Asteroseismic measurements of stellar internal rotation from the space-based missions /Kepler/ and CoRoT provided the first constraints on the efficiency of internal angular momentum (AM) transport with a sample of about a hundred solar-like main-sequence (MS) stars.However, the short lifetimes of the acoustic resonant modes excited in these stars, combined with their slow rotation have prevented placing tight constraints on the internal rotation of these stars. Moreover, the current observational sample of solar-like MS stars with a large enough signal-to-noise ratio to measure precise rotational splittings, especially in the lower mass range 0.8 - 1.0 $M_{\odot}$, is reduced to a handful of stars. The upcoming ESA PLATO mission promises to deliver thousands of solar-like MS stars, characterised with high-precision asteroseismology. Using data from the /Kepler /mission observations and rotating stellar evolutionary models as a reference, we explore the detectability of radial differential rotation in the PLATO sample and discuss methods to improve the current constraints. In this context, we discuss a new method to study the probability distribution of population-level parameters of the internal rotation profile in an ensemble of similar stars. This could allow to combine information from multiple similar targets and leverage the larger sample that will be delivered by PLATO.
