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Stellar feedback in a clumpy galaxy at z 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 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 × 108 M) 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-1. 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 × 108 M) of the four detected low-mass clumps is ≲50 Myr.
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Contributor : Nathalie POTHIER Connect in order to contact the contributor
Submitted on : Friday, July 1, 2022 - 1:56:13 PM
Last modification on : Saturday, July 2, 2022 - 3:40:13 AM

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E. Iani, A. Zanella, J. Vernet, J. Richard, M. Gronke, et al.. Stellar feedback in a clumpy galaxy at z 3.4. Monthly Notices of the Royal Astronomical Society, 2021, 507, pp.3830-3848. ⟨10.1093/mnras/stab2376⟩. ⟨insu-03711487⟩



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