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Spectropolarimetry of supernova remnant G296.5 + 10.0

Published online by Cambridge University Press:  01 November 2008

Lisa Harvey-Smith ,
Bryan M. Gaensler ,
C.-Y. Ng  and
Anne J. Green
Lisa Harvey-Smith
Affiliation:
Sydney Institute for Astronomy (SIFA), School of Physics, The University of Sydney, NSW 2006, Australia. email: lhs@usyd.edu.au
Bryan M. Gaensler
Affiliation:
Sydney Institute for Astronomy (SIFA), School of Physics, The University of Sydney, NSW 2006, Australia. email: lhs@usyd.edu.au
C.-Y. Ng
Affiliation:
Sydney Institute for Astronomy (SIFA), School of Physics, The University of Sydney, NSW 2006, Australia. email: lhs@usyd.edu.au
Anne J. Green
Affiliation:
Sydney Institute for Astronomy (SIFA), School of Physics, The University of Sydney, NSW 2006, Australia. email: lhs@usyd.edu.au
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Abstract

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Radio continuum emission from the supernova remnant G296.5 + 10.0 was observed using the Australia Telescope Compact Array. Using a 104 MHz bandwidth split into 13 × 8 MHz spectral channels, it was possible to produce a pixel-by-pixel image of Rotation Measure (RM) across the entire remnant. A lack of correlation between RM and X-ray surface brightness reveals that the RMs originate from outside the remnant. Using this information, we will characterise the smooth component of the magnetic field within the supernova remnant and attempt to probe the magneto-ionic structure and turbulent scale sizes in the ISM and galactic halo along the line-of-sight.

Keywords

Polarization – magnetic fields – ISM: supernova remnants – ISM: radio continuum – X-rays: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 141 - 144
Copyright
Copyright © International Astronomical Union 2009

References

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