Clumpy galaxies at cosmic noon show systematically lower metallicities than the mass-metallicity relation, with clump properties indicating metal-poor gas accretion as the driver rather than mergers.
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Metal-Poor Gas Accretion Drives Giant Clump Formation at 0.6 < z < 2.6
Clumpy galaxies at cosmic noon show systematically lower metallicities than the mass-metallicity relation, with clump properties indicating metal-poor gas accretion as the driver rather than mergers.
- The Fraction of Clumpy Galaxies in JADES Over $2<z<9$