  There are no strong constraints placed thus far on the amplitude of internal
gravity waves (IGWs) that are stochastically excited in the radiative interiors
of solar-type stars. Late F-type stars have relatively thin convective
envelopes with fast convective flows and tend to be fast rotators compared to
solar-type stars of later spectral types. These two elements are expected to
directly impact the IGW excitation rates and properties. We want to estimate
the amplitude of stochastically excited gravity modes (g-modes) in F-type stars
for different rotational regimes. We used the ASH code to perform 3D
simulations of deep-shell models of 1.3 $M_\odot$ F-type solar-type stars,
including the radiative interior and the shallow convective envelope. The IGWs
are excited by interface interactions between convective plumes and the top of
the radiative interior. We were able to characterise the IGWs and g-mode
properties in the radiative interior, and we compared these properties using
the computation from the 1D oscillation code GYRE. The amplitude of
low-frequency modes is significantly higher in fast-rotating models and the
evolution of the period spacing of consecutive modes exhibits evidence of a
behaviour that is modified by the influence of the Coriolis force. For our
fastest rotating model, we were able to detect the intermediate degree g-mode
signature near the top of the simulation domain. Nevertheless, the predicted
luminosity perturbations from individual modes still remain at small
amplitudes. We obtained mode amplitudes that are several orders of magnitude
higher than those of prior 3D simulations of solar models. Our simulations
suggest that g-mode signatures could be detectable in late F-type stars.
[abridged]
