  During the first Gyr of their life, exoplanet atmospheres suffer from
different atmospheric escape phenomena that can strongly affect the shape and
morphology of the exoplanet itself. These processes can be studied with
Ly$\alpha$, H$\alpha$ and/or He I triplet observations. We present
high-resolution spectroscopy observations from CARMENES and GIARPS checking for
He I and H$\alpha$ signals in 20 exoplanetary atmospheres: V1298Tau c, K2-100b,
HD63433b, HD63433c, HD73583b, HD73583c, K2-77b, TOI-2076b, TOI-2048b,
HD235088b, TOI-1807b, TOI-1136d, TOI-1268b, TOI-1683b, TOI-2018b, MASCARA-2b,
WASP-189b, TOI-2046b, TOI-1431b, and HAT-P-57b. We report two new
high-resolution spectroscopy He I detections for TOI-1268b and TOI-2018b, and
an H$\alpha$ detection for TOI-1136d. The MOPYS (Measuring Out-flows in Planets
orbiting Young Stars) project aims to understand the evaporating phenomena and
test their predictions from the current observations. We compiled a list of 70
exoplanets with He I and/or H$\alpha$ observations, from this work and the
literature, and we considered the He I and H$\alpha$ results as proxy for
atmospheric escape. Our principal results are that 0.1-1Gyr-old planets do not
exhibit more He I or H$\alpha$ detections than older planets, and evaporation
signals are more frequent for planets orbiting $\sim$1-3Gyr-old stars. We
provide new constrains to the cosmic shoreline, the empirical division between
rocky planets and planets with atmosphere, by using the evaporation detections
and explore the capabilities of a new dimensionless parameter, $R_{\rm
He}/R_{\rm Hill}$, to explain the He I triplet detections. Furthermore, we
present a statistically significant upper boundary for the He I triplet
detections in the $T_{\rm eq}$ vs $\rho_{\rm p}$ parameter space. Planets
located above that boundary are unlikely to show He I absorption signals.
