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A Dynamical Study of the Young Oxygen-Rich Supernova Remnant in the Small Magellanic Cloud

Published online by Cambridge University Press:  04 August 2017

Ian R. Tuohy  and
Michael A. Dopita
Ian R. Tuohy
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
Michael A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University

Extract

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We present a velocity map of the young oxygen-rich supernova remnant (1E0102.2–7219) in the Small Magellanic Cloud, obtained with the Anglo-Australian Telescope. The velocity structure is complex, and implies a high degree of asymmetry during the Type II supernova explosion. Our data can be modelled geometrically in terms of a severely distorted ring of oxygen-rich ejecta. This result, together with the evidence for expanding rings in similar remnants, suggests non-spherical ejection to be an intrinsic characteristic of Type II supernovae. We have also obtained two-dimensional spectroscopy of the diffuse halo of emission which partially surrounds 1E0102.2–7219. The halo exhibits the high excitation line of HeII λ4686, and is either a fossil HII region created by a UV flash accompanying the supernova, or alternately, is being excited by intense UV radiation from the remnant itself. It is the first clear association of a high excitation region with a supernova remnant.

Type
I. Young Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 165 - 169
Copyright
Copyright © Reidel 1983 

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