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Deep Extragalactic VIsible Legacy Survey (DEVILS): The sSFR-M$_{\star}$ plane part II: Starbursts, SFHs and AGN Feedback

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read This paper claims that AGN feedback, traced by X-ray, radio, and SED-selected AGN, is the primary driver of the high specific star-formation rate dispersion at high stellar mass.

desk verdict Careful, honest DEVILS study that makes a plausible case for AGN feedback as the high-mass quenching driver; the ProSpect SFH shape caveat is real but the paper's independent AGN checks and mass-matched SFH comparison keep the claim standing. read the letter →

arxiv 2505.21948 v1 pith:C4VHR2RG submitted 2025-05-28 astro-ph.GA

L. J. M. Davies , J. E. Thorne , S. Bellstedt , R. H. W. Cook , M. Bravo , A. S. G. Robotham , C. del P. Lagos , S. Phillipps
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M. Siudek B. W. Holwerda M. N. Bremer J. D'Silva S. P. Driver
This is my paper · ORCID
classification astro-ph.GA
keywords starformationhistoriesAGNfeedbackgalaxyquenchingsSFR-M*planeSFRdispersionDEVILSSEDfittingevolution
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that the processes moving galaxies through the specific star-formation rate versus stellar mass plane split cleanly at the stellar mass where SFR dispersion is smallest, the $M_\star^{\sigma-\mathrm{min}}$ point. Below that mass, large SFR scatter comes from stochastic star formation and a wide spread of constant star-formation histories, not from AGN. Above it, galaxies with sharply declining star-formation histories host an overabundance of AGN, so the paper concludes that AGN feedback is the primary cause of high SFR dispersion and galaxy quenching at high stellar mass. The evidence is that the AGN overabundance is bounded by $M_\star^{\sigma-\mathrm{min}}$ at every redshift epoch studied.

What carries the argument

The mechanical core is the $\Delta\mathrm{SFH}_{200\,\mathrm{Myr}}$ metric, the change in a galaxy's star-formation rate over the last 200 Myr, derived from ProSpect's parametric skew-log-normal truncated SFH fits. This reduces recent SFH shape to a single signed number, with negative values meaning declining star formation. The paper combines this with the $M_\star^{\sigma-\mathrm{min}}$ point, the stellar mass at which SFR dispersion is minimal, to separate two regimes, and with AGN selection from SED, X-ray, and radio to test correlations. The key identity is the proportionality between the AGN overabundance region and the high-dispersion region above $M_\star^{\sigma-\mathrm{min}}$.

What would settle it

Compare ProSpect-derived $\Delta\mathrm{SFH}_{200\,\mathrm{Myr}}$ for the same DEVILS galaxies against spectroscopically measured star-formation histories (for example from stacked high-signal-to-noise spectra) or against non-parametric SED fits; if the declining-SFH population shows no systematic negative $\Delta\mathrm{SFH}_{200\,\mathrm{Myr}}$ and no AGN overabundance, the central claim fails.

Watch

Extended reading notes

Core claim

The central discovery is that AGN activity and rapidly declining star formation are spatially coincident in the high-mass region of the sSFR-$M_\star$ plane, and that this coincidence tracks the evolving minimum-dispersion mass $M_\star^{\sigma-\mathrm{min}}$ at all epochs. Galaxies with strongly negative $\Delta\mathrm{SFH}_{200\,\mathrm{Myr}}$ above $M_\star^{\sigma-\mathrm{min}}$ show an overabundance of AGN whether selected by ProSpect SED fitting, Chandra X-ray, or MIGHTEE radio, while low-mass high-dispersion galaxies show flat SFHs and no AGN excess. The paper interprets this as direct observational support for AGN feedback causing quenching at high stellar masses.

Load-bearing premise

The argument collapses if ProSpect's smooth, skewed log-normal star-formation histories systematically misclassify real galaxies as declining in star formation, because then the rapidly quenching class and its AGN association are manufactured by the fitting method.

