Offsets of ISF protostars (left), ISF stars (center), and L1641 stars (right) from the gas ridgelines in α (Figs. 6 and 7) and RV (Fig. 8). The protostars are shown only for the ISF because of the difficulty of capturing the filament structure further south by simple prescriptions. Points are color-coded north-to-south ↔ red-to-blue. Ratio of axis scales is 1 Myr. Hence, the vertically-elongated structure of these diagrams indicates timescales ≪ 1 Myr, < 1 Myr, and ~ 1 Myr for the three diagrams, respectively. These could be either lifetime or turnaround time. The stellar distributions (both ISF and L1641) are broadly distributed, with no obvious filament-hugging subpopulations, like the ISF protostars. However, they also show significant lumpiness demonstrating incomplete relaxation. The protostars show some severe clumping, with a high density near the origin, in particular.
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