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Fig. 6


Average velocity differences between the gas and the stellar disk normalised to the average observed rotational velocity of the gas, difference in position angle between the projected distributions of the gaseous and stellar disks, and between the projected stellar disk and the kinematic axis of the gas, for merger simulations (black) and for systems in isolation (red). The different rows correspond to different ranges of viewing angles. In this figure we have included the model-A dwarf with M = 1.4 × 108 M (solid circles), as well as values for systems with M = 4.4 × 106 M (dashes) and with M = 1.1−2.7 × 107 M (diamonds).

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