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.
J., Springel, V ., White, S
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High-resolution MUSE observations of 30 Gaia multipeak targets confirm 19 AGN multiplets including 6 dual AGN, accounting for 22% of known close pairs below 7 kpc and showing the selection method's efficiency.
Fast-rotating green valley galaxies maintain higher metallicities than slow-rotating ones because slow rotators experience stronger outflows and more mergers that deplete their chemical content.
X-ray AGN fraction increases with central star formation rate density in local galaxies, supporting coeval black hole and galaxy growth with only modest time-averaged AGN feedback effects.
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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Cosmic Duets I. High-spatial resolution spectroscopy of dual and lensed AGN with MUSE-NFM
High-resolution MUSE observations of 30 Gaia multipeak targets confirm 19 AGN multiplets including 6 dual AGN, accounting for 22% of known close pairs below 7 kpc and showing the selection method's efficiency.
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Contrasting evolutionary pathways of fast- and slow-rotating galaxies in the green valley
Fast-rotating green valley galaxies maintain higher metallicities than slow-rotating ones because slow rotators experience stronger outflows and more mergers that deplete their chemical content.
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Investigating central star formation in local AGN host galaxies: is there tension between coeval growth and AGN feedback?
X-ray AGN fraction increases with central star formation rate density in local galaxies, supporting coeval black hole and galaxy growth with only modest time-averaged AGN feedback effects.
- Clues to inside-out quenching in quiescent galaxies at $1.2\lesssim z\lesssim2.2$: Age, Fe-, and Mg-abundance gradients from JWST-SUSPENSE