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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6 Pith papers cite this work. Polarity classification is still indexing.
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astro-ph.GA 6representative citing papers
The size-mass relation for star-forming galaxies at 0.6 < z ≤ 4 shows a gradient in slope with rest-frame wavelength, crossing at ~10^9.5 solar masses proposed as the transition between diffuse and compact morphologies.
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.
Star-forming galaxies show a transition from negative to positive sSFR radial gradients around z~2, implying a change from outside-in to inside-out growth.
Star-forming galaxies show R_e,J ∝ (1+z)^(-0.92) and μ_J evolution with γ=3.07 while quiescent galaxies evolve faster (β=-1.34, γ=3.70) at fixed stellar mass, with evolution driven by luminosity and size changes.
citing papers explorer
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Transition from Outside-in to Inside-Out at $z\sim 2$: Evidence from Radial Profiles of Specific Star Formation Rate based on JWST/HST
Star-forming galaxies show a transition from negative to positive sSFR radial gradients around z~2, implying a change from outside-in to inside-out growth.
- The Fraction of Clumpy Galaxies in JADES Over $2<z<9$