Tidal tails of nearby open clusters - II. A review of simulated properties and the reliability of observational catalogues

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Table 1

Initial conditions of the N-body simulations.

Model name	Initial mass [M_☉]	xyz_{galactocentric} [pc]	V_xV_yV_{z galactocentric} [km s⁻¹]
M68, M82, …, M20000	68, 82, 100, 121, 146, 177, 215, 261, 316, 383, 464, 562, 681, 825, 1000, 1211, 1467, 1778, 2154, 2610, 3162, 3831, 4641, 5623, 6812, 20 000	−8000, 0, 0	0, −220, 0
M20000_e	20 000	−7067.59, 2899.3, 99.92	−110.96, −193.72, 5.33

Notes. Models M68—M20000 are a grid of clusters on circular orbits, while M20000_e is on an eccentric (Praesepe-like) orbit. The initial number density within the half-mass radius was kept the same at 306 stars pc⁻³ for all simulations.

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