  We report the results of a 50 ks Chandra observation of the recently
discovered radio object G141.2+5.0, presumed to be a pulsar-wind nebula. We
find a moderately bright unresolved X-ray source which we designate CXOU
J033712.8 615302 coincident with the central peak radio emission. An absorbed
power-law fit to the 241 counts describes the data well, with absorbing column
$N_H = 6.7 (4.0, 9.7) \times 10^{21}$ cm$^{-2}$ and photon index $\Gamma = 1.8
(1.4, 2.2)$. For a distance of 4 kpc, the unabsorbed luminosity between 0.5 and
8 keV is $ 1.7^{+0.4}_{-0.3} \times 10^{32}$ erg s$^{-1}$ (90\% confidence
intervals). Both $L_X$ and $\Gamma$ are quite typical of pulsars in PWNe. No
extended emission is seen; we estimate a conservative $3 \sigma$ upper limit to
the surface brightness of any X-ray PWN near the point source to be $3 \times
10^{-17}$ erg cm$^{-2}$ s$^{-1}$ arcsec$^{-2}$ between 0.5 and 8 keV, assuming
the same spectrum as the point source; for a nebula of diameter $13"$, the flux
limit is 6\% of the flux of the point source. The steep radio spectrum of the
PWN ($\alpha \sim -0.7$), if continued to the X-ray without a break, predicts
$L_X\ \rm{(nebula)} \sim 1 \times 10^{33}$ erg s$^{-1}$, so additional spectral
steepening between radio and X-rays is required, as is true of all known PWNe.
The high Galactic latitude gives a $z$-distance of 350 pc above the Galactic
plane, quite unusual for a Population I object.
