A Hubble-like sequence of galaxy morphologies exists by redshift 4, with low-mass galaxies as persistent star-forming disks and massive galaxies following either stable disk or rapid compaction-quenching paths.
M., P´ erez-Gonz´ alez, P
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BAGPIPES fitting of 9289 massive quiescent galaxies shows most SFHs rise gradually then quench in 1-2 Gyr, with faster quenching at z>1 and slower at z<1, interpreted as multiple AGN feedback and gas-supply mechanisms.
Post-starburst galaxies at cosmic noon show very low radio detection rates and compact weak sources, consistent with short-lived low-luminosity AGN, while older quiescent galaxies exhibit stronger extended radio emission.
The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.
Globular cluster mass fractions, in-situ fractions, metallicity spreads, and spatial profiles in simulated compact galaxies can identify massive relic analogs with early assembly histories.
citing papers explorer
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The Hubble sequence in JWST CEERS from unbiased galaxy morphologies
A Hubble-like sequence of galaxy morphologies exists by redshift 4, with low-mass galaxies as persistent star-forming disks and massive galaxies following either stable disk or rapid compaction-quenching paths.
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Inferring the star-formation histories of massive quiescent galaxies with BAGPIPES: Evidence for multiple quenching mechanisms
BAGPIPES fitting of 9289 massive quiescent galaxies shows most SFHs rise gradually then quench in 1-2 Gyr, with faster quenching at z>1 and slower at z<1, interpreted as multiple AGN feedback and gas-supply mechanisms.
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Tracing Radio AGN-Driven Quenching in Post-Starburst Galaxies at Cosmic Noon
Post-starburst galaxies at cosmic noon show very low radio detection rates and compact weak sources, consistent with short-lived low-luminosity AGN, while older quiescent galaxies exhibit stronger extended radio emission.
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The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies
The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.
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Tracing the relic nature of compact galaxies through their globular cluster systems
Globular cluster mass fractions, in-situ fractions, metallicity spreads, and spatial profiles in simulated compact galaxies can identify massive relic analogs with early assembly histories.