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Detecting and characterising exoworlds around very young stars (age$<$10 Myr)are key aspects of exoplanet demographic studies, especially for understandingthe mechanisms and timescales of planet formation and migration. However,detection using the radial velocity method alone can be very challenging, sincethe amplitude of the signals due to magnetic activity of such stars can beorders of magnitude larger than those induced even by massive planets. Weobserved the very young ($\sim$2 Myr) and very active star V830 Tau with theHARPS-N spectrograph to independently confirm and characterise the previouslyreported hot Jupiter V830 Tau b ($K_{\rm b}=68\pm11$ m/s; $m_{\rm b}sini_{\rmb}=0.57\pm0.10$ $M_{jup}$; $P_{\rm b}=4.927\pm0.008$ d). Due to the observed$\sim$1 km/s radial velocity scatter clearly attributable to V830 Tau'smagnetic activity, we analysed radial velocities extracted with differentpipelines and modelled them using several state-of-the-art tools. We devisedinjection-recovery simulations to support our results and characterise ourdetection limits. The analysis of the radial velocities was aided by usingsimultaneous photometric and spectroscopic diagnostics. Despite the highquality of our HARPS-N data and the diversity of tests we performed, we couldnot detect the planet V830 Tau b in our data and confirm its existence. Oursimulations show that a statistically-significant detection of the claimedplanetary Doppler signal is very challenging. Much as it is important tocontinue Doppler searches for planets around young stars, utmost care must betaken in the attempt to overcome the technical difficulties to be faced inorder to achieve their detection and characterisation. This point must be keptin mind when assessing their occurrence rate, formation mechanisms andmigration pathways, especially without evidence of their existence fromphotometric transits.

The GAPS Programme at TNG XXVII. Reassessment of a young planetary system with HARPS-N: is the hot Jupiter V830 Tau b really there?