I90VY2 the evolution is dramatically different for the two dwarfs, so we include the result for Dwarf2 as a dashed curve in Fig. \[fig:rot\].

For all simulations, there is essentially no rotation around the intermediate axis and the evolution of the rotation around the minor axis is trivial: the disk preserves the rotation until the two dwarfs actually start to merge and then the rotation vanishes and remains close to zero until the end of the simulation. We show one example of the evolution of the mean rotation velocity around all principal axes for our default simulation I90R in Fig. \[fig:rot4i90\].

. \[fig:maps\]

Fig. \[fig:maps\] shows the maps of line-of-sight properties of the final outputs for all five simulations in projection onto the $xy$ plane, i.e. as seen along the $z$ axis of the merger remnant. Here, $x$, $y$ and $z$ correspond to the major, intermediate and minor axis of the combined stellar components of both dwarfs. The images confirm that the rotation signal (middle-column panels of Fig. \[fig:maps\]) is around the longest ($x$) axis, i.e. the rotation is clearly prolate in all simulations, even when the rotation level is very low as in I90VY2.

The amount of prolate rotation 