Editorial extensions

If this is right

  • If AGN feedback quenches high-mass galaxies, the high stellar mass end of the star-forming main sequence is a population caught mid-quenching, not a self-regulated sequence.
  • The minimum SFR dispersion point marks the threshold stellar mass below which AGN feedback is too weak to drive galaxies off the sequence.
  • Different AGN selection methods probe different phases of the quenching process: X-ray AGN are associated with ongoing rapid decline, while radio AGN are associated with past or slower decline.
  • The decline of the star-forming population toward low redshift is partly driven by AGN-triggered quenching that moves to lower stellar masses as the Universe evolves.
  • The rapidly quenching population shows no strong morphological or structural difference from main-sequence galaxies, implying structure change follows, not precedes, the quenching event.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A testable extension: if the parametric SFH form biases recent SFHs toward declining shapes, some of the rapidly quenching class would be an artifact, and a non-parametric SFH fit on the same photometry would settle whether the AGN association survives.
  • The paper does not include environment, which could also drive quenching at intermediate masses; adding group halo masses might move some slow-quenching galaxies from AGN causality to environment causality.
  • A prediction of the AGN-feedback picture is that the mass threshold $M_\star^{\sigma-\mathrm{min}}$ should correlate with the AGN luminosity function cutoff across cosmic time.
  • If confirmed with direct spectroscopic SFHs from high-signal-to-noise spectra of the same galaxies, the result would turn AGN feedback from a simulation requirement into a directly observed quenching mechanism.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper uses ProSpect-derived recent star-formation histories (SFH) for DEVILS D10 galaxies, quantified by ΔSFH_200Myr, to partition the sSFR–M* plane into regions of common recent SFH and to search for physical drivers of the measured σ_SFR–M* relation. The authors report two regimes separated by the minimum-dispersion stellar mass M*_σ-min: at lower stellar masses the large sSFR dispersion is attributed to a combination of stochastic star formation and constant-SFH galaxies with diverse sSFR normalizations, while at higher stellar masses galaxies with rapidly declining SFHs show a strong overabundance of AGN by ProSpect, Chandra X-ray, and MIGHTEE radio selections. The paper interprets this as observational evidence that AGN feedback is the primary driver of high σ_SFR at high stellar masses.

Significance. If the result holds, this is a valuable observational constraint: it directly connects a frequently used aggregate statistic (the sSFR–M* dispersion) to a physical quenching mechanism, and it does so with three independent AGN selections. The paper's strengths include the explicit prior-sensitivity refits (Section 2.3, Figure 2), the SHARK-based recovery validation (median offset 0.01, MAD 0.05), the no-AGN refit checks discussed in Section 3.2.2, and the stellar-mass-matched SFH comparison in Section 3.3. The central caveat is that ΔSFH_200Myr is a parametric quantity derived from a skew-log-normal SFH, and the recovery validation is performed on smooth mock SFHs; if the functional form biases real, more diverse SFHs toward declining shapes, the rapidly quenching class and its AGN association would be partly an artifact. The manuscript is candid about this limitation, but the issue is load-bearing and needs a more demanding test.

