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AU Mic~b is a Neptune size planet on a 8.47-day orbit around the nearestpre-main sequence ($\sim$20 Myr) star to the Sun, the bright (V=8.81) M dwarfAU Mic. The planet was preliminary detected in Doppler radial velocity timeseries and recently confirmed to be transiting with data from the TESS mission.AU Mic~b is likely to be cooling and contracting and might be accompanied by asecond, more massive planet, in an outer orbit. Here, we present theobservations of the transit of AU Mic~b using ESPRESSO on the VLT. We obtaineda high-resolution time series of spectra to measure the Rossiter-McLaughlineffect and constrain the spin-orbit alignment of the star and planet, andsimultaneously attempt to retrieve the planet's atmospheric transmissionspectrum. These observations allow us to study for the first time the earlyphases of the dynamical evolution of young systems. We apply differentmethodologies to derive the spin-orbit angle of AU Mic~b, and all of themretrieve values consistent with the planet being aligned with the rotationplane of the star. We determine a conservative spin-orbit angle $\lambda$ valueof $-2.96^{+10.44}_{-10.30}$, indicative that the formation and migration ofthe planets of the AU Mic system occurred within the disk. Unfortunately, anddespite the large SNR of our measurements, the degree of stellar activityprevented us from detecting any features from the planetary atmosphere. Infact, our results suggest that transmission spectroscopy for recently formedplanets around active young stars is going to remain very challenging, if atall possible, for the near future.

Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic