfur abundance of 2.1 ( 1.7 , 2.7 ) times solar ( 90 % confidence limits ) .
Two-component models with one solar and one enriched component are also plausible , but are not well constrained by the data .
Various estimates give a remnant age of order 10 ^ { 3 } yr , which would make G15.9+0.2 among the dozen or so youngest remnants in the Galaxy .
The sparse point source spectrum is consistent with either a steep \Gamma \sim 4 power law or a kT \sim 0.4 keV blackbody .
The spectrum is absorbed by a H column density N _ { H } \sim 4 \times 10 ^ { 22 } cm ^ { -2 } similar to that required for the remnant shell .
The implied 2–9.5 keV source luminosity is about 10 ^ { 33 } ergs s ^ { -1 } for an assumed distance of 8.5 kpc consistent with the high absorption column .
We suggest that the point source is either a rotation-powered pulsar or a compact central object ( CCO ) .