We present the results of a 32 ks Advanced Satellite for Cosmology and
Astrophysics (ASCA) observation of G11.2-0.3, which is by far the str
ongest candidate for the remnant of the historical supernova SN 386. A
center-brightened, hard, nonthermal X-ray source was found within the
remnant, which we interpret to be plerionic emission due to an embedd
ed pulsar. Our observations indicate that the remnant is a member of t
he class of ''composite'' remnants, as was hinted by previous observat
ions. The central emission is not pulsed down to a detection limit of
similar to 10(33) ergs s(-1). It could be that the putative pulsar is
not beamed in our direction. We also argue that the distance and surfa
ce brightness of G11.2-0.3 imply that the remnant is young and very li
kely to be the counterpart of the supernova observed by the Chinese in
A.D. 386, making it the youngest known Galactic composite. The possib
le similarity between the spectra of G11.2-0.3 and 3C 58, two of the y
oungest plerions, is brought out. These spectra are observed to be qui
te different from that of the Crab, which is very similar in age. Last
, we remark that only after a sustained observational effort spanning
two decades by various groups is the true nature of G11.2-0.3 at last
clear. To us this has been a valuable lesson that highlights the impor
tance of a detailed multiwavelength effort, with emphasis on high-freq
uency radio and X-ray spectral observations for proper classification
of remnants. The overabundance of pure shell remnants must be an artif
act of the lack of such observations and the selection effects that wo
rk against the discovery of plerions.