The supernova remnant (SNR) candidate was identified as a faint shell in the MGPS-2 survey. We followed up on it with multi-wavelength observations, confirming it to be an SNR at a high Galactic latitude that shows spatially coinciding γ-ray emission. We conducted the first detailed investigation of the radio emission from the region, aiming to characterise the radio structure, polarisation measurements, and the coinciding GeV emission. We used recent radio continuum observations at from the EMU and POSSUM surveys with ASKAP, as well as 16. 5 years of 943. 5 observations. We furthermore considered the multi-wavelength context of the object by investigating observations previously conducted with other instruments, such as IR and X-ray surveys. We confirm that _ is indeed an SNR, which we have dubbed We detect the presence of a faint, extended (diameter) bilateral radio shell with an ASKAP radio flux density of 1. 5^ 30 +1. 5 -0. 1, with no obvious IR counterparts. With a radio surface brightness of about 2. 4^ +2. 4 _ -0. 1 -22, , it is is one of the faintest radio SNRs known. The northern part of the shell shows linearly polarised radio emission, which is characteristic of synchrotron emission in SNRs. The physical size of the SNR is estimated to be around 42^ +42 _ -21, , which would correspond to a distance of around 4. 9^ pc +4. 9 _ -2. 5,. Furthermore, the spatially coincident γ-ray source 4FGL, J1413. 9--6705 shows an energy flux of įlo pc 1. 26 with a significance of between and. We placed 5. 7 100 100 in context with other known high-latitude SNRs with γ-ray counterparts and compared their observational properties. New radio surveys are discovering a population of faint high-Galactic-latitude SNRs with GeV counterparts in isolated environments. More sensitive observations with the CTAO in the next few years should provide valuable insights into particle acceleration and escape in these important cosmic ray accelerators.
Burger-Scheidlin et al. (Wed,) studied this question.