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arxiv: 2606.20800 · v1 · pith:JWHIU53Rnew · submitted 2026-06-18 · 🌌 astro-ph.GA

No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam

Guillaume Hewitt , Omar Almaini , David Maltby , Emma Chapman , Thomas de Lisle , Pallavi Patil , Kate Rowlands , Maya Skarbinski
show 8 more authors
Elizabeth Taylor Vivienne Wild Adam C. Carnall James S. Dunlop Norman Grogin Anton M. Koekemoer Derek J. McLeod Pablo G. P\'erez-Gonz\'alez
This is my paper

Pith reviewed 2026-06-26 16:28 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords post-starburst galaxiesobscured AGNJWST MIRImid-infrared emissiongalaxy quenchingstellar mass dependencepassive galaxiesresidual star formation
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The pith

Massive recently-quenched galaxies lack mid-infrared excess that would indicate hidden AGN.

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

The paper studies 65 photometrically selected post-starburst galaxies at redshifts 1 to 2 with new JWST MIRI imaging at 7.7 and 18 microns combined with NIRCam and HST data. High-mass systems show no excess mid-infrared emission, matching the quiescent population, while low-mass systems display extra 18-micron light attributed to leftover star formation. Template fits then place an upper bound below 1 percent Eddington ratio on any dust-hidden AGN in the massive subset. A simple F770W minus F1800W color emerges as a clean separator between passive and star-forming galaxies at high stellar mass. These patterns indicate that massive and low-mass post-starburst galaxies reach quiescence by different routes.

Core claim

Combining JWST MIRI 7.7 and 18 micron imaging with eight NIRCam and three HST bands for 65 post-starburst galaxies at 1<z<2 reveals that most systems above 10^10 solar masses exhibit no mid-infrared excess, matching older passive galaxies and limiting any dust-enshrouded AGN to Eddington ratios below 1 percent. Low-mass post-starbursts instead show enhanced 18-micron emission consistent with residual star formation. The F770W-F1800W color alone separates passive from star-forming galaxies effectively, especially at high mass. The sample therefore supplies evidence for distinct quenching pathways and confirms that massive post-starbursts carry no detectable excess AGN activity relative to the

What carries the argument

Mid-infrared excess measured in JWST MIRI F770W and F1800W bands as a tracer of hot dust emission from either obscured AGN or residual star formation.

If this is right

  • High-mass post-starburst galaxies are consistent with the older passive population in their infrared properties.
  • Any dust-enshrouded AGN in massive post-starbursts must operate at Eddington ratios below 1 percent.
  • Low-mass post-starbursts retain residual star formation that produces the observed 18-micron enhancement.
  • The F770W-F1800W color provides an effective single-band diagnostic for separating passive and star-forming galaxies at high stellar mass.
  • Mass-dependent differences in infrared properties support separate quenching pathways for low-mass and high-mass post-starburst galaxies.

Where Pith is reading between the lines

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

  • The same mid-infrared color cut could be applied to wider-field JWST or future infrared surveys to classify large numbers of galaxies without full SED fitting.
  • Absence of AGN signatures at these wavelengths narrows the set of viable quenching mechanisms that must be modeled for massive galaxies.
  • Extending the same MIRI photometry to a larger sample at slightly higher or lower redshift would test whether the mass-dependent pattern persists across cosmic time.
  • X-ray or optical spectroscopic follow-up on the same targets could check whether low-level AGN activity exists below the mid-infrared detection threshold.

Load-bearing premise

The photometric selection plus SED fitting cleanly isolates recently quenched galaxies without substantial contamination from dusty star-forming or older passive systems.

What would settle it

Detection of mid-infrared excess above the quiescent level in a statistically significant fraction of massive post-starburst galaxies selected by the same photometric criteria would falsify the Eddington-ratio upper limit.

Figures

Figures reproduced from arXiv: 2606.20800 by Adam C. Carnall, Anton M. Koekemoer, David Maltby, Derek J. McLeod, Elizabeth Taylor, Emma Chapman, Guillaume Hewitt, James S. Dunlop, Kate Rowlands, Maya Skarbinski, Norman Grogin, Omar Almaini, Pablo G. P\'erez-Gonz\'alez, Pallavi Patil, Thomas de Lisle, Vivienne Wild.

