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arxiv: 2605.00822 · v1 · submitted 2026-05-01 · 🌌 astro-ph.GA

Recognition: unknown

PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence

Gibson B. Bowling , Rafael Ortiz III , S. P. Willner , Seth H. Cohen , Timothy Carleton , Rogier A. Windhorst , Rolf A. Jansen , Christopher N. A. Willmer
show 24 more authors
W. Peter Maksym Anton M. Koekemoer Madeline A. Marshall Rosalia O'Brien Payaswini Saikia Massimo Ricotti Jordan C. J. D'Silva Dan Coe Christopher J. Conselice Jose M. Diego Simon P. Driver Brenda L. Frye Norman A. Grogin Rachel Honor Jake Summers Nor Pirzkal Aaron Robotham Russell E. Ryan Jr. Brent M. Smith Haojing Yan Cheng cheng Liam Nolan Heidi B. Hammel Stefanie N. Milam
Authors on Pith no claims yet

Pith reviewed 2026-05-09 18:27 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords AGN hostsstar formation main sequenceJWST NIRCamgalaxy evolutionpoint source subtractionquiescent galaxiesactive galactic nucleistar formation rates
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The pith

NIRCam-selected AGN hosts split into two populations where AGN activity, not stellar mass, controls their star formation rates.

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

The paper decomposes JWST/NIRCam and HST images of 36 AGN candidates in the North Ecliptic Pole field by modeling and subtracting central point sources. Residual host-galaxy light is then used to estimate star formation rates via SED fitting and offsets from the star-forming main sequence. This reveals two groups: a branch with SFRs above the main sequence that increase with AGN fraction, and a bridge with lower SFRs linking radio and X-ray sources. Both groups show recent transitions between star-forming and quiescent states, with no dependence on stellar mass or redshift.

Core claim

Point-source subtraction on NIRCam imaging separates AGN and host light for 36 candidates, showing host galaxies form a cleanly separated branch above Delta SFMS = -1 whose star formation rate trends positively with AGN fraction, and a bridge between moderate radio-source SFRs and low X-ray-source SFRs. Branch members are mostly late-type galaxies with strong point sources, while bridge members are early-type with weaker sources that may be stellar bulges. Both populations display signs of recent movement between star formation and quiescence without preference for higher or lower stellar mass or redshift.

What carries the argument

AGN-host decomposition by fitting and subtracting central point sources from NIRCam light profiles, followed by SED modeling of the residual host emission to compute Delta SFMS offsets that define the bridge and branch populations.

Load-bearing premise

The point-source subtraction cleanly isolates host-galaxy light without residual AGN contamination or morphological misclassification, and the apparent two-group structure is not produced by selection effects in the NIRCam sample or the radio/X-ray cross-matches.

What would settle it

A larger sample of similarly selected AGN hosts imaged at comparable resolution that shows no separation into branch and bridge groups on the Delta SFMS diagram, or instead shows a stronger trend with stellar mass than with AGN fraction.

Figures

Figures reproduced from arXiv: 2605.00822 by Aaron Robotham, Anton M. Koekemoer, Brenda L. Frye, Brent M. Smith, Cheng cheng, Christopher J. Conselice, Christopher N. A. Willmer, Dan Coe, Gibson B. Bowling, Haojing Yan, Heidi B. Hammel, Jake Summers, Jordan C. J. D'Silva, Jose M. Diego, Liam Nolan, Madeline A. Marshall, Massimo Ricotti, Norman A. Grogin, Nor Pirzkal, Payaswini Saikia, Rachel Honor, Rafael Ortiz III, Rogier A. Windhorst, Rolf A. Jansen, Rosalia O'Brien, Russell E. Ryan Jr., Seth H. Cohen, Simon P. Driver, S. P. Willner, Stefanie N. Milam, Timothy Carleton, W. Peter Maksym.

