Fig. 6.

image

Hyades cluster and its tidal tails used to explain the transition from the classical CP metod to newly introduced CCP method. Top panel: classical CP method diagram showing the velocity distribution of M1-simulated Hyades and its tidal tails projected onto the parallel (horizontal axes) and perpendicular direction (vertical axes) to the CP. The predicted velocity component is removed based on the on-the-sky position of individual objects (see text for more details). The snapshots beginning at 620 Myr–695 Myr are plotted, each placed at the Hyades position in spatial and velocity space. In red we show snapshots at 620, 625, 630, 635, 640, 645, and 650 Myr, in black those at 655 Myr, and in blue the snapshots at 660, 665, 670, 675, 680, 685, and 690 Myr. This shows the scatter in the CP diagram that is caused by the time evolution of the tidal tail. The extent of the points on the horizontal axes reaches 40 km s−1. Middle panel: dependence of v||pred − v||obs as used in the CP method (horizontal axes in the top panel) as a function of the distance from the cluster centre (Rcl). The objects farther from the cluster centre move relatively faster. The red line shows the approximately linear relation denoted as the function Λ(R − Rcl). Bottom panel: modelled points in the CP diagram (top panel) without the velocity trend from the middle panel described by the function Λ(R − Rcl). This operation compacts the whole structure (star cluster plus the tidal tail) within a region spanning a few km s−1. We call this method the CCP method and use it in Sect. 3.1 to search for the full extent of the Hyades tidal tails in the Gaia data.

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