Anisotropic quenching is detected at the highest redshift yet and linked to preprocessing dominating over intrahalo effects by ~20% along the major axis in a delay-then-rapid quenching model informed by cluster accretion histories.
The reversal of the star formation-density relation in the distant universe
6 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We study the relationship between the local environment of galaxies and their star formation rate (SFR) in the Great Observatories Origins Deep Survey, GOODS, at z~1, from ultradeep imaging at 24 microns with the MIPS camera onboard Spitzer. We show that the star formation-density relation observed locally was reversed at z~1: the average SFR of an individual galaxy increased with local galaxy density when the universe was less than half its present age. Hierarchical galaxy formation models (simulated lightcones from the Millennium model) predicted such a reversal to occur only at only at earlier epochs (z>2) and at a lower level. We present a remarkable structure at z~1.016, containing X-ray traced galaxy concentrations, which will eventually merge into a Virgo-like cluster. This structure illustrates how the individual SFR of galaxies increases with density at the ~1-2 Mpc scale. The SFR of z~1 galaxies is found to correlate with stellar mass suggesting that mass plays a role in the observed star formation-density trend. However the specific SFR (=SFR/M*) decreases with stellar mass while it increases with galaxy density, which implies that the environment does directly affect the star formation activity of galaxies. Major mergers do not appear to be the unique or even major cause for this effect since nearly half (46%) of the luminous infrared galaxies (LIRGs) at z~1 present the HST-ACS morphology of spirals, while only a third present a clear signature of major mergers. The remaining galaxies are divided into compact (9%) and irregular (14%) galaxies. Moreover, the specific SFR of major mergers is only marginally stronger than that of spirals. Reproducing the SFR-density relation at z ~ 1 is a new challenge for models, requiring a correct balance between mergers and in-situ star formation at early epochs.
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astro-ph.GA 6years
2026 6representative citing papers
At fixed stellar mass, inner gas mass—not size, SFR, or potential—best predicts gas metallicity, and differences in long-term inflow histories can explain the pattern.
Low-mass Paβ emitters in the Spiderweb protocluster show enhanced star formation rates compared to field galaxies, with no significant deviation at higher masses.
Massive post-starburst galaxies at 1<z<2 show no mid-IR excess, limiting any dust-obscured AGN to Eddington ratios below 1%, while low-mass PSBs retain residual star formation.
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
PSD modeling of SFR scatter at six timescales shows dominant variability on 10-30 Myr scales, stronger in lower-mass galaxies at z=3-8.
citing papers explorer
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Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters
Anisotropic quenching is detected at the highest redshift yet and linked to preprocessing dominating over intrahalo effects by ~20% along the major axis in a delay-then-rapid quenching model informed by cluster accretion histories.
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Beyond the Fundamental Metallicity Relation: galaxy sizes encode the link between inflow and metallicity
At fixed stellar mass, inner gas mass—not size, SFR, or potential—best predicts gas metallicity, and differences in long-term inflow histories can explain the pattern.
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Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\beta$ narrow-band imaging
Low-mass Paβ emitters in the Spiderweb protocluster show enhanced star formation rates compared to field galaxies, with no significant deviation at higher masses.
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No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam
Massive post-starburst galaxies at 1<z<2 show no mid-IR excess, limiting any dust-obscured AGN to Eddington ratios below 1%, while low-mass PSBs retain residual star formation.
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On the later evolution of observationally selected protocluster candidates at $z\,{\gtrsim}\,5$
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
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Star-formation variability on the star-forming main sequence during the Epoch of Reionization
PSD modeling of SFR scatter at six timescales shows dominant variability on 10-30 Myr scales, stronger in lower-mass galaxies at z=3-8.