We present some arguments in support of the association of the pulsar PSR B1706-44 with the supernova remnant G343.1-2.3, based on the idea that these objects could be the result of a supernova explosion within a mushroom-like cavity (created by the supernova progenitor wind breaking out of the parent molecular cloud). We suggest that in addition to the known bright half of G343.1-2.3 there should exist a more extended and weaker component, such that the actual shape of G343.1-2.3 is similar to that of the well-known SNR VRO 42.05.01. We have found such a component in archival radio data.
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