Can we measure the rotation rate inside stars ?

We examine the possibility of obtaining localized information on the rotation rate inside stars through asteroseismic observations from space. Attention is focused on δ Scuti stars where both opacity-driven and solar-like turbulence-driven modes may be detected. Plausible sets of modes with attendant rotational splitting data are deduced from the results of linear stability calculations, effects of amplitude averaging for modes with higher l's, and information gathered from ground-based photometry. For such sets of modes, optimally localized averaging kernels are constructed, and we show that fairly detailed information about the behavior of the rotation rate can be obtained only if opacity-driven modes like those anticipated are indeed detected. The turbulence-driven modes are essentially irrelevant for probing rotation.