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REVIEW 3 major objections 4 minor 165 references

Radio jets from central galaxies quench star formation in their satellites, with the strongest effect around AGNs that drive large radio lobes.

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2026-07-12 06:57 UTC pith:VYYUD267

load-bearing objection Largest matched sample shows radio jets (especially FR-II lobes) raise quiescent satellite fractions in groups by a few to ~10 percent; solid empirical step on conformity, but residual assembly bias and N=130 FR-IIs keep the causal claim provisional. the 3 major comments →

arxiv 2607.02801 v1 pith:VYYUD267 submitted 2026-07-02 astro-ph.GA

Satellite quenching by radio jets of central galaxies in galaxy groups

Yijun Wang (1) , Tao Wang (1) , Dingyi Zhao (2) , Yingjie Peng (2) , Ziwen Zhang (3) , Houjun Mo (4) , Feng Yuan (5) , Zhaozhou Li (1)
show 13 more authors
Lingyu Wang (6 7) Yu Qiu (8) Yangyao Chen (1) Ke Xu (1) ((1) Nanjing University (2) Peking University (3) University of Science Technology of China (4) University of Massachusetts Amherst (5) Fudan University (6) SRON Netherlands Institute for Space Research (7) University of Groningen (8) Guilin University of Technology)
This is my paper
classification astro-ph.GA
keywords Radio galaxiesAGN feedbackGalaxy groupsSatellite galaxiesStar formation quenchingGalaxy evolutiongalactic conformity
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper argues that mechanical (jet-mode) feedback from active galactic nuclei reaches beyond the host galaxy and quenches star formation in satellite galaxies inside groups. Using the largest available sample of radio AGNs in SDSS groups and repeatedly matching on host halo mass, redshift, and the central galaxy’s stellar mass and star-formation rate, the authors find a higher quiescent satellite fraction around radio AGNs than around ordinary centrals. The excess is largest for FR-II sources with extended radio lobes (roughly 10 percent) and is still present, though smaller, for compact-core radio AGNs; optical AGNs show no clear quenching. The result supplies a concrete physical driver for two long-standing observational puzzles—galactic conformity and the strong small-scale clustering of quiescent galaxies—and implies that models of satellite quenching must include kinetic feedback from the central black hole.

Core claim

After matching groups on halo mass, redshift, central stellar mass and star-formation rate, the quiescent satellite fraction within one virial radius is higher around radio AGNs (total Δfq ≈ 3–4 percent) and especially around FR-II sources with large radio lobes (total Δfq ≈ 10–12 percent) than around normal galaxies. The excess is stronger at small projected radii and in lower-mass groups; optical AGNs produce no statistically significant quenching of satellites.

What carries the argument

Repeated construction of target–control pairs (radio-AGN, FR-II and optical-AGN groups versus normal-galaxy groups) matched in host halo mass, redshift, central stellar mass and SFR, followed by measurement of the differential quiescent satellite fraction Δfq as a function of projected radius and halo mass.

Load-bearing premise

Matching only on halo mass, redshift and the central galaxy’s mass and star-formation rate is assumed to eliminate every other difference that could make satellites around radio AGNs more quiescent, even though halo assembly history and black-hole properties remain unmatched.

