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the discovery that the _ cos - b _ gamma - ray source was a pulsar ( psr b1706 - 44 ) was made by johnston et al ( 1992 ) .
mcadam , osborne , & parkinson ( 1993 ) published a map made by the most telescope at 843  mhz of the area around the gamma - ray source .
it showed a semicircular arc of emission , which has subsequently been denoted as the supernova remnant ( snr ) g343.1 - 2.3 , with the pulsar seemingly embedded in a small feature at its south eastern extremity .
it was argued that the approximate distance of 3  kpc for the remnant , derived from the surface brightness - diameter relationship ( @xmath0-d ) was not incompatible with the pulsar s dispersion measure , although the distance indicated by the widely used interstellar electron density model of taylor & cordes ( 1993 ) would be only 1.8  kpc .
the @xmath0-d relationship was based on the flux values from single dish observations , as both the vla and the most integrated flux fell short of what would be expected from these ( mcadam et al 1993 ) .    if the association of the pulsar and the supernova remnant were real a transverse velocity of @xmath1  kms@xmath2
would be required for the pulsar to have moved from the approximate geometric centre of the snr arc in the characteristic spin down time of 17  kyr .
this is a high value but not the highest measured value for a pulsar nor as high as that implied for some seemingly well - established pulsar - snr associations .
frail , goss , & whiteoak ( 1994 ) mapped the area around the pulsar at 20  cm and 90  cm with the vla and cast some doubt on it s association with g343.1 - 2.3 based on the morphology , and the argument that the dispersion measure and @xmath0-d distance were discrepant .
the latter was subsequently countered by a 21  cm hydrogen line absorption measurement of the pulsar by koribalski et  al .
( 1995 ) which gives a distance range of 2.4 to 3.2  kpc .
nicastro , johnston , & koribalski ( 1996 ) also argue against the association .
they report a maximum value only 27  kms@xmath2 for the magnitude of the transverse velocity of the pulsar calculated from the interstellar scintillation .
however in both dodson ( 1997 ) and then their later paper ( johnston , nicastro , & koribalski 1998 ) this estimate is revised up to 100  kms@xmath2 .
the possibility of a direct determination of the proper motion of psr b1706 - 44 has been investigated , but no phase reference sufficiently strong for the current australian vlbi network ( the lba ) could be found .
we have made a number of radio images of the remnant to determine its full extent .
these are with mrt at 150  mhz , with the atca at 1400  mhz and at 6.6  ghz with the 26 m dish at mt pleasant observatory , hobart .
the object as seen at 150  mhz , and at 6.6  ghz are shown in figure [ fig : mrt+mtp ] .
the 150-mhz map is a preliminary result from the mrt all sky survey .
the 6.6-ghz image was produced as part of the honours thesis of m. howlett ( howlett 1998 ) , a survey along the galactic plane using the 26 m antenna run by the university of tasmania .
both contain all spatial frequencies up to their resolution .
they both show broad extended structure to the south of the bright arc seen by most .
the australia telescope compact array has been use to re - observe g343.1 - 2.3 , with a nineteen pointing mosaic .
mosaicing was required to cover the extent of the source , but also to assist in the recovery of the flux on the shortest _ uv _ spacings , which were missed in the most and the vla observations .
the images in figure [ fig : at_i ] a ) , look very much like those of most and indeed have very similar resolution ( @xmath3 ) ( the longer baselines , to the 6 km antenna , were not used due to their poor support ) .
we have included as a constraint in the deconvolution the observed total flux for the snr , 30 jy , as seen with the 26 m single dish in hobart .
figure [ fig : at_i ] b ) shows the polarisation angle overlaid on the polarised intensity .
the polarised fraction is typically about 20 per cent and the polarisation angle is randomly orientated and changes rapidly around the bright ring .
wisps of polarised emission can be seen to extend beyond the ring as originally defined , and throughout the region with broadscale emission .
this confirms that the broadscale emission is associated with the synchrotron emission from the snr .
it is instructive to compare the vla maps of figure 4 in frail et al ( 1994 ) with the map in figure [ fig : at_i ] a ) .
the spur of emission on which the pulsar lies is clearly a continuous feature covering more than @xmath4 .
this makes it extremely unlikely to be a cometary tail from the pulsar .
furthermore the width of the spur , @xmath5 , is unlikely to be that due to ram pressure of a moving pulsar .
it is intriguing this approximately the size that would be expected from a static pulsar wind , i.e. the sedov equations with a continuous input of energy , with the @xmath6 of psr1706 - 44 ( rees & gunn 1974 ) .
the arguments against the association were based around kaspi s critia ( kaspi 1996 ) .
these were that the pulsar dm distance and the snr @xmath0-d distance did not match , and the pulsar was at the edge of the snr and had too low a velocity to have travelled from the geometric centre of the snr .
also there was no morphological evidence to imply a velocity direction .
it has turned out that it is the dm distance is incorrect , and the extent of the snr has been underestimated .
it is clear from both the low total flux values found by the most and vla maps that there is a smooth broad component to this snr .
the atca observations confirm the extent of the broad emission , and that this is syncrotron in character . taking this smooth component as the true limits of the snr enlarges the extent and moves it southwards .
this places the pulsar psr1706 - 44 within the snr shell , rather than on the rim .
we expect a snr to be associated with psr1706 - 44 because of its youth .
the association was rejected in the past , and we have shown that the grounds for the rejection are not compelling as previously believed . the question of the pulsar velocity could be resolved by finding a phase reference for vlbi observation , with either the ska or an upgrade to the current lba .
we will be able to rule out the upper velocity limits with the atca within the next few years but will not be able to measure to the lower limits for a few decades .
the association of g343.1 - 2.3 and psr 1706 - 44 has been controversial from its first proposal . in this paper 
 we present new evidence from images made by with the australia telescope compact array ( atca ) , mrt and mt . 
 pleasant . to cover the full extent of g343.1 - 2.3 with atca mosaicing was required , and we present the polarisation images from this experiment . 
 the atca observations confirms the much larger extent of the snr , which now encompasses the pulsar .    
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