The association of G343.1-2.3 and PSR B1706-44 has been controversial from its first proposal. In this paper we address the difficulties, and argue that the association is still likely. New evidence comes from images of G343.1-2.3 obtained using the Australia Telescope Compact Array (ATCA), and of the pulsar obtained using the Chandra X-ray observatory. Mosaicking was required to cover the full extent of G343.1-2.3, and we present the polarization images from this experiment. Also an X-ray pulsar wind nebula has been found in the archived Chandra observations, with the correct morphology to support the association. The ATCA observations confirm the much larger extent of the supernova remnant, which now encompasses the pulsar. The X-ray morphology points back toward the centre of the supernova remnant, indicating the direction of the proper motion, and that the pulsar and supernova remnant are associated.