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Mapping the orbital obliquity distribution of young planets is one avenuetowards understanding mechanisms that sculpt the architectures of planetarysystems. TOI-942 is a young field star, with an age of ~60 Myr, hosting aplanetary system consisting of two transiting Neptune-sized planets in 4.3- and10.1-day period orbits. We observed the spectroscopic transits of the innerNeptune TOI-942b to determine its projected orbital obliquity angle. Throughtwo partial transits, we find the planet to be in a prograde orbit, with aprojected obliquity angle of |lambda| = 1/+41-33 deg. In addition,incorporating the light curve and the stellar rotation period, we find the truethree-dimensional obliquity to be 2/+27-23 deg. We explored various sources ofuncertainties specific to the spectroscopic transits of planets around youngactive stars, and showed that our reported obliquity uncertainty fullyencompassed these effects. TOI-942b is one of the youngest planets to have itsobliquity characterized, and one of even fewer residing in a multi-planetsystem. The prograde orbital geometry of TOI-942b is in line with systems ofsimilar ages, none of which have yet been identified to be in stronglymisaligned orbits.

TOI-942b: A Prograde Neptune in a ~60 Myr old Multi-transiting System