Figure 1
Figure 1. Figure 1: Stellar mass of the sample galaxies against their photometric red￾shifts (or spectroscopic if available). The sample is selected from the F200W NIRCam filter image, with a magnitude completeness of mag < 26.5 for 0.5" apertures. Overlaid are the 90% stellar mass completeness curves of the star￾forming, quiescent, and PSB populations, following the procedure in Pozzetti et al. (2010). Since this work is foc… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Comparison of the F770W–F1800W colour of all quiescent and star-forming galaxies (as classified by the PCA technique), against their redshift. Each population is split at the stellar mass limit of 1010 M⊙, with the red and blue points showing the high-mass quiescent and high-mass star-forming population, respectively, and the light-red and light-blue points showing the respective low-mass populations… view at source ↗
Figure 3
Figure 3. Figure 3: Visualization of physical spectral features being probed by the F444W, F770W, and F1800W filters at 1 < 𝑧 < 2. Vertical grey columns correspond to the restframe of the filter effective wavelength probed across our redshift range (1 < 𝑧 < 2). The galaxy SED templates from Polletta et al. (2007) (Ell5, S0, Sb, M82, ULIRG) are normalized to 1.6 𝜇m, and the AGN templates from (Kirkpatrick et al. 2012) (featAGN… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of the F770W–F1800W colour and the F444W–F770W colour within the 1 < 𝑧 < 1.5 (left) and 1.5 < 𝑧 < 2 (right) redshift bins for the star-forming, quiescent, and PSB populations. Just like [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Colour-colour diagram of galaxies, matching the form shown in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Colour-colour locations and probability distributions of PSBs, and how their colours change with the addition of an AGN template accreting at various Eddington ratios. The left panels show the fiducial location of all MIR non-excess PSBs (F770W-F1800W values less than the vertical dashed line), and the right panels show the fiducial location of all MIR excess PSBs (with high-mass PSBs denoted as brown squa… view at source ↗
Figure 7
Figure 7. Figure 7: SEDs of PSBs with MIR non-excess (top) and with MIR excess (middle). They have been shifted to their rest wavelength values based on their redshifts, and normalized to their interpolated 1.6 𝜇m flux value. Each galaxy is coloured by their stellar mass values. The bottom panel compares the median SEDs of each population directly, again with the same normalization. The errors around the median is the standar… view at source ↗
read the original abstract

We investigate the role of obscured active galactic nuclei (AGN) in recently quenched post-starburst galaxies (PSBs), using a sample of 65 photometrically selected PSBs in the PRIMER-UDS field at $1 < z < 2$. Combining JWST/MIRI 7.7 $\mu$m and 18 $\mu$m (F770W and F1800W) imaging with eight NIRCam and three HST/ACS bands, we probe hot dust emission to test for hidden AGN or dust-enshrouded star formation. We find strong differences between the low- and high-mass PSBs. Most high-mass PSBs ($ > 10^{10}\textrm{M}_\odot$) show no excess infrared emission (consistent with the quiescent population), indicating little or no dust-obscured activity, while low-mass PSBs display enhanced emission at 18 $\mu$m, which we attribute to residual star formation. AGN template modelling indicates that the absence of mid-IR excess in massive PSBs limits any dust-enshrouded AGN to Eddington ratios of $ < 1\%$. In addition, we show that the F770W--F1800W colour alone is a highly effective diagnostic for separating passive and star-forming galaxies, particularly at high stellar masses. Overall, our results provide further evidence for distinct quenching pathways within the PSB population, and confirm that massive PSBs show no evidence for excess AGN activity relative to older passive galaxies.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript analyzes 65 photometrically selected post-starburst galaxies (PSBs) at 1<z<2 in the PRIMER-UDS field using JWST/MIRI 7.7μm and 18μm imaging combined with NIRCam and HST bands. It reports that high-mass PSBs (>10^10 M⊙) show no mid-IR excess (consistent with older quiescent galaxies), while low-mass PSBs exhibit enhanced 18μm emission attributed to residual star formation. AGN template modelling of the MIRI non-detections is used to limit any dust-enshrouded AGN in massive PSBs to Eddington ratios <1%. The F770W–F1800W color is presented as an effective separator of passive and star-forming systems, supporting distinct mass-dependent quenching pathways in the PSB population.

