Galactic synchrotron emissivity measurements between 250° < l < 355° from the GLEAM survey with the MWA

Abstract

Synchrotron emission pervades the Galactic plane at low radio frequencies, originating from cosmic ray electrons interacting with the Galactic magnetic field. Using a low-frequency radio telescope, the Murchison Widefield Array (MWA), we measure the free-free absorption of this Galactic synchrotron emission by intervening HII regions along the line of sight. These absorption measurements allow us to calculate the Galactic cosmic-ray electron emissivity behind and in front of 47 detected HII regions in the region $250^{\circ }<l<355^{\circ }$, $|b|<2^{\circ }$. We find that all average emissivities between the HII regions and the Galactic edge along the line of sight ($\hat{I}{\mu }_b$) are in the range of 0.24$\sim$0.70Kpc${}^{-1}$ with a mean of 0.40Kpc${}^{-1}$ and a variance of 0.10Kpc${}^{-1}$ at 88MHz. Our best model, the Two-circle model, divides the Galactic disk into three regions using two circles centring on the Galactic centre. It shows a high emissivity region near the Galactic centre, a low emissivity region near the Galactic edge, and a medium emissivity region between these two regions, contrary to the trend found by previous studies.

12 pages, 8 figures. Published on MNRAS. A conversion factor is corrected in this version. For the original published version, see https://academic.oup.com/mnras/article-abstract/465/3/3163/2544366/Galactic-synchrotron-emissivity-measurements?redirectedFrom=fulltext For its erratum, see https://academic.oup.com/mnras/article-abstract/472/1/828/4083643/Erratum-Galactic-synchrotron-emissivity