  We examine metallicities, ages and orbital properties of halo stars in a
Milky-Way like disk galaxy formed in the cosmological hydrodynamical MaGICC
simulations. Halo stars were either accreted from satellites or they formed in
situ in the disk or bulge of the galaxy and were then kicked up into the halo
("in situ/ kicked-up" stars). Regardless of where they formed both types show
surprisingly similar orbital properties: the majority of stars of both types
are on short-axis tubes with the same sense of rotation as the disk -- implying
that a large fraction of satellites are accreted onto the halo with the same
sense of angular momentum as the disk.
