X-Ray Emission from the Radio Pulsar PSR J1105−6107

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Abstract
We have detected significant X-ray emission from the direction of the young radio pulsar PSR J1105-6107 using the ASCA observatory. The 11 σ detection includes 459 background-subtracted source counts derived using data from all four ASCA detectors. The emission shows no evidence of pulsations; the pulsed fraction is less than 31%, at the 90% confidence level. The X-ray emission can be characterized by a power-law spectrum with photon index α=1.8±0.4, for a neutral hydrogen column density NH = 7 × 1021 cm-2. The unabsorbed 2-10 keV flux assuming the power-law model is (6.4±0.8) × 10−13 ergs cm-2 s-1. The implied efficiency for conversion of spin-down luminosity to ASCA-band emission is (1.6±0.2) × 10−3, assuming a distance of 7 kpc to the source. Within the limited statistics, the source is consistent with being unresolved. We argue that the X-rays are best explained as originating from a pulsar-powered synchrotron nebula.
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