Top left panel: spatial separation between baryon and DM clumps at the redshift of collapse, normalized by the virial radius of the DM halo, for 2σ (solid line) and 3σ (dashed line) fluctuations, plotted against the baryon clump mass M_b. Collapse is defined by the condition , for 2σ and 3σ. Note that clumps with baryon mass larger than a few× 10⁶ M_☉ are separated from their DM halos by less than the virial radius (they are "inside" the DM halo) and vice versa for clumps with smaller masses ("outside"). Calculations are for v_bc = 1σ_vbc, θ = 0. Bottom left panel: estimated survival time of baryon clumps against spiral-in and merger through dynamical friction ("inside" the DM halo) and loss of stars through evaporation ("outside" the halo). Baryon clumps with masses in the range ~10⁵–4 × 10⁶ M_☉ are potentially long-lived, especially if tidal forces from other nearby clumps unbind them from their DM halos. Right panels: similar to left panels, except that collapse is defined by . The results are generally similar.