Galaxy structure depends on environment at fixed stellar mass at >5σ, secondary to mass, with cluster-only effects at z<0.5 and multi-scale effects for massive systems at z≥0.5.
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Galaxies become less concentrated, more asymmetric and less clumpy toward lower stellar masses, with bar fraction declining to zero near 10^8 solar masses and CAS parameters losing separating power in the dwarf regime.
ATTILA tool identifies 24 new ultra-diffuse galaxies in Hydra I, doubling the known population to 48, plus 92 additional low surface brightness galaxies, while recovering over 80% of previously known ones.
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.
Galaxy properties in IllustrisTNG form a continuum across the multiscale caustic skeleton, with formation time of web components influencing colors and star formation activity.
citing papers explorer
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Environmental Sculpting of Galaxy Structure at Fixed Stellar Mass: A Multi-Scale Analysis Across Cosmic Time using 3 Million HSC Galaxies
Galaxy structure depends on environment at fixed stellar mass at >5σ, secondary to mass, with cluster-only effects at z<0.5 and multi-scale effects for massive systems at z≥0.5.
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Global trends in morphology from massive to dwarf galaxies
Galaxies become less concentrated, more asymmetric and less clumpy toward lower stellar masses, with bar fraction declining to zero near 10^8 solar masses and CAS parameters losing separating power in the dwarf regime.
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Advancing the detection of low surface brightness galaxies. I. ATTILA: multi-tAsking deTecTIon tool for Lsb gAlaxies
ATTILA tool identifies 24 new ultra-diffuse galaxies in Hydra I, doubling the known population to 48, plus 92 additional low surface brightness galaxies, while recovering over 80% of previously known ones.
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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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Galaxy Populations in the IllustrisTNG Caustic Skeleton
Galaxy properties in IllustrisTNG form a continuum across the multiscale caustic skeleton, with formation time of web components influencing colors and star formation activity.