Figure 1
Figure 1. Figure 1: RGB image cutouts of the sample galaxies. Stamps are shown in order of increasing redshift and are ∼6 ′′ on a side. Each object’s redshift and O24 ID are shown in the lower and upper left corners of their stamps, respectively. Objects with X-ray counterparts have an X in the top right corner, objects with radio counterparts have an R, and ob￾jects with both have X+R. The image RGB colors use the Trilogya (… view at source ↗
Figure 2
Figure 2. Figure 2: Images of the modeling done for IDs 2 (left), 62 (middle), and 40 (right). Each set of 3 images corresponds to the indicated filter; the leftmost image is the galaxy image, the middle image is the best-fit model light profile found by GALFIT, and the right image is the residual. The goodness-of-fit statistic χ 2 ν of each is shown in the bottom right of the residual panel of each. All images are ∼ 4 ′′ on … view at source ↗
Figure 3
Figure 3. Figure 3: The UV–visible–NIR point source magnitude as a function of rest-frame wavelength for ID 27. Point-source magnitudes are drawn in gold with error bars from the pro￾cedure of §3.2, and the total magnitudes and error bars from O24 are drawn in blue. Their uncertainties are very small in the NIRCam filters, generally significant only for faint ob￾jects in HST filters. The fitting procedure outlined in §3.1 and… view at source ↗
Figure 4
Figure 4. Figure 4: Best-fit host-galaxy SEDs from CIGALE. The redshift, χ 2 of the SED fit, and logarithms of the SFR, stellar mass, and sSFR ≡ SFR/M⋆ shown in the upper left of each panel. Host-galaxy flux densities are plotted in red with uncertainties computed via Equation (5), and model SEDs are drawn in black. Nebular emission is drawn in green, stellar attenuated and unattenuated are drawn in orange and blue, respectiv… view at source ↗
Figure 5
Figure 5. Figure 5: Star-forming properties of the sample. This study’s NIRCam-selected objects are plotted as orange squares, and the X-ray- (R. Ortiz et al. 2026, in prep.) and radio-selected (S. P. Willner et al. 2026) objects are plotted as pink Xs and blue circles, respectively. NIRCam-selected objects with an X-ray counterpart (W. P. Maksym et al. in prep.) are plotted with a black ×; those with a radio counterpart (M. … view at source ↗
Figure 6
Figure 6. Figure 6: Offsets from the SFMS as a function of fAGN. For clarity, only the NIRCam-selected sample is shown. X-ray and radio detections are marked with × and +, respectively, and marker colors correspond to redshift as shown in the scale bar. The vertical dotted line is the fAGN ≥ 0.3 cut used in the sample selection, and the horizontal dashed line at ∆SFMS = −1 is used to separate the bridge portion of the sample … view at source ↗
Figure 7
Figure 7. Figure 7: JWST/F090W light-profile models for six galaxies. The left column shows branch galaxies and the right column bridge galaxies with IDs and redshifts labeled. For each galaxy, the left panel shows the observed image, the middle panel shows the model, and the right panel shows the residual. ties. One is that the bridge galaxies are not AGN but are instead galaxies with bright, compact central re￾gions that ap… view at source ↗
Figure 8
Figure 8. Figure 8: Normalized distributions of the NIRCam sample’s properties. The upper left panel shows SMFS offsets, the upper right stellar mass, the lower left O24 fAGN, and the lower right JWST/F444W point-source fraction. The latter is the F444W point-source magnitude mPS (§3.1) minus total magnitude mcat (O24). The bridge distributions are drawn in blue and the branch distributions in orange. The means (circles) and … view at source ↗
Figure 9
Figure 9. Figure 9: Renders of the PSF models given to GALFIT for spoke 1’s various position angles. The position angle indicators a, b, and ab are as in view at source ↗
read the original abstract

We present the results of AGN--host-galaxy decomposition using JWST/NIRCam, HST/ACS, and HST/WFC3 imaging of the North Ecliptic Pole Time Domain Field (NEP-TDF). The light-profiles of 36 NIRCam-selected AGN candidates are modeled for measurement of their point sources, and point source-subtracted host-galaxy emission is used in SED modeling for star formation rate (SFR) estimation. Offsets from the canonical star-forming main sequence (SFMS) show that the host galaxies form two distinct groups distinguished by their star formation: a ``bridge'' between the moderate SFRs of radio sources and low SFRs of X-ray sources, and a cleanly-separated ``branch'' above $\Delta \rm SFMS = -1$ whose SFR trends positively with AGN fraction. Branch galaxies include late-type galaxies with X-ray and radio detections and more dominant point sources that are most certainly AGN, while bridge galaxies have predominantly early-type morphologies with weaker point sources that may be due to compact stellar bulges. Both groups show evidence of recent transition between star formation and quiescence, but neither group shows preference for higher or lower stellar mass or redshift, suggesting that star formation in NIRCam-selected AGN-hosts is more strongly determined by AGN activity than by stellar mass.

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

3 major / 2 minor

Summary. The manuscript analyzes 36 NIRCam-selected AGN candidates in the NEP-TDF using JWST/NIRCam, HST/ACS, and HST/WFC3 imaging. It performs AGN-host decomposition to isolate point-source AGN light and subtract it for host-galaxy SED modeling and SFR estimation. Offsets from the star-forming main sequence (SFMS) reveal two populations: a 'bridge' linking moderate-SFR radio sources to low-SFR X-ray sources, and a 'branch' above ΔSFMS = -1 whose SFR increases with AGN fraction. Both groups show signs of recent transitions between star formation and quiescence, yet neither exhibits preference for stellar mass or redshift, leading to the claim that AGN activity determines star formation more strongly than stellar mass in these hosts.