What would settle it

A larger matched sample that also equalizes independent proxies for halo assembly history (or black-hole mass and spin) and still recovers a statistically significant positive Δfq would support the claim; recovery of Δfq consistent with zero after that extra matching would falsify it.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Kinetic AGN feedback heats or magnetizes the circumgalactic medium enough to suppress cooling onto satellites.
  • Galactic conformity can arise because the same jets that help quench the central also quench its satellites.
  • Part of the strong small-scale clustering of quiescent galaxies reflects shared jet-mode environments.
  • Galaxy-formation models that omit satellite quenching by central jets will under-predict the quiescent satellite fraction, especially in groups.
  • The effect is most visible in lower-mass halos where conventional halo quenching has not yet taken over.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Because jet activity can be re-triggered and its heating may linger, currently radio-quiet centrals with past jet episodes could still show elevated satellite quiescence.
  • High-redshift JWST systems in which a quiescent galaxy sits near a powerful AGN neighbour may be analogues of the same process operating at earlier epochs.
  • If the quenching is driven by lobe–CGM interaction, satellites lying along the jet axis should be more quenched than those lying perpendicular to it—an orientation test that future radio–optical catalogues can perform.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper constructs the largest sample to date of radio AGNs (and FR-II sources with extended lobes) in SDSS groups at 0.01 < z < 0.2 and compares the quiescent satellite fraction fq around them to carefully matched normal-galaxy controls. Matching is performed on host halo mass (two independent estimators), redshift, central stellar mass and central SFR, with 100 random control draws and beta-distribution errors. After matching, fq is elevated by ~3.5 % around compact radio AGNs and by ~10–12 % around FR-II sources (stronger at small projected radii and in lower-mass halos), while optical AGNs show no significant excess. The authors interpret the excess as kinetic (jet-mode) AGN feedback acting on the CGM and thereby quenching satellites, and they link the result to galactic conformity and the small-scale clustering of quiescent galaxies.

Significance. If the residual-bias concerns can be adequately addressed, the result would be a genuine advance: it supplies the first large-sample, multi-parameter-matched evidence that kinetic AGN feedback from group centrals reaches satellite galaxies, and it offers a concrete physical channel for galactic conformity and the strong small-scale clustering of quiescent galaxies. The dual halo-mass estimators, repeated control matching, and conventional SFMS cut are methodological strengths that make the empirical measurement itself robust and falsifiable. The work therefore has clear potential impact on both observational and theoretical galaxy-formation studies.

major comments (3)
  1. Materials and methods (matching criteria, Eq. 1) and Discussion: the central causal claim attributes Δfq to contemporaneous kinetic feedback, yet halo assembly history, black-hole spin/mass and prior jet episodes remain unmatched. Radio-loud centrals are known to prefer earlier-forming environments even at fixed Mh and M★; residual assembly bias or long-lived CGM heating from earlier episodes can produce a Δfq of the observed size without present-day jet–satellite interaction. Matching on instantaneous central SFR does not close this channel. A quantitative residual-bias test (e.g., using available assembly-history proxies or a mock-catalogue exercise) is needed before the causal interpretation can be regarded as secure.
  2. Results (Figs. 1–3) and sample summary: the FR-II sample comprises only 130 groups. While the total Δfq ~10–12 % is formally significant, the small N makes the result sensitive to a modest residual bias of the kind noted above and to the precise visual-cleaning cuts applied to the FR-II catalogues. The paper should either enlarge the FR-II sample or demonstrate that the signal survives jackknife or leave-one-out tests that quantify the influence of individual systems.
  3. Results (Fig. 1, optical-AGN panels) and Materials and methods: the optical-AGN Δfq changes sign depending on which halo-mass estimator is adopted. This estimator dependence weakens the claim that radiative feedback has no effect and raises the possibility that residual systematics in Mh still affect the radio-AGN comparison. The paper should quantify how much of the radio-AGN Δfq could be absorbed by the same estimator difference and, if necessary, adopt a joint or consensus Mh prior.
minor comments (4)
  1. Materials and methods: the IMF and stellar-mass catalogue offsets (+0.025 and –0.07 dex) are applied, but the final completeness limit for satellites is stated only in prose; an explicit equation or table would aid reproducibility.
  2. Extended Data Figs. 1–6: the histograms of matched quantities are useful, but a quantitative Kolmogorov–Smirnov or Anderson–Darling statistic for each matched variable would strengthen the claim that the distributions are statistically indistinguishable.
  3. Discussion: the link to high-z JWST quiescent galaxies is intriguing but currently qualitative; a short quantitative estimate of the expected satellite-quenching radius or duty cycle would make the connection more concrete.
  4. Throughout: a few typographical inconsistencies appear (e.g., “GGM” vs “CGM”, “stallite” in Fig. 3 caption). A careful proof-read is needed.

