JWST is providing a unique opportunity to directly study the feedback processes regulating star formation (SF) in early galaxies. The two z > 5 quiescent systems (JADES-GS-z7-01-QU and MACS0417-z5BBG) detected so far show a recent starburst after which SF is suppressed. To clarify whether such quenching is due to supernova (SN) feedback, we have developed a minimal physical model. We derive a condition on the minimum star formation rate, , lasting for a time interval Δtb, required to quench SF in a galaxy at redshift z, with gas metallicity Z, and hosted by a halo of mass Mh. We find that lower (z, Z, Mh) systems are more easily quenched. We then apply the condition to JADES-GS-z7-01-QU (z = 7.3, M⋆ = 108.6M⊙) and MACS0417-z5BBG (z = 5.2, M⋆ = 107.6M⊙) and find that SN feedback largely fails to reproduce the observed quenched SF history. Alternatively, we suggest that SF is rapidly suppressed by radiation-driven dusty outflows sustained by the high specific star formation rates (43 and 25 Gyr−1, respectively) of the two galaxies. Our model provides a simple tool to interpret the SF histories of post-starburst galaxies and unravel quenching mechanisms from incoming JWST data

Can Supernovae Quench Star Formation in High-z Galaxies?

Ferrara, Andrea;Pallottini, Andrea
2024

Abstract

JWST is providing a unique opportunity to directly study the feedback processes regulating star formation (SF) in early galaxies. The two z > 5 quiescent systems (JADES-GS-z7-01-QU and MACS0417-z5BBG) detected so far show a recent starburst after which SF is suppressed. To clarify whether such quenching is due to supernova (SN) feedback, we have developed a minimal physical model. We derive a condition on the minimum star formation rate, , lasting for a time interval Δtb, required to quench SF in a galaxy at redshift z, with gas metallicity Z, and hosted by a halo of mass Mh. We find that lower (z, Z, Mh) systems are more easily quenched. We then apply the condition to JADES-GS-z7-01-QU (z = 7.3, M⋆ = 108.6M⊙) and MACS0417-z5BBG (z = 5.2, M⋆ = 107.6M⊙) and find that SN feedback largely fails to reproduce the observed quenched SF history. Alternatively, we suggest that SF is rapidly suppressed by radiation-driven dusty outflows sustained by the high specific star formation rates (43 and 25 Gyr−1, respectively) of the two galaxies. Our model provides a simple tool to interpret the SF histories of post-starburst galaxies and unravel quenching mechanisms from incoming JWST data
2024
Settore FIS/05 - Astronomia e Astrofisica
High-redshift galaxies; Galaxy evolution; Galaxy quenching; Cosmology
   NEar FiEld cosmology: Re-Tracing Invisible TImes
   NEFERTITI
   European Commission
   Horizon 2020 Framework Programme
   804240

   The Interstellar Medium of High Redshift Galaxies
   INTERSTELLAR
   European Commission
   Horizon 2020 Framework Programme
   740120
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11384/139304
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