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In exoplanetary systems, the interaction between the central star and theplanet can trigger Auroral Radio Emission (ARE), due to the Electron CyclotronMaser mechanism. The high brightness temperature of this emission makes itvisible at large distances, opening new opportunities to study exoplanets andto search for favourable conditions for the development of extra-terrestriallife, as magnetic fields act as a shield that protects life against externalparticles and influences the evolution of the planetary atmospheres. In thelast few years, we started an observational campaign to observe a sample ofnearby M-type stars known to host exoplanets with the aim to detect ARE. Weobserved YZ Ceti with the upgraded Giant Metrewave Radio Telescope (uGMRT) inband 4 (550-900 MHz) nine times over a period of five months. We detected radioemission four times, two of which with high degree of circular polarization.With statistical considerations we exclude the possibility of flares due tostellar magnetic activity. Instead, when folding the detections to the orbitalphase of the closest planet YZ Cet b, they are at positions where we wouldexpect ARE due to star-planet interaction (SPI) in sub-Alfvenic regime. With adegree of confidence higher than 4.37 sigma, YZ Cet is the first extrasolarsystems with confirmed SPI at radio wavelengths. Modelling the ARE, we estimatea magnetic field for the star of about 2.4 kG and we find that the planet musthave a magnetosphere. The lower limit for the polar magnetic field of theplanet is 0.4 G.

Star-Planet Interaction at radio wavelengths in YZ Ceti: Inferring planetary magnetic field