Fig. 16.

image

Encounter of the cluster and its tidal tails with a massive Galactic lump. This asymmetrically stretches the tail (note the displaced positions of the epicyclic overdensities; compare with Fig. 2) and changes the velocity distribution in the star cluster and in its tails. As the star cluster is disrupted by the lump, its velocity distribution increases. The snapshot here combines lump distance and mass so that the velocity dispersion of the model cluster is increased to the potentially higher observed value in the Hyades star cluster (see text for more details). This affects the appearance of the star cluster and of its tail in different parameter spaces. The change when the CP method is applied in the bottom panel is clearly visible. The disruption process thus can not only produce a temporary asymmetry in the tidal tails (prior to complete disruption), but can affect the detection using the CP method, which can lead to an incomplete recovery of the tail.

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