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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17 Pith papers cite this work, alongside 9,121 external citations. Polarity classification is still indexing.
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representative citing papers
The [CII]-to-molecular gas conversion factor evolves from over 10,000 to about 10 solar masses per solar luminosity as galaxies enrich from very low metallicity at high redshift to higher values later, making a redshift-independent factor unusable.
First ALMA [CII] observations of high-redshift quiescent galaxies reveal gas fractions from 0.1% to 25%, dust temperatures of 40-50 K, strong [CII] deficits, and merger-like features, suggesting merger-driven quenching with non-stellar dust heating.
Simulations reveal that two-parameter extinction PDFs fit SN Ia data better than the exponential, implying intrinsically redder supernovae by about 2 sigma.
High-resolution molecular gas observations show that spiral arms and bars in z~1.5 disk galaxies drive substantial radial inflows at rates matching star formation, linking morphology directly to gas transport.
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.
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.
Euclid identifies 16 massive compact galaxies with V-shaped SEDs at z>4, half as old as the universe at their redshift, mostly distinct from known AGN.
M51 group shows more advanced dynamical evolution than M101, with flattened age and nebular metallicity gradients, enhanced dust, and environmental quenching signatures from interactions.
AGN obscuration classifications mismatch in ~30% of cases, with broad-line X-ray-absorbed and narrow-line X-ray-unabsorbed populations showing distinct gas-to-dust ratios and host properties, indicating obscuration arises from both orientation and multi-scale distributions.
A z=1.74 cluster has 18% red galaxies and a merging proto-BCG of 5.7e11 solar masses, implying Euclid will find ~400 assembling BCGs.
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.
NGC 1427A shows a complex star formation history with young (~10 Myr) and intermediate-age (100-300 Myr) clusters that trace environmental processing during its orbit in the Fornax cluster.
New adaptive optics data from nine LIRGs yields undetectable CCSN fractions of 88% for optical and 61% for near-IR surveys when combined with prior results.
X-ray AGN at intermediate redshifts live in dark matter halos of mass ~10^13 solar masses with no significant dependence on black hole mass, Eddington ratio or X-ray luminosity.
MIR diagnostics and X-ray stacking on 1104 X-ray-undetected AGNs in COSMOS identify 23 CT-AGN candidates at 2.1 percent of the sample, far below the ~30 percent expected from CXB synthesis models.
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 evolution of the [CII]-to-molecular gas relation
The [CII]-to-molecular gas conversion factor evolves from over 10,000 to about 10 solar masses per solar luminosity as galaxies enrich from very low metallicity at high redshift to higher values later, making a redshift-independent factor unusable.
-
A first [CII] view of high-z quiescent galaxies
First ALMA [CII] observations of high-redshift quiescent galaxies reveal gas fractions from 0.1% to 25%, dust temperatures of 40-50 K, strong [CII] deficits, and merger-like features, suggesting merger-driven quenching with non-stellar dust heating.
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Examining extinction distributions for type Ia supernovae in simulated 3D galaxies
Simulations reveal that two-parameter extinction PDFs fit SN Ia data better than the exponential, implying intrinsically redder supernovae by about 2 sigma.
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NOEMA3D: Resolving radial gas flows in disk galaxies at z~1.1-1.6 with high-resolution CO observations
High-resolution molecular gas observations show that spiral arms and bars in z~1.5 disk galaxies drive substantial radial inflows at rates matching star formation, linking morphology directly to gas transport.
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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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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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Euclid: Scaled-up little red dots and other sources with v-shaped spectral energy distributions at z>4
Euclid identifies 16 massive compact galaxies with V-shaped SEDs at z>4, half as old as the universe at their redshift, mostly distinct from known AGN.
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Analysis of spatially resolved stellar populations and emission line properties in nearby galaxies with J-PLUS data. II-Results for the M51 group and first comparison with the M101 group
M51 group shows more advanced dynamical evolution than M101, with flattened age and nebular metallicity gradients, enhanced dust, and environmental quenching signatures from interactions.
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AGN obscuration in optical and X-rays: Host properties and the interplay of nuclear and galactic gas and dust in a combined SDSS-XMM sample
AGN obscuration classifications mismatch in ~30% of cases, with broad-line X-ray-absorbed and narrow-line X-ray-unabsorbed populations showing distinct gas-to-dust ratios and host properties, indicating obscuration arises from both orientation and multi-scale distributions.
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Euclid: A blue galaxy population and a brightest cluster galaxy in the making in a $z\sim1.74$ MaDCoWS2 galaxy cluster candidate
A z=1.74 cluster has 18% red galaxies and a merging proto-BCG of 5.7e11 solar masses, implying Euclid will find ~400 assembling BCGs.
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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.
-
The complex history of NGC 1427A revealed by its star clusters and star formation history
NGC 1427A shows a complex star formation history with young (~10 Myr) and intermediate-age (100-300 Myr) clusters that trace environmental processing during its orbit in the Fornax cluster.
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The undetectable fraction of core-collapse supernovae in luminous infrared galaxies -- II. GSAOI/GeMS dataset
New adaptive optics data from nine LIRGs yields undetectable CCSN fractions of 88% for optical and 61% for near-IR surveys when combined with prior results.
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Large-scale environments of star-forming active galactic nuclei: How black hole mass, accretion rate, and luminosity connect to dark matter halos
X-ray AGN at intermediate redshifts live in dark matter halos of mass ~10^13 solar masses with no significant dependence on black hole mass, Eddington ratio or X-ray luminosity.
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Identifying Compton-thick active galactic nuclei in the COSMOS. II. Searching among mid-infrared selected AGNs
MIR diagnostics and X-ray stacking on 1104 X-ray-undetected AGNs in COSMOS identify 23 CT-AGN candidates at 2.1 percent of the sample, far below the ~30 percent expected from CXB synthesis models.
- Clues to inside-out quenching in quiescent galaxies at $1.2\lesssim z\lesssim2.2$: Age, Fe-, and Mg-abundance gradients from JWST-SUSPENSE