Circularity Check

0 steps flagged

Empirical matched-sample comparison of quiescent fractions; no prediction reduces to a fit or self-cited uniqueness theorem.

full rationale

The paper's central result is an observational difference Δfq after explicit matching on Mh, z, M⋆,central and SFR,central (Materials and methods, Eqs. 1–8 and Figs. 1–3). Quiescent galaxies are defined by a conventional iterative SFMS fit to the same SDSS sample (Extended Data Fig. 7, Eqs. 2–3); the cut is not used to force the radio-AGN versus normal comparison. Halo-mass and group catalogues (Yang et al. 2007; Zhao et al. 2025) are self-cited data products, but the Δfq measurement itself is an independent statistical contrast performed on those catalogues and does not reduce by construction to any equation or uniqueness claim in the cited works. No ansatz is smuggled in, no fitted parameter is re-labelled a prediction, and the causal interpretation offered in the Discussion is post-hoc, not part of a circular derivation chain. Residual assembly-bias concerns are real scientific caveats but lie outside circularity.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The result is an observational comparison that rests on standard cosmological and catalog assumptions plus a few analysis choices (matching tolerances, SFMS offset, IMF corrections). No new physical entities are postulated; free parameters are limited to the matching windows and the 0.9 dex quiescent cut.

free parameters (3)
  • matching tolerances (Δlog Mh = 0.1, Δz = 0.04, Δlog M⋆ = 0.1, Δlog SFR = 0.1)
    Chosen by hand to define control samples; different windows would change sample size and possibly Δfq.
  • 0.9 dex offset below SFMS for quiescent classification
    Defines the QG/SFG boundary after iterative fitting of the main sequence; the numerical offset is conventional but free.
  • IMF and stellar-mass catalog offsets (+0.025 and −0.07 dex)
    Ad-hoc corrections applied to reconcile Chabrier/Kroupa and GSWLC/MPA-JHU mass scales before applying completeness limits.
axioms (4)
  • domain assumption Flat ΛCDM cosmology with Ωm = 0.3, ΩΛ = 0.7, H0 = 70 km s−1 Mpc−1 and Chabrier IMF
    Standard background used for distances, virial radii and stellar masses (Materials and methods).
  • domain assumption Brightness-ranked central is the true central galaxy of the group
    Adopted from Yang et al. (2007); used to define which galaxy’s radio activity is tested.
  • domain assumption Halo mass is the dominant environmental variable controlling satellite quenching; assembly history can be ignored once Mh is matched
    Explicitly stated; the paper notes assembly time is hard to constrain and therefore omitted.
  • domain assumption Radio-AGN and FR-II selection methods (Best & Heckman 2012 criteria, visual inspection, lobe-size cut >20 kpc) cleanly isolate kinetic-mode sources
    Sample purity rests on these published and visual criteria.

pith-pipeline@v1.1.0-grok45 · 27436 in / 2762 out tokens · 21950 ms · 2026-07-12T06:57:18.602720+00:00 · methodology

0 comments
read the original abstract

Feedback from active galactic nuclei (AGN) is now recognized as a key component of galaxy formation models. It plays a central role in regulating the growth and quenching of galaxies in the center of groups. However, the impact of AGN feedback from central galaxies on satellite galaxies remains largely unexplored. Here based on the largest sample to date of radio AGNs in galaxy groups (Yang et al. 2007) and a comprehensive consideration of multiple physical parameters that may influence the star formation of satellite galaxies, we demonstrate that the quiescent satellite fraction around radio AGNs is higher than that around normal galaxies. The most significant enhancement is observed around AGNs with large radio lobes. These findings demonstrate that the impact of kinetic AGN feedback beyond their host galaxies to their satellites. These results provide novel insights into the physical origins of some long-standing puzzles in extragalactic astronomy, including, e.g., galactic conformity and the strong small-scale clustering of quiescent galaxies.

discussion (0)

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Reference graph

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