  Context. Due to the presence of magnetic fields, protostellar jets/outflows
are a natural consequence of accretion onto protostars. They are expected to
play an important role for star and protoplanetary disk formation. Aims. We aim
to determine the influence of outflows on star and protoplanetary disk
formation in star forming clumps. Methods. Using RAMSES, we perform the first
magnetohydrodynamics calculation of massive star-forming clumps with ambipolar
diffusion, radiative transfer including the radiative feedback of protostars
and protostellar outflows while systematically resolving the disk scales. We
compare it to a model without outflows. Results. We find that protostellar
outflows have a significant impact on both star and disk formation. They
provide significant additional kinetic energy to the clump, with typical
velocities of a few 10 km/s, impact the clump and disk temperatures, reduce the
accretion rate onto the protostars and enhance fragmentation in the filaments.
We find that they promote a more numerous stellar population. They do not
impact much the low mass end of the IMF, which is probably controlled by the
mass of the first Larson core, however, that they have an influence on its peak
and high-mass end. Conclusions. Protostellar outflows appear to have a
significant influence on both star and disk formation and should therefore be
included in realistic simulations of star-forming environments.
