  Helioseismology and asteroseismology of red giant stars have shown that the
distribution of angular momentum in stellar interiors, and its evolution with
time remains an open issue in stellar physics. Owing to the unprecedented
quality of Kepler photometry, we are able to seismically infer internal
rotation rates in \gamma Doradus stars, which provide the MS counterpart to the
red-giants puzzle. We confront these internal rotation rates to stellar
evolution models with rotationally induced transport of angular momentum, in
order to test angular momentum transport mechanisms. We used a stellar
model-independent method developed by Christophe et al. in order to obtain
seismically inferred, buoyancy radii and near-core rotation for 37 \gamma
Doradus stars observed by Kepler. We show that the buoyancy radius can be used
as a reliable evolution indicator for field stars on the MS. We computed
rotating evolutionary models including transport of angular momentum in
radiative zones, following Zahn and Maeder, with the CESTAM code. This code
calculates the rotational history of stars from the birth line to the tip of
the RGB. The initial angular momentum content has to be set initially, which is
done by fitting rotation periods in young stellar clusters. We show a clear
disagreement between the near-core rotation rates measured in the sample and
the rotation rates obtained from evolutionary models including rotationally
induced transport following Zahn (1992). These results show a disagreement
similar to that of the Sun and red giant stars. This suggests the existence of
missing mechanisms responsible for the braking of the core before and along the
MS. The efficiency of the missing mechanisms is investigated. The transport of
angular momentum as formalized by Zahn and Maeder cannot explain the
measurements of near-core rotation in main-sequence intermediate-mass stars we
have at hand.
