Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Stellar feedback in a clumpy galaxy at z ∼ 3.4


Burkert,  A.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;


Behrendt,  M.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available

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.

Cite as: https://hdl.handle.net/21.11116/0000-0009-A30B-3
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.