Significance. If the decomposition is robust, the identification of two distinct AGN-host populations with different SF behaviors would provide observational support for AGN-driven modulation of star formation independent of mass, with implications for feedback models and quenching pathways. The JWST-enabled decomposition is a methodological strength that could improve separation of nuclear and host light compared to prior work.

major comments (3)
  1. [Decomposition procedure and SFR estimation] The central claim that AGN activity dominates over stellar mass rests on the post-subtraction host SFRs being unbiased. No validation of the point-source subtraction (residual maps, mock tests, or cross-checks against independent SFR indicators) is described, leaving open the possibility that incomplete subtraction systematically inflates SFRs in the branch population (which has more dominant point sources).
  2. [Results on SFMS offsets and group properties] Group membership is defined from observed ΔSFMS offsets and morphological classifications, yet with N=36 and no reported quantitative statistics, error budgets, or selection-bias tests, the bridge/branch separation and the positive SFR–AGN-fraction trend in the branch lack demonstrated robustness against small-number fluctuations or NIRCam/radio/X-ray cross-match biases.
  3. [Morphological and point-source analysis] Bridge galaxies are described as having weaker point sources that 'may be due to compact stellar bulges.' Without explicit quantitative criteria for AGN vs. bulge classification or supporting multi-wavelength confirmation, this introduces a classification uncertainty that directly affects the inferred distinction between groups and the conclusion that AGN activity, rather than mass, drives the SF differences.
minor comments (2)
  1. [Abstract] The abstract states that 'neither group shows preference for higher or lower stellar mass or redshift' but does not specify the statistical test or threshold used to reach this conclusion.
  2. [Figures] Ensure all figures displaying SFMS offsets, AGN fractions, and group trends include individual error bars, group sample sizes, and clear labels for bridge vs. branch.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for the constructive and detailed comments. We address each major comment point by point below, providing clarifications from the manuscript and indicating revisions where they will strengthen the presentation without misrepresenting the analysis performed.

read point-by-point responses

  1. Referee: [Decomposition procedure and SFR estimation] The central claim that AGN activity dominates over stellar mass rests on the post-subtraction host SFRs being unbiased. No validation of the point-source subtraction (residual maps, mock tests, or cross-checks against independent SFR indicators) is described, leaving open the possibility that incomplete subtraction systematically inflates SFRs in the branch population (which has more dominant point sources).

    Authors: The decomposition is described in Section 3, where PSF modeling is applied to isolate the point-source AGN component before host SED fitting with the remaining light. While the current text does not include residual maps or mock tests, the procedure follows established methods validated in prior JWST AGN studies. We will add representative residual maps and a short description of mock AGN+host simulations to quantify subtraction biases in the revised manuscript. Cross-checks with independent SFR indicators such as far-IR are not feasible with the available HST/JWST imaging dataset; we will explicitly note this limitation. revision: partial

  2. Referee: [Results on SFMS offsets and group properties] Group membership is defined from observed ΔSFMS offsets and morphological classifications, yet with N=36 and no reported quantitative statistics, error budgets, or selection-bias tests, the bridge/branch separation and the positive SFR–AGN-fraction trend in the branch lack demonstrated robustness against small-number fluctuations or NIRCam/radio/X-ray cross-match biases.

    Authors: The modest sample size of 36 is a limitation inherent to the NIRCam-selected candidates in the NEP-TDF. The bridge/branch separation appears as a clear gap around ΔSFMS = -1 in Figure 4, with the positive trend visible in the branch. In revision we will add propagated uncertainties on ΔSFMS, a Spearman-rank test for the SFR–AGN-fraction correlation, and a brief assessment of selection biases by comparing the AGN-host subsample to the parent NIRCam catalog. These additions will better quantify robustness against small-number effects. revision: yes

  3. Referee: [Morphological and point-source analysis] Bridge galaxies are described as having weaker point sources that 'may be due to compact stellar bulges.' Without explicit quantitative criteria for AGN vs. bulge classification or supporting multi-wavelength confirmation, this introduces a classification uncertainty that directly affects the inferred distinction between groups and the conclusion that AGN activity, rather than mass, drives the SF differences.

    Authors: Classification combines quantitative outputs from the light-profile decomposition (point-source flux fraction and Sersic index) with available X-ray and radio detections. The tentative phrasing for bridge galaxies reflects objects lacking strong multi-wavelength AGN signatures. We will revise the relevant section to state explicit criteria (e.g., point-source fraction > 0.3 for secure AGN) and include a supplementary table summarizing the morphological and multi-wavelength properties used for each object. revision: yes

standing simulated objections not resolved
  • Cross-checks against independent SFR indicators (e.g., far-IR luminosities) cannot be performed because the dataset is restricted to optical/near-IR imaging.

Circularity Check

0 steps flagged

No circularity: populations defined from direct observations, claim follows from data comparison

full rationale

The paper classifies 36 AGN-host galaxies into 'bridge' and 'branch' groups using observed offsets from the star-forming main sequence (ΔSFMS) and morphological classifications from NIRCam/HST imaging after point-source subtraction. The central inference—that AGN activity determines star formation more strongly than stellar mass—rests on the empirical finding of no mass or redshift preference between the groups. No equations, fitted parameters, or self-citations are invoked to define the groups or force the conclusion by construction. The derivation chain is observational and does not reduce any prediction to its own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The abstract contains no explicit free parameters, axioms, or invented entities; the analysis relies on standard observational techniques whose details are not provided.

pith-pipeline@v0.9.0 · 5698 in / 1151 out tokens · 26739 ms · 2026-05-09T18:27:00.041648+00:00 · methodology

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Reference graph

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