Fig. 4.


Modeled (M1) Hyades star cluster and its tail at time-stacked snapshots from 620 Myr to 695 Myr. Top panel: proper motion distribution in physical km s−1 units. The central clump represents the star cluster, and the extended distribution (up to 80 km s−1) consists of members of the tidal tail. Middle panel: proper motion in RA and radial velocity distribution showing the same 80 km s−1 span for the tidal tails members. Bottom panel: on-the-sky distribution of proper motions of the modeled cluster and its tails. Because of the proximity of Hyades to the Sun, the spread in proper motion is large (see the loose lump representing the cluster members), and the two overdensities in the shape of tentacles caution against using a blind clustering algorithm in order to search for tidal tails in the data.

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