  We present a series of 20 cosmological zoom simulations of the formation of
massive galaxies with and without a model for AGN feedback. Differences in
stellar population and kinematic properties are evaluated by constructing mock
integral field unit (IFU) maps. The impact of the AGN is weak at high redshift
when all systems are mostly fast-rotating and disc-like. After $z \sim 1$ the
AGN simulations result in lower mass, older, less metal rich and slower
rotating systems with less disky isophotes - in general agreement with
observations. Two-dimensional kinematic maps of in-situ and accreted stars show
that these differences result from reduced in-situ star formation due to AGN
feedback. A full analysis of stellar orbits indicates that galaxies simulated
with AGN are typically more triaxial and have higher fractions of x-tubes and
box orbits and lower fractions of z-tubes. This trend can also be explained by
reduced late in-situ star formation. We introduce a global parameter, $\xi_3$ ,
to characterise the anti-correlation between the third-order kinematic moment
$h_3$ and the line-of-sight velocity ($v_{los}/{\sigma}$), and compare to
ATLAS$^{3D}$ observations. The kinematic asymmetry parameter $\xi_3$ might be a
useful diagnostic for large integral field surveys as it is a kinematic
indicator for intrinsic shape and orbital content.

Astrophysics of Galaxies