major comments (3)
  1. [Section 3.2.2, paragraph beginning 'One possible issue with this analysis'] The definition of the rapidly quenching class rests entirely on ΔSFH_200Myr values recovered by ProSpect under a truncated skew-log-normal SFH. The paper itself states that the peaked ΔSFH distribution is 'driven by the overall methodology using a skew-log-normal distribution,' and Figure 2 shows that the observed negative-side distribution tracks the distribution generated from random prior draws. The only recovery validation (median offset 0.01, MAD 0.05) is against SHARK mock galaxies whose SFHs are smooth parametric forms, so it does not test whether episodic, step-like, or otherwise non-smooth real SFHs are recovered without a systematic bias toward declining shapes. Because a bias of this kind would create the rapidly declining population and hence the AGN overabundance in Figures 5 and 6, I request an additional recovery test using non-smooth SFHs (or a non-parametric refit of a subset of DEVILS galaxies) and a quantitative statement of how large a ΔSFH bias would be required to erase the observed AGN excess.
  2. [Section 3.3 / Figure 7] The claim that refitting without an AGN component produces 'almost no difference' in the positions of X-ray and radio AGN in the ΔSFH_200Myr and sSFR planes is asserted but not shown quantitatively. Since this is the key check that the AGN–SFH association is not induced by jointly fitting the AGN component and the SFH, the paper should present the equivalent distributions (or a table of median offsets and AGN fractions) for the no-AGN fits. Without those numbers, the independence of the central result from co-fitting remains a matter of assertion rather than demonstration.
  3. [Section 3.3 / Figure 7] The stellar-mass-controlled comparison in Figure 7 is used to argue that X-ray AGN are associated with an ongoing quenching event and radio AGN with a past one, based on the running slope of the median SFH relative to the non-AGN sample. The plotted Poisson error polygons on the median SFHs do not directly quantify the uncertainty on the running-slope difference, and no statistical test is given for the divergence at ~1 Gyr in the X-ray panel. Given the small number of radio-loud AGN (497 in the full sample) and the non-unique membership across AGN classes, bootstrap confidence intervals on the running slopes or a formal comparison test are needed to support the different-phases interpretation.
minor comments (5)
  1. [Abstract] The abstract contains a typo: 'can be be largely split' should read 'can be largely split'.
  2. [Section 2.3] The sentence 'we are argue that there is no evidence' should be corrected to 'we argue that there is no evidence'.
  3. [Section 2.2 / Section 4.1.3] The quantity M*_σ-min is used throughout but is not defined in this paper; a one-sentence definition referring to D22 (or Paper I) would make the paper more self-contained.
  4. [Figure 5 and Figure 6] The axis label 'ΔSFR200Myr' appears in Figure 5's color bar label while the text consistently uses ΔSFH_200Myr; please use a single notation throughout.
  5. [Appendix A2] The text refers to 'Cook et al (in prep)' while the reference list contains Cook et al. (2025); please unify the citation.

Circularity Check

0 steps flagged · score 2.0 of 10

No constructional circularity: the AGN–SFH association is tested with X-ray and radio AGN independent of the ProSpect fit, and the co-fit degeneracy is explicitly controlled.

full rationale

The central empirical claim is that galaxies with rapidly declining recent SFHs at stellar masses above M*_sigma-min show an overabundance of AGN, and that this supports AGN feedback as the driver of high sSFR dispersion. This is not a self-definitional result: the recent SFH metric DeltaSFH_200Myr is derived from ProSpect SED fitting, while AGN are selected by three independent methods. The X-ray (Chandra COSMOS-Legacy) and radio (MIGHTEE) AGN samples are external catalogues that do not use the ProSpect AGN component, so the AGN–SFH correlation is not forced by construction. The paper explicitly acknowledges the potential degeneracy in Section 3.2.1, where in-situ sSFR, DeltaSFH_200Myr and AGN luminosity are all ProSpect-derived, and then breaks this degeneracy in Section 3.2.2 by repeating the comparison using ProSpect fits without an AGN component, finding almost no difference for X-ray and radio AGN. The M*_sigma-min boundary is imported from the same team's D22 work, but it is a previously measured population property, not a parameter fitted to the AGN–DeltaSFH correlation, and the fact that the AGN overabundance tracks this boundary is a new comparison rather than an identity. The main vulnerability is the parametric skew-log-normal SFH assumption, which the paper itself concedes shapes the DeltaSFH_200Myr distribution (Section 2.3), and the recovery validation is performed on SHARK mock galaxies from same-team simulation papers. This is a genuine methodological limitation and a moderate self-citation load, but it is not a circular reduction: no equation equates the AGN excess to the SFH functional form, and the independent X-ray and radio selections preserve external content. The causal statement that AGN feedback is the 'primary driver' is explicitly framed as a suggestion consistent with theory, not as a derived consequence. Overall, the derivation chain is not circular in the constructional sense; the score of 2 reflects the admitted model dependence and the heavy reliance on same-team validation rather than any by-construction equivalence.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The central classification variable ΔSFH_200Myr is a derived output of the ProSpect parametric fit, so every population label in the paper inherits the fitting assumptions (axioms 1 to 3). The regime boundary M*_σ-min comes from the same team's D22 measurement, and the six regions from the same team's paper I, so the interpretive scaffolding is largely self-referential even though the measured correlations are new. No new physical entities are introduced: the AGN studied are standard supermassive-black-hole accretion states selected by conventional multi-wavelength methods, so the invented-entities ledger is empty.

