halo. The dwarfs had equal masses and only differed by the disk scale lengths. They were placed on a radial orbit towards each other and their disks were inclined by $\pm45$deg to the collision axis so that the angular momentum vectors of the disks and the velocities of the dwarfs were initially in the same plane. The model adequately reproduces the observed properties of And II, including the prolate rotation and shape. The presence of the different stellar populations can be interpreted as originating from different dwarfs: the two populations then have different density distributions (as a result of different initial disk scale lengths) but very similar kinematics.

Another scenario known to lead to the formation of dSph galaxies is the one based on tidal interaction of the initially disky dwarf satellites with bigger hosts, like the Milky Way or M31 [e.g. @lo14bar; @lo15]. However, as argued by @lo14andii, tidal interaction is able to remove very efficiently the initial rotation of the disk (around the shortest axis) as it transforms to a bar and then a spheroid, but cannot induce any significant prolate rotation (around the longest axis).

The initial conditions used in the simulation described in @lo14andii may seem 