Stellar feedback in a clumpy galaxy at <i>z</i> ? 3.4

ABSTRACT Giant star-forming regions (clumps) are widespread features of galaxies at z ? 1?4. Theory predicts that they can play a crucial role in galaxy evolution, if survive to stellar feedback for &amp;gt;50 Myr. Numerical simulations show clumps’ survival depends on the recipes adopted. Up date, observational constraints both outflows strength and gas removal time-scale still uncertain. In this context, we study line-emitting redshift ? 3.4 lensed by foreground cluster Abell 2895. Four compact clumps with sizes ?280 pc representative low-mass end mass distribution (stellar masses ?2 × 108 M?) dominate morphology. The likely forming stars starbursting mode have young population (?10 Myr). properties Lyman-? (Ly?) emission nebular far-ultraviolet absorption lines indicate presence ejected material global outflowing velocities ?200–300 km s?1. Assuming detected consequence star formation feedback, infer an average loading factor (?) ?1.8–2.4 consistent results obtained from hydrodynamical clumpy assume relatively strong feedback. no inflows (semiclosed box model), estimates ? suggest over which expel molecular reservoir (?7 four is ?50