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

Abstract

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.

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

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Cited by in corpus (11)

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• Profile morphology and polarization of young pulsars
• Distances, Radial Distribution and Total Number of Galactic Supernova Remnants
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• A Complete Catalogue of Dusty Supernova Remnants
• Discovery of a New X-ray Filled Radio Supernova Remnant Around the Pulsar Wind Nebula in 3EG J1809-2328
• PSR J1410-6132: A young, energetic pulsar associated with EGRET source 3EG J1410-6147
• The Age Evolution of the Radio Morphology of Supernova Remnants
• Cross-match between the latest Swift-BAT and Fermi-LAT catalogs
• Multifrequency Strategies for the Identification of Gamma-Ray Sources
• Analysis of the possible detection of the pulsar wind nebulae of PSR J1208-6238, J1341-6220, J1838-0537 and J1844-0346