A search for the radio counterpart of the unidentified γ - ray source 3 EG J 1410 − 6147

We have made radio continuum, H i and X-ray observations in the direction of the unidentified EGRET source 3EG J1410−6147, using the Australia Telescope Compact Array and the Chandra X-ray Observatory. The observations encompass the supernova remnant (SNR) G312.4–0.4 and the two young pulsars PSRs J1412–6145 and J1413– 6141. We derive a lower distance limit of 6 kpc to the SNR, although interpretation of positive velocity features in the H i spectrum may imply the SNR is more distant than 14 kpc. PSR J1412–6145, with an age of 50 kyr, is the pulsar most likely associated with SNR G312.4–0.4. X-rays are not detected from either pulsar and diffuse X-ray emission near the bright western edge of the SNR is weak. Although there is circumstantial evidence that this western region is a pulsar wind nebula (PWN), the embedded pulsar PSR J1412–6145 is apparently not sufficiently powerful to explain the radio enhancement. The origin of the electron acceleration in this region and of the γ-rays remain unidentified, unless the distance to PSR J1413–6141 is at least a factor of 3 lower than its dispersion measure distance.