Top panel: velocity fields of the tails obtained using a Gaussian smoothing of 3 pixels FWHM. The two subsystems have been put at rest frames, so that they can be compared on the same figure. Bottom panel: velocity dispersion map of the tail obtained using a Gaussian smoothing of 3 pixels FWHM. The contours correspond to [O II] flux emission as in Fig. 3. The green circles indicate the position of other cluster member galaxies.
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