The maps of line-of-sight velocity dispersion in the right column of Fig. \[fig:maps\] show considerable variation among the different simulations without any clear trend: some remnants have a maximum dispersion in the center while others have the maxima at larger distances. It seems that the complicated structure of the dispersion maps may be used as an indicator of the merger origin of the galaxy even after many Gyr of evolution.

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Triaxiality
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In order to study the evolution of the shape of the merger remnants, we again analyzed each dwarf separately selecting the stars inside the sphere of 2kpc centered on a given dwarf. In Fig. \[fig:triax\] we plot the intermediate to major axis ratio, $b/a$, the minor to major axis ratio, $c/a$, and the triaxiality parameter, $T$, defined as $T=[1-(b/a)^2]/[1-(c/a)^2]$. When $T$ is lower than $1/3$ the galaxy is rather oblate, values greater than $2/3$ indicate a prolate shape and when $T$ falls between these values the galaxy has a triaxial shape.

The most dramatic change of the shape of the dwarfs happens around the second passage (approximately at $\sim$4Gyr). The ratio $b/a$, which is equal to unity at the beginning, slightly drops to values between about 