Smeaton et al. present the discovery of possibly the youngest Galactic supernova remnant (SNR) with associated pulsar-wind nebula (PWN), which they name Perun (G329.9−0.5). Perun was serendipitously discovered in the ASKAP-EMU survey at 943 MHz, and subsequent follow-up observations were conducted with the Australia Telescope Compact Array observatory at 5500 and 9000 MHz. These data were combined with additional radio observations from the MeerKAT, Molonglo Observatory Synthesis Telescope, and Murchison Widefield Array telescopes, infrared (IR) observations from the Spitzer Space Telescope, and X-ray observations from the Chandra X-ray observatory to perform a multifrequency analysis. The radio morphology shows a small angular size shell (D = 70 arcsec) with a luminous, central PWN. Crucial evidence for Perun’s SNR classification comes from the detection of linear fractional polarization at radio frequencies of 7~10% with both radial and tangential orientations, similar to the young SNR G1.9+0.3. Data from the Southern Galactic Plane Survey is used to perform an HI (neutral hydrogen) analysis and estimate a favoured distance range of 6–9 kpc, and thus a favoured age range of ∼70–500 yr. The image above is a composite RGB image where the total intensity map of Perun, observed by ASKAP at 944 MHz, is in red and blue and Spitzer 24μm IR map is in green.