Quiescent fractions reach ~50% in hot-accretion high-z groups and ~0% in cold-accretion ones, supporting accretion-mode driven quenching via inside-out starvation.
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7 Pith papers cite this work. Polarity classification is still indexing.
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2026 7representative citing papers
Intermediate-redshift galaxies show systematically higher dust attenuation at fixed star formation rate surface density than local galaxies, with the excess strongest for galaxies below the star-forming main sequence.
Main-sequence galaxies at z~1.1–1.6 host extended CO, [C I], and dust disks with roughly constant gas fraction and depletion time out to 2 Re, supporting steady accretion rather than mergers.
Switching between four common stellar population synthesis models produces systematic offsets of up to 0.6 dex in stellar mass and 0.4 dex in star formation rate for the same galaxies.
An analytical model of galaxies evolving along the star-forming main sequence shows that episodic quiescence or late assembly is required to reproduce observed star formation histories and avoid over-massive galaxies today.
Void galaxies show modestly higher star formation rates in early spirals and outer disks, lower extinction, and higher gas-fraction proxies than matched galaxies in filaments and walls, suggesting slower quenching in underdense environments.
In TNG50, high-stellar-mass galaxies show shallow inner DM slopes regardless of central or satellite status, low-mass galaxies exhibit diverse profiles with satellites steeper especially if red and in massive hosts, and inner slopes steepen from z~1 to z=0 more strongly in the hydro run.
citing papers explorer
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Quiescent fractions in high-redshift galaxy groups reflect their hot-or-cold state of gas accretion
Quiescent fractions reach ~50% in hot-accretion high-z groups and ~0% in cold-accretion ones, supporting accretion-mode driven quenching via inside-out starvation.
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The MAGPI Survey: Evidence for Non-Universal Resolved Dust Attenuation Relations Beyond the Local Universe
Intermediate-redshift galaxies show systematically higher dust attenuation at fixed star formation rate surface density than local galaxies, with the excess strongest for galaxies below the star-forming main sequence.
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NOEMA3D: extended CO, [C I] and dust in massive star-forming main sequence galaxies at cosmic noon
Main-sequence galaxies at z~1.1–1.6 host extended CO, [C I], and dust disks with roughly constant gas fraction and depletion time out to 2 Re, supporting steady accretion rather than mergers.
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Impact of stellar population models on the estimated physical properties of galaxies
Switching between four common stellar population synthesis models produces systematic offsets of up to 0.6 dex in stellar mass and 0.4 dex in star formation rate for the same galaxies.
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Built to Rest: The Evolving Star-Forming Main Sequence Requires Episodic Quiescence or Late Assembly
An analytical model of galaxies evolving along the star-forming main sequence shows that episodic quiescence or late assembly is required to reproduce observed star formation histories and avoid over-massive galaxies today.
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The CAVITY project. The spatially resolved SFR of galaxies in voids
Void galaxies show modestly higher star formation rates in early spirals and outer disks, lower extinction, and higher gas-fraction proxies than matched galaxies in filaments and walls, suggesting slower quenching in underdense environments.
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The Inner Dark-Matter Structure of Galaxies
In TNG50, high-stellar-mass galaxies show shallow inner DM slopes regardless of central or satellite status, low-mass galaxies exhibit diverse profiles with satellites steeper especially if red and in massive hosts, and inner slopes steepen from z~1 to z=0 more strongly in the hydro run.