Wolf-Rayet (WR) stars are massive late stage stars with broad emission lines. Wolf-Rayet stars follow an evolutionary cycle that is identifiable by their previous mass–loss history, where mass-loss outbursts are inconsistent and caused by internal pulsations. Bradley et al. present the first radio–continuum detection of the circumstellar shell around the well-known Wolf-Rayet star WR16 at 943.5 MHz using the ASKAP Evolutionary Map of the Universe (EMU) survey. Combining the ASKAP data with previous ATCA measurements at 2.4, 4.8, and 8.6 GHz, yields a spectral index of α = +0.7, indicating thermal emission. We propose that the shell and star both exhibit thermal emission, supported by the its appearance in near-infrared and Hα observations. The latest Gaia parallax is used to determine a distance of 2.28±0.09 kpc. This star is well known for its surrounding circular nebulosity, and using the distance and an angular diameter of 8.4 arcminutes, the team determine the shell size to be 5.6 parsecs. They use the Gaia proper motion of WR16 to determine that the peculiar tangential velocity of the star is 51±7 km/s in a north-west direction. Using this proper motion to determine the shell’s origin, they estimate an age of around 9500 years, and determine its average expansion velocity to be about 280 km/s. The image above shows the EMU detection of WR16 and its inner shell at 943.5 MHz. The image is linearly scaled and the 15 arcsecond beam size is presented by the small white circle in the bottom-left of the image. The white square indicates the position of WR16, the dashed circle shows the position of the ‘inner’ circular shell. The dashed polygons labelled 1 and 2 indicate the position of ‘outer’ shell remnants.