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New candidate radio supernova remnants detected in the GLEAM survey over 345° < l < 60°, 180° < l < 240°

  • N. Hurley-Walker (a1), M. D. Filipović (a2), B. M. Gaensler (a3) (a4), D. A. Leahy (a5), P. J. Hancock (a1) (a6), T. M. O. Franzen (a7), A. R. Offringa (a7), J. R. Callingham (a7), L. Hindson (a8), C. Wu (a9), M. E. Bell (a10), B.-Q. For (a3) (a9), M. Johnston-Hollitt (a1), A. D. Kapińska (a11), J. Morgan (a1), T. Murphy (a6) (a12), B. McKinley (a1), P. Procopio (a6) (a13), L. Staveley-Smith (a3) (a9), R. B. Wayth (a1) (a6) and Q. Zheng (a14)...

Abstract

We have detected 27 new supernova remnants (SNRs) using a new data release of the GLEAM survey from the Murchison Widefield Array telescope, including the lowest surface brightness SNR ever detected, G 0.1 – 9.7. Our method uses spectral fitting to the radio continuum to derive spectral indices for 26/27 candidates, and our low-frequency observations probe a steeper spectrum population than previously discovered. None of the candidates have coincident WISE mid-IR emission, further showing that the emission is non-thermal. Using pulsar associations we derive physical properties for six candidate SNRs, finding G 0.1 – 9.7 may be younger than 10 kyr. Sixty per cent of the candidates subtend areas larger than 0.2 deg2 on the sky, compared to < 25% of previously detected SNRs. We also make the first detection of two SNRs in the Galactic longitude range 220°–240°.

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Corresponding author

Author for correspondence: Natasha Hurley-Walker, Email: nhw@icrar.org

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Keywords

New candidate radio supernova remnants detected in the GLEAM survey over 345° < l < 60°, 180° < l < 240°

  • N. Hurley-Walker (a1), M. D. Filipović (a2), B. M. Gaensler (a3) (a4), D. A. Leahy (a5), P. J. Hancock (a1) (a6), T. M. O. Franzen (a7), A. R. Offringa (a7), J. R. Callingham (a7), L. Hindson (a8), C. Wu (a9), M. E. Bell (a10), B.-Q. For (a3) (a9), M. Johnston-Hollitt (a1), A. D. Kapińska (a11), J. Morgan (a1), T. Murphy (a6) (a12), B. McKinley (a1), P. Procopio (a6) (a13), L. Staveley-Smith (a3) (a9), R. B. Wayth (a1) (a6) and Q. Zheng (a14)...

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