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 ^ { \prime \prime } , 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 } ( 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 .