  Transport of angular momentum has been a challenging topic within the stellar
evolution community, even more since the recent asteroseismic surveys. All
published studies on rotation using asteroseismic observations show a
discrepancy between the observed and calculated rotation rates, indicating
there is an undetermined process of angular momentum transport active in these
stars. We aim to constrain the efficiency of this process by investigating
rotation rates of 2.5 M$_{\odot}$ stars. First, we investigated whether the
Tayler-Spruit dynamo could be responsible for the extra transport of angular
momentum for stars with an initial mass of 2.5 M$_{\odot}$. Then, by computing
rotating models including a constant additional artificial viscosity, we
determined the efficiency of the missing process of angular momentum transport
by comparing the models to the asteroseismic observations of core helium
burning stars. Parameter studies were performed to investigate the effect of
the stellar evolution code used, initial mass, and evolutionary stage. We
evolved our models into the white dwarf phase, and provide a comparison to
white dwarf rotation rates. The Tayler-Spruit dynamo is unable to provide
enough transport of angular momentum to reach the observed values of the core
helium burning stars investigated in this paper. We find that a value for the
additional artificial viscosity $\nu_{\rm{add}}$ around 10$^7$ cm$^2$ s$^{-1}$
provides enough transport of angular momentum. However, the rotational period
of these models is too high in the white dwarf phase to match the white dwarf
observations. From this comparison we infer that the efficiency of the missing
process must decrease during the core helium burning phase. When excluding the
$\nu_{\rm{add}}$ during core helium burning phase, we can match the rotational
periods of both the core helium burning stars and white dwarfs.
