Chawner, H., Howard, A. D. P., Gomez, H. L. ![]() ![]() ![]() ![]() ![]() |
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Abstract
We present complicated dust structures within multiple regions of the candidate supernova remnant (SNR) the ‘Tornado’ (G357.7−0.1) using observations with Spitzer and Herschel. We use Point Process Mapping, PPMAP, to investigate the distribution of dust in the Tornado at a resolution of 8″, compared to the native telescope beams of 5 − 36″. We find complex dust structures at multiple temperatures within both the head and the tail of the Tornado, ranging from 15 to 60 K. Cool dust in the head forms a shell, with some overlap with the radio emission, which envelopes warm dust at the X-ray peak. Akin to the terrestrial sandy whirlwinds known as ‘Dust Devils’, we find a large mass of dust contained within the Tornado. We derive a total dust mass for the Tornado head of 16.7 M⊙, assuming a dust absorption coefficient of κ300 =0.56m2kg−1, which can be explained by interstellar material swept up by a SNR expanding in a dense region. The X-ray, infra-red, and radio emission from the Tornado head indicate that this is a SNR. The origin of the tail is more unclear, 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 the helical tail structure in a similar manner to that of the SNR W50 and microquasar SS433.
Item Type: | Article |
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Date Type: | Publication |
Status: | Published |
Schools: | Advanced Research Computing @ Cardiff (ARCCA) Physics and Astronomy |
Publisher: | Oxford University Press |
ISSN: | 0035-8711 |
Date of First Compliant Deposit: | 17 September 2020 |
Date of Acceptance: | 16 September 2020 |
Last Modified: | 05 Nov 2024 22:15 |
URI: | https://orca.cardiff.ac.uk/id/eprint/134918 |
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