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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2026 3representative citing papers
Star formation histories inferred for z=2-5 massive quiescent galaxies imply past number densities that align with observed rapid evolution since z~7.
The Milky Way disk spin-up to rotationally supported motion occurred at mean age 12.1 Gyr for -1.25 < [Fe/H] < -0.9, traced by high-alpha stars, while low-alpha stars show no transition and start at disk-like velocities.
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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Winding Back the Clock: Recent Star Formation Histories of Massive Quiescent Galaxies Are Consistent With Their Rapid Number Density Evolution Since $\mathbf{z\sim7}$
Star formation histories inferred for z=2-5 massive quiescent galaxies imply past number densities that align with observed rapid evolution since z~7.
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Dawn of the Milky Way disk: Determination of when a rotationally supported disk appears and dating the spin-up of the disk
The Milky Way disk spin-up to rotationally supported motion occurred at mean age 12.1 Gyr for -1.25 < [Fe/H] < -0.9, traced by high-alpha stars, while low-alpha stars show no transition and start at disk-like velocities.