free parameters (4)
  • ProSpect SFH shape parameters (mSFR, mpeak, mperiod, mskew, Zfinal) = Fitted per galaxy to broadband photometry (Thorne et al. 2022)
    These set ΔSFH_200Myr, the variable that defines every common-SFH class in this paper; the SHARK recovery validation (MAD 0.05) bounds but does not remove the dependence of the classification on the fitted shape.
  • Common-SFH region boundaries (regions 1 to 6) = Hand-drawn from binned median ΔSFH in paper I (Figure 1 here)
    All population comparisons inherit these boundaries, which are not derived from a model or external benchmark.
  • AGN fraction threshold = 0.1 (Thorne et al. 2022)
    Defines SED-selected AGN in Figure 4; the paper notes this method can mis-identify low-luminosity AGN in low signal-to-noise sources.
  • AGN luminosity thresholds = 10^41 erg/s analysis cut and D'Silva et al. (2023) completeness limits
    Galaxies below 10^41 erg/s are treated as non-AGN in the Figure 4 comparisons; the completeness-limited definition drives the Figure 5 over-density maps.
assumptions (6)
  • domain assumption ProSpect's skew-log-normal truncated SFH is an appropriate functional form for galaxy SFHs
    The paper tests this via SHARK simulations (median ΔSFH offset 0.01, MAD 0.05) and prior-sensitivity fits (Section 2.3), but the functional form itself shapes the ΔSFH distribution, a point the paper concedes.
  • domain assumption Change in SFR over the last 200 Myr (ΔSFH_200Myr) captures a galaxy's trajectory through the sSFR-M★ plane
    Defined in Section 2.3; this single number replaces the full SFH shape, and the paper cannot probe bursts shorter than about 100 Myr.
  • domain assumption SHARK semi-analytic model galaxies are a valid proxy for real galaxies in testing SFH recovery
    Recovery test in paper I and Section 2.3; errors measured on mock photometry are assumed to transfer to DEVILS data.
  • standard math Bruzual and Charlot (2003) templates with Chabrier (2003) IMF and the Charlot and Fall (2000) and Dale et al. (2014) dust models are valid
    Standard SED fitting ingredients, Section 2.3; the paper notes Bellstedt and Robotham (2024) found template choice dominates over methodology choice.
  • domain assumption The minimum SFR dispersion mass M*_σ-min (D22) is a physically meaningful boundary between evolution regimes
    The two-regime interpretation (Section 4.1) and the AGN tracking result (Figures 5 and 6) both hinge on this point from the authors' own prior measurement.
  • domain assumption AGN fraction greater than 0.1 from ProSpect and the D'Silva et al. (2023) AGN completeness limits reliably identify AGN in SED fits
    Used throughout Section 3.2; the paper notes the AGN fraction can be unreliable without FIR detections.

