Ensemble figures
Interactive versions of the paper's key ensemble figures, computed from the released catalogue files. Hover for the star, click to open its record. All orbit quantities are point-estimate model outputs.
Pericentre vs apocentre — the plunge diagram
cf. paper Fig. 7 / Fig. 12Every Tier A+B+C star, coloured by eccentricity (blue e≈0.88 → red e≈1). The entire sample sits far below the R_peri = R_apo line: these are radial plunges. Switching the potential model shifts pericentres (medians ~115 pc static → ~14 pc barred) but the radial character survives — the paper's central robustness claim, which you can check here model by model.
Toomre diagram
cf. paper Fig. 8Azimuthal velocity against the perpendicular velocity component at the observed epoch, coloured by tier. Disc stars cluster near v_φ ≈ ±229 km s⁻¹; the slow-VGRF sample hugs the origin by construction — the interesting content is its spread and the tier structure near the 25 km s⁻¹ boundary.
Membership probability vs point-estimate speed
cf. fig_phase14_pvgrf_vs_vgrfHow the tiers are defined: P(VGRF<25 km/s) from the adaptive Monte Carlo against the point-estimate speed, for the full candidate pool below 60 km s⁻¹. The vertical spread at fixed speed is measurement quality: a star at 20 km s⁻¹ with large distance uncertainty can have P ≈ 0.5, while a precise one is a secure member. Colours are tiers (A cyan → X grey).
Sky distribution (galactic Aitoff)
cf. paper Fig. 5Tier A–D candidates in galactic coordinates (Aitoff projection, centre l = 0 toward the Galactic centre, l increasing leftward), coloured by point-estimate speed (cyan <15, blue <25, amber <35 km/s). The concentration toward the inner Galaxy — 39.7% of Tier A+B+C within |l| ≤ 30° vs 6.2% toward the anticentre — is expected for stars near apocentre of inward-plunging orbits, modulated by the sparse RVS selection function.