  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.