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Cite this review

Pith. "Pith review of Deep Extragalactic VIsible Legacy Survey (DEVILS): The sSFR-M$_{\star}$ plane part II: Starbursts, SFHs and AGN Feedback." pith.science (2026). https://pith.science/paper/C4VHR2RG

@misc{pith2026250521948,
  author       = {Pith},
  title        = {Pith review of: Deep Extragalactic VIsible Legacy Survey (DEVILS): The sSFR-M$_\star$ plane part II: Starbursts, SFHs and AGN Feedback},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/C4VHR2RG}},
  note         = {Machine review of arXiv:2505.21948}
}
abstract

In part I of this series we discussed the variation of star-formation histories (SFHs) across the specific star formation rate - stellar mass plane (sSFR-M$_{\star}$) using the Deep Extragalactic VIsible Legacy Survey (DEVILS). Here we explore the physical mechanisms that are likely driving these observational trends, by comparing the properties of galaxies with common recent SFH shapes. Overall, we find that the processes shaping the movement of galaxies through the sSFR-M$_{\star}$ plane can be be largely split into two stellar mass regimes, bounded by the minimum SFR dispersion ($\sigma_{SFR}$) point. At lower stellar masses we find that large $\sigma_{SFR}$ values are likely observed due to a combination of stochastic star-formation processes and a large variety in absolute sSFR values, but relatively constant/flat SFHs. While at higher stellar masses we see strong observational evidence that Active Galactic Nuclei (AGN) are associated with rapidly declining SFHs, and that these galaxies reside in the high $\sigma_{SFR}$ region of the plane. As such, we suggest that AGN feedback, leading to galaxy quenching, is the primary driver of the high $\sigma_{SFR}$ values. These results are consistent with previous theoretical interpretations of the $\sigma_{SFR}$-M$_{\star}$ relation.

Figures

Figures reproduced from arXiv: 2505.21948 by the authors.

Figure 1
Figure 1. Summary of the sample selection undertaken in paper I to identify galaxies with common recent SFHs. Here we only show galaxies at 0.4 < 𝑧 < 0.55. The left panel displays the sSFR-M★ plane, with points colour-coded by the slope of their recent SFH (ΔSFH200 Myr). These have been split into various bands of ΔSFH200 Myr given in the legend above the figure (see paper I for details). Galaxies with common ΔSFH200 Myr fall… view at source ↗
Figure 2
Figure 2. Potential impact of choice of ProSpect priors on derived ΔSFH200 Myr values. Blue displays the ΔSFH200 Myr values for the DEVILS sample, red shows the resultant ΔSFH200 Myr values produced from SFHs gen￾erated from random sample of the priors described in Thorne et al. (2022), green shows distribution of ΔSFH200 Myr values from refits to a random 2000 galaxies in the DEVILS sample using broadened priors, while gold … view at source ↗
Figure 3
Figure 3. Comparison of the distribution of morphological/structural physical properties of galaxies selected to have common SFHs. Top row: the full sample with common SFHs selected using the region in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Comparison of the distribution of ProSpect-selected AGN properties of galaxies selected to have common SFHs. Top row: the full sample with common SFHs selected using the region in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p009_4.png]
Figure 5
Figure 5. Figure 5: Normalised fraction of AGN sources in [M★,ΔSFR200 𝑀𝑦𝑟 ] bins divided by the normalised fraction of all sources in the [M★,ΔSFR200 𝑀𝑦𝑟 ] bins. AGN here are selected to have ProSpect AGN luminosities above the completeness limits derived in D’Silva et al. (2023). This fi…
Figure 6
Figure 6. Figure 6: Left: The position of AGN selected via various methods at 0.4 < 𝑧 < 0.7 in the ΔSFH200 Myr vs stellar mass (top) and sSFR-M★ plane (bottom). We show sources detected as AGN from the ProSpect SED fitting that have an AGN luminosity greater than the limits outlined in D’…
Figure 7
Figure 7. Figure 7: The median SFH of galaxies selected at 10.75<log10(M★/M⊙)<11.25 and 0.4<z<0.7, split into non-AGN (red), ProSpect-luminous AGN (green), xray-selected AGN (purple) and radio-loud AGN (gold). The top left panel shows the stellar mass distribution of each subsample. We th…
Figure 8
Figure 8. Figure 8: Cartoon representation of the types of galaxies found in different regions of the sSFR-M★ plane (top) and how those populations are likely moving through the plane (bottom). See text for details. to better constrain galaxy SFHs (such as ProFuse, Robotham, Bell￾stedt, &…

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    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.