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Table 1

Comprehensive properties of high-velocity BSSs and representative core members in NGC 188.

Source ID (Gaia DR3) RA (deg) Dec (deg) G0 (mag) (BPRP)0 (mag) vrel (km s−1) cos θ (Radial) Tej (Myr) rorigin (pc) RUWE NSS Flag IPD Frac Seq. Type
Dynamically ejected halo candidates
573778429264792832 16.8356 85.3144 14.96 0.79 8.9 0.99 1.5 ± 0.1 0.44 1.04 0 0.00 Red
573973111543073024 13.6312 85.5359 14.77 0.72 5.9 0.98 1.5 ± 0.1 0.82 1.00 0 0.00 Red

Representative core BSS population
573968576057423360 11.0892 85.4417 13.26 0.45 . . . . . . . . . . . . 1.40 0 0.00 Red
573938408207239296 12.0834 85.2242 14.11 0.41 . . . . . . . . . . . . 1.01 0 0.00 Blue
573941294425258496 11.8000 85.2254 14.36 0.79 . . . . . . . . . . . . 0.96 0 0.00 Red

Notes. G0 and (GBPGRP)0 are corrected for differential reddening. vrel and cos θ (alignment with the radial vector) are calculated in the cluster rest frame. Tej (ejection age) and rorigin (minimum distance to core) are derived from orbit back-integration using a 2180 M Plummer potential. RUWE, NSS flag, and IPD Frac (ipd_frac_multi_peak) are astrometric quality and multiplicity indicators from Gaia DR3. he BSS population statistics (N = 45) show that the red sequence comprises 88.9% (MT-origin) and the blue sequence comprises 11.1% (collision-origin).

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