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11th of October 2016
Molecular Shocks and the Gamma-ray Clouds of the W28 Supernova Remnant
by Nigel Maxted (UNSW)
The W28 supernova remnant complex in three images. The top left image shows the radio continuum emission (red) from electrons inside the W28 shell. The supernova remnant is interacting with molecular gas seen in CO(2-1) ( magenta contours). The densest gas is traced by CS(1-0) (green) and corresponds to high energy gamma-ray emission (cyan contours), which strongly suggests that cosmic rays have been accelerated and are interacting in the region. On the right is a zoomed-in image of the molecular gas directly shocked by W28. In addition to shock-tracing SiO emission (red) at the border of thermal X-rays (blue) emitted by shock-heated gas, signatures of a shock may be present in multiple inversion transition lines of the NH3 molecule (one transition is shown in green). The bottom-left image is an illustration of a cosmic-ray diffusion scenario that is consistent with multi-wavelength observations of the W28 region. More detailed descriptions of images/results are presented in Maxted et al (2016, submitted).

Reference: Nigel Maxted, Gavin Rowell, Phoebe de Wilt, Michael Burton, Catherine Braiding, Andrew Walsh, Yasuo Fukui, Akiko Kawamura 2016, American Institute of Physics Conference Series, submitted (astro-ph/1610-00865).

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