%ALeung, James%AMurphy, Tara%AGhirlanda, Giancarlo%AKaplan, David%ALenc, Emil%ADobie, Dougal%ABanfield, Julie%AHale, Catherine%AHotan, Aidan%AMcConnell, David%AMoss, Vanessa%APritchard, Joshua%ARaja, Wasim%AStewart, Adam%AWhiting, Matthew%Anull Ed.%BJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 503; Journal Issue: 2 %D2021%I %JJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 503; Journal Issue: 2 %K %MOSTI ID: 10294251 %PMedium: X %TA search for radio afterglows from gamma-ray bursts with the Australian Square Kilometre Array Pathfinder %XABSTRACT We present a search for radio afterglows from long gamma-ray bursts using the Australian Square Kilometre Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, covering the entire celestial sphere south of declination +41○, and three epochs of the Variables and Slow Transients Pilot Survey (Phase 1), covering ∼5000 square degrees per epoch. The observations we used from these surveys spanned a nine-month period from 2019 April 21 to 2020 January 11. We cross-matched radio sources found in these surveys with 779 well-localized (to ≤15 arcsec) long gamma-ray bursts occurring after 2004 and determined whether the associations were more likely afterglow- or host-related through the analysis of optical images. In our search, we detected one radio afterglow candidate associated with GRB 171205A, a local low-luminosity gamma-ray burst with a supernova counterpart SN 2017iuk, in an ASKAP observation 511 d post-burst. We confirmed this detection with further observations of the radio afterglow using the Australia Telescope Compact Array at 859 and 884 d post-burst. Combining this data with archival data from early-time radio observations, we showed the evolution of the radio spectral energy distribution alone could reveal clear signatures of a wind-like circumburst medium for the burst. Finally, we derived semi-analytical estimates for the microphysical shock parameters of the burst: electron power-law index p = 2.84, normalized wind-density parameter A* = 3, fractional energy in electrons ϵe = 0.3, and fractional energy in magnetic fields ϵB = 0.0002. %0Journal Article