  Most of the information we have about the internal rotation of stars comes
from modes that are weakly affected by rotation, for example by using
rotational splittings. In contrast, we present here a method, based on the
asymptotic theory of Prat et al. (2016), which allows us to analyse the
signature of rotation where its effect is the most important, that is in
low-frequency gravity modes that are strongly affected by rotation. For such
modes, we predict two spectral patterns that could be confronted to observed
spectra and those computed using fully two-dimensional oscillation codes.
