Radio spectral energy distribution for Pollux between 1 and 300 GHz. The red dash-dotted line is the expected blackbody emission assuming a uniform intensity disk with angular diameter φ = φ_⋆ and brightness temperature T_b = T_eff. The black filled circles are the VLA detections at 21.2 and 9 GHz. The blue dotted line is the expected spectral energy distribution of Pollux using the model atmosphere from Sim (2001). Our 3 GHz upper limit is also shown along with previous upper limits taken from Wendker (1995). The black dashed line represents a least-square fit to our detections assuming that S_ν ∝ ν^α.