Bulgeless galaxies trace the upper envelope of the mass-R1 relation with scatter driven by central stellar density and the spatial configuration of mergers rather than their number.
Title resolution pending
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
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astro-ph.GA 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
Massive quiescent galaxies at cosmic noon are compact and bulge-dominated with inside-out quenching, where inner regions formed stars ~0.5 Gyr earlier and quenched faster than outskirts.
citing papers explorer
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Bulgeless Evolution And the Rise of Discs (BEARD) I. Physical drivers of the mass-size relation for Milky Way-like galaxies
Bulgeless galaxies trace the upper envelope of the mass-R1 relation with scatter driven by central stellar density and the spatial configuration of mergers rather than their number.
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Morphological and Star Formation Properties of Cosmic Noon Massive Quiescent Galaxies
Massive quiescent galaxies at cosmic noon are compact and bulge-dominated with inside-out quenching, where inner regions formed stars ~0.5 Gyr earlier and quenched faster than outskirts.