Skip to content
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
A Galactic dust devil: Far-infrared observations of the Tornado supernova remnant candidate
Monthly Notices of the Royal Astronomical Society, Volume 499, No. 4, Year 2020
Notification
URL copied to clipboard!
Description
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 arcsec, compared to the native telescope beams of 5-36 arcsec. 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 = 0.56 m2 kg-1, which can be explained by interstellar material swept up by a SNR expanding in a dense region. The X-ray, infrared, 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 SS 433. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Authors & Co-Authors
Chawner, Hannah
United Kingdom, Cardiff
Cardiff University
Gomez, Haley L.
United Kingdom, Cardiff
Cardiff University
Matsuura, Mikako
United Kingdom, Cardiff
Cardiff University
Priestley, Felix D.
United Kingdom, Cardiff
Cardiff University
Barlow, M. J.
United Kingdom, London
University College London
de Looze, Ilse
United Kingdom, London
University College London
Belgium, Ghent
Universiteit Gent
Papageorgiou, Andreas
United Kingdom, Cardiff
Cardiff University
Smith, Matthew W.L.
United Kingdom, Cardiff
Cardiff University
Rho, Jeonghee
United States, Mountain View
Seti Institute
Dunne, Loretta
United Kingdom, Cardiff
Cardiff University
Statistics
Citations: 5
Authors: 10
Affiliations: 6
Identifiers
Doi:
10.1093/mnras/staa2925
ISSN:
00358711
Research Areas
Environmental
Study Locations
Multi-countries