VLA and ALMA Briggs-weighted (robust 0) images of Antares at frequencies between 3 and 405 GHz. The optically thin emission from the ionized cavity in the outer wind of Antares is caused by the UV radiation field of its hot B-type companion and is not detected in our images above 11 GHz. The size and shape of the restoring beam at each frequency is shown in the lower left corner of each image. Contour levels are set to (5, 10, 20, 30, 40, 60, 80, 200, 300, 400) × σ_rms and (5, 100, 300, 600, 900, 1200, 2100) × σ_rms for the VLA and ALMA images, respectively. The dashed box in panel 1 indicates the region depicted in panels 7–14.