tubes are convex while the inner ones are concave.

Comparing the distributions of the ratio $\kappa/\omega$ in the right panels of Fig. \[fig:om\] we see significant differences among simulations. In particular, the shape of the histogram for simulation I60R is significantly different than for the other ones. The difference is not only that there are more stars on long-axis tubes (the distribution takes larger values) but the left peak of $\kappa/\omega \approx 1.4$ is significantly more populated than the right peak with $\kappa/\omega \approx 1.8$. Since we have identified the left peak (lower branch) with the inner long-axis tubes this means that the merger remnant in simulation I60R is populated more by these orbits than the outer long-axis tubes. The situation is opposite for the remaining simulations. Since the inner tubes tend to produce more boxy shapes this explains why the galaxy formed in I60R was much more boxy (see Fig. \[fig:maps\]) than the other ones.

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Mergers versus tidal stirring
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As mentioned in the Introduction, an alternative, and far better studied, scenario for the formation of dSph galaxies in the Local Group involves their interaction with a bigger host galaxy like the Milky Way or M31. In this 