Predicted flux density arising at a nominal frequency of 670 MHz from SPI. The yellow (cross-hatched) areas correspond to the expected radio flux density, including (neglecting) free-free absorption from the thermal electrons in the stellar wind. The rows correspond to the expected emission for two different values of the coronal temperature, T_c= 4.7 MK (the nominal value; top row) and T_c= 2.5 MK (3σ lower limit; bottom row). The left and middle panels show the predicted flux density as a function of the stellar wind mass-loss rate for an unmagnetized planet (left) and a magnetized one with B_pl= 0.85 G (middle), with a vertical dashed line showing the nominal value, ${\dot{M}}_{\star }$ = 1.4 ${\dot{M}}_{\odot }$ (see text for details). The right panels show the predicted flux density as a function of the planetary magnetic field for the aforementioned nominal value of ${\dot{M}}_{\star }$, and a vertical dashed line corresponds to the nominal value of the magnetic field, B_pl= 0.85 G. Red areas correspond to values M_A ≥ 1, that is, where the planet is in the super-Alfvénic regime; therefore model predictions are not valid. The horizontal dash-dotted lines correspond to the 3σ detection threshold of our observations (where σ = 30 μJy b⁻¹).