Clumps in high-redshift spiral galaxies are smaller than commonly reported, spatially concentrated toward spiral arms, smaller but brighter inside arms than between them, with similar colors, suggesting arms stimulate clump formation but do not alter their star formation properties.
Giant Clumps in Simulated High- z
4 Pith papers cite this work. Polarity classification is still indexing.
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astro-ph.GA 4representative citing papers
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.
Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.
citing papers explorer
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Clumps in spiral galaxies at $z \lesssim 3$: Disentangling two spatial modes of star formation
Clumps in high-redshift spiral galaxies are smaller than commonly reported, spatially concentrated toward spiral arms, smaller but brighter inside arms than between them, with similar colors, suggesting arms stimulate clump formation but do not alter their star formation properties.
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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.
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Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$
Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.
- The Fraction of Clumpy Galaxies in JADES Over $2<z<9$