UVJ colors saturate below log(sSFR) ~ -10.5; new UV/MIR color-color diagrams allow more efficient selection of galaxies with substantially lower ongoing star formation.
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7 Pith papers cite this work. Polarity classification is still indexing.
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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.
Group-scale halos produce a dual effect on infalling galaxies: pre-processing raises quiescent fraction early, while protection delays cluster-driven quenching to smaller d_R.
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.
Observational analysis of COSMOS galaxy groups shows quiescent fraction builds steadily from z~1.5-2 with faster growth in richer groups, first RS ridgeline galaxies by z~2, a possible early overdensity at z=3.4, and no significant evolution in RS slope or scatter.
A multimodal neural network trained on MPA-JHU references produces SFR, stellar mass, and metallicity estimates for 547 million low-redshift galaxies in DESI LS DR10.
Barred galaxies with residual central emission and NUV-r color transition at the bar end represent an intermediate evolutionary phase in bar-driven quenching before full central quenching.
citing papers explorer
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Beyond UVJ: More Efficient Selection of Quiescent Galaxies With UV / Mid-IR Fluxes
UVJ colors saturate below log(sSFR) ~ -10.5; new UV/MIR color-color diagrams allow more efficient selection of galaxies with substantially lower ongoing star formation.
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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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The dual effect of group-scale environments on galaxy quenching during cluster infall: pre-processing and protection
Group-scale halos produce a dual effect on infalling galaxies: pre-processing raises quiescent fraction early, while protection delays cluster-driven quenching to smaller d_R.
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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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COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction
Observational analysis of COSMOS galaxy groups shows quiescent fraction builds steadily from z~1.5-2 with faster growth in richer groups, first RS ridgeline galaxies by z~2, a possible early overdensity at z=3.4, and no significant evolution in RS slope or scatter.
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A Value-added Physical Properties Catalog for Low-redshift Galaxies from DESI Legacy Imaging Surveys DR10
A multimodal neural network trained on MPA-JHU references produces SFR, stellar mass, and metallicity estimates for 547 million low-redshift galaxies in DESI LS DR10.
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Tracing evolutionary pathways of bar-driven quenching in local Universe disc galaxies
Barred galaxies with residual central emission and NUV-r color transition at the bar end represent an intermediate evolutionary phase in bar-driven quenching before full central quenching.