A search for the radio counterpart of the unidentified gamma-ray source 3EG J1410-6147

Details A search for the radio counterpart of the unidentified gamma-ray source 3EG J1410-6147 A search for the radio counterpart of the unidentified gamma-ray source 3EG J1410-6147

2002-11-12

arxiv.org/abs/astro-ph/0211246v2

Mon.Not.Roy.Astron.Soc. 339 (2003) 1048

Astronomy and Astrophysics

Astrophysics

10 pages, plus 5 jpeg figures, MNRAS, in press. Full postscript or pdf including all figures is available at http://www.ast.ca

Scientific paper

10.1046/j.1365-8711.2003.06265.x

We have made radio continuum, HI 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 HI 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 gamma-rays remain unidentified, unless the distance to PSR J1413-6141 is at least a factor of 3 lower than its dispersion measure distance.

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