Significance. If the PSB selection is robust and the template-derived Eddington limit is well-justified, the work supplies direct mid-IR observational constraints against obscured AGN activity in massive recently-quenched systems and highlights mass-dependent differences within the PSB class. The proposed color diagnostic has potential utility beyond this sample. The JWST MIRI data provide a timely probe of hot dust that is not available from prior facilities.

major comments (2)
  1. [AGN template modelling paragraph] AGN template modelling paragraph (results section): The quantitative upper limit of Eddington ratios <1% for dust-enshrouded AGN in high-mass PSBs is derived from non-detections in the MIRI bands via template fitting. The manuscript must specify the AGN template library, the grid of obscuration parameters (e.g., N_H, covering factors, viewing angles), and the bolometric correction assumptions, because changes in these inputs can loosen or tighten the reported limit. This modelling step is load-bearing for the central claim of no hidden AGN.
  2. [Sample selection and completeness discussion] Sample selection and completeness discussion: The photometric criteria used to isolate the 65 PSBs must include quantitative tests for contamination by dusty star-forming galaxies or older passive systems, particularly to substantiate the reported differences between low- and high-mass bins. Without such validation, the mass-dependent IR properties cannot be unambiguously attributed to distinct quenching pathways.
minor comments (1)
  1. The abstract states 'eight NIRCam and three HST/ACS bands' but does not list the specific filters; these should be enumerated in the methods section for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report. We agree that both major comments identify areas where the manuscript can be strengthened with additional detail and validation. We will revise accordingly to make the AGN modeling assumptions fully transparent and to add quantitative tests supporting the sample selection.

read point-by-point responses

  1. Referee: [AGN template modelling paragraph] AGN template modelling paragraph (results section): The quantitative upper limit of Eddington ratios <1% for dust-enshrouded AGN in high-mass PSBs is derived from non-detections in the MIRI bands via template fitting. The manuscript must specify the AGN template library, the grid of obscuration parameters (e.g., N_H, covering factors, viewing angles), and the bolometric correction assumptions, because changes in these inputs can loosen or tighten the reported limit. This modelling step is load-bearing for the central claim of no hidden AGN.

    Authors: We agree that explicit documentation of the template-fitting procedure is essential to substantiate the Eddington-ratio upper limit. In the revised manuscript we will expand the relevant results paragraph (and add a short methods subsection if space permits) to name the specific AGN template library, tabulate or describe the grid of obscuration parameters (N_H range, covering factors, viewing angles), and state the bolometric corrections adopted. This will allow readers to evaluate how the <1% limit depends on these choices. revision: yes

  2. Referee: [Sample selection and completeness discussion] Sample selection and completeness discussion: The photometric criteria used to isolate the 65 PSBs must include quantitative tests for contamination by dusty star-forming galaxies or older passive systems, particularly to substantiate the reported differences between low- and high-mass bins. Without such validation, the mass-dependent IR properties cannot be unambiguously attributed to distinct quenching pathways.

    Authors: We accept that quantitative contamination tests would strengthen the interpretation. In the revised manuscript we will add a dedicated paragraph (or subsection) presenting contamination estimates, for example by comparing the PSB selection criteria against control samples of dusty star-forming and older passive galaxies, and by reporting the expected contamination fractions in each mass bin. These tests will support the claim that the observed mass-dependent mid-IR properties reflect distinct quenching pathways. revision: yes

Circularity Check

0 steps flagged

No significant circularity; Eddington limit derived from external templates applied to non-detections

full rationale

The central claim applies standard AGN template modelling to the observed MIRI photometry (non-detections at 7.7 and 18 μm) to place an upper limit on Eddington ratios for massive PSBs. This step uses external templates rather than any self-derived scaling or fitted parameter from the present dataset. No equations reduce the reported <1% bound to the input photometry by construction, and the abstract and provided text contain no load-bearing self-citations or uniqueness theorems. The photometric selection of PSBs is an independent upstream step whose validity is an empirical question, not a definitional loop. Minor self-citation risk is possible in the full methods but is not load-bearing for the quoted limit.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The claim rests on standard assumptions that mid-IR excess traces either AGN or star formation, and that AGN templates from the literature can be scaled to set upper limits. No new entities are introduced.

free parameters (1)
  • Eddington ratio upper limit
    Derived by scaling AGN templates until they exceed the observed photometry; the <1% value is the threshold that fits the non-detection.
axioms (1)
  • domain assumption Mid-infrared emission at 7.7 and 18 microns is produced only by hot dust heated by AGN or young stars
    Invoked when attributing the lack of excess to absence of both AGN and star formation.

pith-pipeline@v0.9.1-grok · 5877 in / 1258 out tokens · 23582 ms · 2026-06-26T16:28:34.983717+00:00 · methodology

discussion (0)

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Reference graph

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