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[Abridged] The study of disc kinematics has recently opened up as a promisingmethod to detect unseen planets. However, a systematic, statisticallymeaningful analysis of such an approach remains missing. The aim of this workis to devise an automated, statistically robust technique to identifykinematical perturbations induced by the presence of planets in a gas disc, andto accurately infer their location. For this purpose, we produce hydrosimulations of planet-disc interactions with different planet masses, 0.3, 1.0and 3.0 $M_{Jup}$, at a radius of $R=100$ au in the disc, and perform radiativetransfer calculations of CO to simulate observables for 13 planet azimuths.Using the DISCMINER package, we fit the synthetic data cubes with a Keplerianmodel of the channel-by-channel emission to study line profile differences,including deviations from Keplerian rotation. The detection technique, based online centroid differences, captures localised planet-driven perturbations, andcan distinguish them from axisymmetric velocity perturbations. The method candetect all three simulated planets, at all azimuths, with an average accuracyof $\pm3^\circ$ in azimuth and $\pm8$ au in radius. Owing to disc structure andline-of-sight projection effects, planets at azimuths close to $\pm45^\circ$yield the highest velocity fluctuations, whereas those at limiting cases,$0^\circ$ and $\pm90^\circ$, drive the lowest. The observed peak velocitiesrange within 40$-$70, 70$-$170 and 130$-$450 m s$^{-1}$ for 0.3, 1.0 and 3.0$M_{Jup}$ planets. Our analysis indicates that the variance of peak velocitiesis boosted near planets due to organised gas motions prompted by theirlocalised gravitational well. We propose an approach that exploits thisvelocity coherence to provide, for the first time, statistically significantdetections of localised planet-driven perturbations in the gas disc kinematics.

The Disc Miner I: A statistical framework to detect and quantify kinematical perturbations driven by young planets in discs