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We present complicated dust structures within multiple regions of thecandidate supernova remnant (SNR) the `Tornado' (G357.7-0.1) using observationswith Spitzer and Herschel. We use Point Process Mapping, PPMAP, to investigatethe distribution of dust in the Tornado at a resolution of 8", compared to thenative telescope beams of 5-36". We find complex dust structures at multipletemperatures within both the head and the tail of the Tornado, ranging from 15to 60K. Cool dust in the head forms a shell, with some overlap with the radioemission, which envelopes warm dust at the X-ray peak. Akin to the terrestrialsandy whirlwinds known as `Dust Devils', we find a large mass of dust containedwithin the Tornado. We derive a total dust mass for the Tornado head of 16.7solar masses, assuming a dust absorption coefficient of kappa_300 =0.56m^2kg^1, which can be explained by interstellar material swept up by a SNRexpanding in a dense region. The X-ray, infra-red, and radio emission from theTornado head indicate that this is a SNR. The origin of the tail is moreunclear, although we propose that there is an X-ray binary embedded in the SNR,the outflow from which drives into the SNR shell. This interaction forms thehelical tail structure in a similar manner to that of the SNR W50 andmicroquasar SS433.

A Galactic Dust Devil: far-infrared observations of the Tornado Supernova Remnant candidate