We present 35ks Chandra ACIS observations of the 42Myr old radio pulsar PSR B1451-68. A point source is detected 0″.32 ± 0″.73 from the expected radio pulsar position. It has ∼200 counts in the 0.3-8keV energy range. We identify this point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 is located close to a Two Micron All Sky Survey point source for which we derive 7% as the upper limit on the flux contribution to the measured pulsar X-ray flux. The pulsar spectrum can be described by either a power-law model with photon index Γ = 2.4+0.4 -0.3 and a unrealistically high absorbing column density N H = (2.5 +1.2 - 1.3) × 1021cm-2, or by a combination of a kT = 0.35+0.12 - 0.07 keV blackbody and a Γ = 1.4 ± 0.5 power-law component for N DM H = 2.6 × 1020cm-2, estimated from the pulsar dispersion measure. At the parallactic, a Lutz-Kelker bias corrected distance of 480pc, the non-thermal X-ray luminosities in the 0.3-8keV energy band are either L nonth 0.3-8 keV = (11.3 ± 1.7) × 1029ergs-1 or L nonth 0.3-8 keV = (5.9+4.9 - 5.0) × 10 29ergs-1, respectively. This corresponds to non-thermal X-ray efficiencies of either or νnonth0.38 keV= L nonth0.38keV/Ė ∼ 5 × 10?3 or 10-3, respectively.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science