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  Stellar feedback in a clumpy galaxy at z ∼ 3.4

Iani, E., Zanella, A., Vernet, J., Richard, J., Gronke, M., Harrison, C. M., et al. (2021). Stellar feedback in a clumpy galaxy at z ∼ 3.4. Monthly Notices of the Royal Astronomical Society, 507(3), 3830-3848. doi:10.1093/mnras/stab2376.

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Iani, E., Author
Zanella, A., Author
Vernet, J., Author
Richard, J., Author
Gronke, M., Author
Harrison, C. M., Author
Arrigoni-Battaia, F., Author
Rodighiero, G., Author
Burkert, A.1, Author           
Behrendt, M.1, Author           
Chen, Chian-Chou, Author
Emsellem, E., Author
Fensch, J., Author
Hibon, P., Author
Hilker, M., Author
Le Floc’h, E., Author
Mainieri, V., Author
Swinbank, A. M., Author
Valentino, F., Author
Vanzella, E., Author
Zwaan, M. A., Author more..
Affiliations:
1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 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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Language(s): eng - English
 Dates: 2021-08-23
 Publication Status: Published online
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 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/stab2376
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Title: Monthly Notices of the Royal Astronomical Society
  Abbreviation : Mon. Not. Roy. Astron. Soc.
Source Genre: Journal
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Pages: - Volume / Issue: 507 (3) Sequence Number: - Start / End Page: 3830 - 3848 Identifier: ISSN: 0035-8711
ISSN: 1365-8711