Spectropolarimetry of SNR G296.5+10.0

TL;DR

This study uses spectropolarimetric radio observations to map the magnetic field structure of supernova remnant G296.5+10.0, revealing external origins of rotation measures and insights into the interstellar medium's magneto-ionic properties.

Contribution

It provides the first pixel-by-pixel RM map of G296.5+10.0, enabling analysis of the remnant's magnetic field and the surrounding interstellar medium's turbulence.

Findings

RM originates outside the remnant, not correlated with X-ray brightness

Characterized the smooth magnetic field component within the remnant

Probed magneto-ionic structure and turbulence scales in the ISM and galactic halo

Abstract

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 x 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.