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We present 35 ks Chandra ACIS observations of the 42 Myr old radio pulsar PSRB1451-68. A point source is detected 0.32" +/- 0.73" from the expected radiopulsar position. It has ~200 counts in the 0.3-8 keV energy range. We identifythis point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 islocated close to a 2MASS point source, for which we derive 7% as the upperlimit on the flux contribution to the measured pulsar X-ray flux. The pulsarspectrum can be described by either a power-law model with photon indexGamma=2.4 (+0.4/-0.3) and a unrealistically high absorbing column density N(H)=(2.5 (+1.2/-1.3)) * 10^(21) cm^-2, or by a combination of a kT=0.35(+0.12/-0.07) keV blackbody and a Gamma = 1.4 +/- 0.5 power-law component forN(H)[DM]= 2.6 * 10^(20) cm^-2, estimated from the pulsar dispersion measure. Atthe parallactic, Lutz-Kelker bias corrected distance of 480 pc, the non-thermalX-ray luminosities in the 0.3-8 keV energy band are either Lx(nonth)= (11.3 +/-1.7) * 10^(29) erg/s or Lx(nonth)= (5.9 (+4.9/-5.0)) * 10^(29) erg/s,respectively. This corresponds to non-thermal X-ray efficiencies of eithereta(nonth)= Lx(nonth) / (dE/dt) ~ 0.005 or 0.003, respectively.

Chandra observations of the old pulsar PSR B1451-68