  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 $n_et = 6 (4, 9) \times 10^{10}$ 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).
