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
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
fields
astro-ph.GA 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
The Big Wheel at z~3 has a stellar-to-halo mass ratio of 0.06, higher than expected, implying efficient stellar assembly without major mergers or instabilities.
Bulgeless galaxies in TNG50 form later, maintain high disc fractions since z~1, and preferentially experience gas-rich coplanar mergers that preserve discs, unlike bulge-dominated galaxies.
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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The galaxy-halo connection and the dynamical evolution of a giant disc in a massive node of the Cosmic Web at z~3
The Big Wheel at z~3 has a stellar-to-halo mass ratio of 0.06, higher than expected, implying efficient stellar assembly without major mergers or instabilities.
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Bulgeless Evolution And the Rise of Discs (BEARD) II. The role of mergers in shaping the Milky Way analogues in TNG50
Bulgeless galaxies in TNG50 form later, maintain high disc fractions since z~1, and preferentially experience gas-rich coplanar mergers that preserve discs, unlike bulge-dominated galaxies.