  Detecting and understanding rotation in stellar interiors is nowadays one of
the unsolved problems in stellar physics. Asteroseismology has been able to
provide insights on rotation for the Sun, solar-like stars, and compact objects
like white dwarfs. However, this is still very difficult for intermediate-mass
stars. These stars are moderate-to-rapid rotators. Rotation splits and shifts
the oscillation modes, which makes the oscillation spectrum more complex and
harder to interpret. Here we study the oscillation patterns of a sample of
benchmark $\delta$~Sct stars belonging to eclipsing binary systems with the
objective to find the frequency spacing related to the rotational splitting
($\delta r$). For this task, we combine three techniques: the Fourier
transform, the autocorrelation function, and the histogram of frequency
differences. The last two showed a similar behaviour. For most of the stars, it
was necessary to determine the large separation ($\Delta\nu$) prior to spot
$\delta r$. This is the first time we may clearly state that one of the
periodicities present in the p~modes oscillation spectra of $\delta$~Sct stars
corresponds to the rotational splitting. This is true independently of the
stellar rotation rate. These promising results pave the way to find a robust
methodology to determine rotational splittings from the oscillation spectra of
$\delta$~Sct stars and, thus, understanding the rotational profile of
intermediate-mass pulsating stars.
