Iani, E.E.IaniZANELLA, ANITAANITAZANELLAVernet, J.J.VernetRichard, J.J.RichardGronke, M.M.GronkeHarrison, C. M.C. M.HarrisonArrigoni-Battaia, F.F.Arrigoni-BattaiaRodighiero, G.G.RodighieroBurkert, A.A.BurkertBehrendt, M.M.BehrendtChen, Chian-ChouChian-ChouChenEmsellem, E.E.EmsellemFensch, J.J.FenschHibon, P.P.HibonHilker, M.M.HilkerLe Floc'h, E.E.Le Floc'hMainieri, V.V.MainieriSwinbank, A. M.A. M.SwinbankValentino, F.F.ValentinoVanzella, E.E.VanzellaZwaan, M. A.M. A.Zwaan2025-05-082025-05-0820210035-8711http://hdl.handle.net/20.500.12386/37110Giant 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 they survive to stellar feedback for >50 Myr. Numerical simulations show that clumps' survival depends on the stellar feedback recipes that are adopted. Up to date, observational constraints on both clumps' outflows strength and gas removal time-scale are still uncertain. In this context, we study a line-emitting galaxy at redshift z ≃ 3.4 lensed by the foreground galaxy cluster Abell 2895. Four compact clumps with sizes ≲280 pc and representative of the low-mass end of clumps' mass distribution (stellar masses ≲2 × 10<SUP>8</SUP> M<SUB>⊙</SUB>) dominate the galaxy morphology. The clumps are likely forming stars in a starbursting mode and have a young stellar population (~10 Myr). The properties of the Lyman-α (Lyα) emission and nebular far-ultraviolet absorption lines indicate the presence of ejected material with global outflowing velocities of ~200-300 km s<SUP>-1</SUP>. Assuming that the detected outflows are the consequence of star formation feedback, we infer an average mass loading factor (η) for the clumps of ~1.8-2.4 consistent with results obtained from hydrodynamical simulations of clumpy galaxies that assume relatively strong stellar feedback. Assuming no gas inflows (semiclosed box model), the estimates of η suggest that the time-scale over which the outflows expel the molecular gas reservoir (≃7 × 10<SUP>8</SUP> M<SUB>⊙</SUB>) of the four detected low-mass clumps is ≲50 Myr.STAMPAenArticle10.1093/mnras/stab23762-s2.0-85117121485https://academic.oup.com/mnras/article/507/3/3830/6356587https://api.elsevier.com/content/abstract/scopus_id/851171214852021MNRAS.507.3830IFIS/05 - ASTRONOMIA E ASTROFISICA