{"id":"964aea53-18f7-4927-9249-1499dcd02319","arxiv_id":"2607.02666","paper_version":1,"verdict":"ACCEPT","confidence":"HIGH","novelty_score":6.5,"correctness_risk":"medium","formal_verification":"none","parameter_count":4,"one_line_summary":"MEOW MIRI survey identifies 16 high-z obscured AGN whose bolometric luminosity function at z=4.5-6 is comparable to broad-line AGN and LRDs, establishing MIRI as essential for a complete early SMBH census.","lead":"JWST/MIRI imaging of GOODS fields finds 16 dust-obscured AGN at z=4.5-7.2, most newly identified and including narrow-line systems missed by broad-line searches. Their luminosity function matches broad-line AGN and little red dots, showing obscured growth is a major channel for early supermassive black holes.","discovery_kind":"new_application","skeptic_critique":{"model":"grok-4.5","headline":"No significant objection identified beyond the reader's already-flagged f_AGN threshold; the LF comparison remains supported under stated assumptions.","rationale":"The paper is a transparent observational survey whose strongest claim is a number-density comparison, not a new physical mechanism. The reader correctly isolates the model-dependent f_AGN cut as the softest link. My re-examination finds that link is real but already quantified: the authors show color-color separation, report both pure-AGN and composite samples, and the LF remains comparable even when composites are included. No hidden circularity, no unaccounted incompleteness that would systematically inflate ϕ by the factor needed to erase the comparison, and no contradiction with the spectroscopic narrow-line subset. Therefore the ACCEPT verdict stands; the concrete test above is a useful robustness check rather than a required fix. Confidence remains high for an observational result of this type.","tokens_in":31145,"tokens_out":557,"duration_ms":6183,"concrete_test":"Re-run the full CIGALE grid allowing free θ_AGN (type-1 + type-2) and recompute f_AGN and L_bol for the 16 objects; if more than ~3 sources drop below f_AGN=0.1 or the z=4.5–6 ϕ points in Table 4 shift by >0.3 dex outside the quoted uncertainties, the comparability claim weakens. Otherwise the result is robust to the fixed-inclination choice.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The reader's weakest assumption (CIGALE f_AGN thresholds with fixed type-2 skirtor viewing angle) is correctly identified as the main model dependence. After re-reading §4.2.1–5.5, Table 2–4 and Fig. 5/9, I find no stronger internal inconsistency. Color-color tracks (Fig. 5) and the five spectroscopically confirmed narrow-line objects provide independent support that the MIRI excess is real and not pure SF. Completeness is constructed from stacked empirical templates split by f_AGN bin and folded into V_eff (Eq. 1–2, Fig. 4); the resulting ϕ values sit within the scatter of independent BL/LRD LFs. Small-N Poisson + L_bol resampling is already handled by the MCMC. Field-to-field checks (Appendix B) show no large discrepancy. Thus the central claim—that MIRI-selected number densities are comparable—holds under the paper's stated SED assumptions; residual risk is the usual observational model dependence already noted by the reader, not a new load-bearing flaw.","agreement_with_reader":"agree"},"referee_report":{"model":"grok-4.5","summary":"The paper presents MEOW, a JWST/MIRI F1000W+F2100W imaging survey of 95 arcmin² in GOODS-N/S, and uses CIGALE SED fits (with HST, NIRCam, SCUBA-2) to identify 16 MIRI-selected AGN at z=4.5–7.2 (12 with spectroscopic redshifts), of which 12 are new and at least five are narrow-line. Completeness is estimated from source-injection tests and empirical stacked templates split by f_AGN; an MCMC bolometric luminosity function at z=4.5–6 (Table 4, Fig. 9) is reported to be comparable in number density to JWST broad-line AGN and LRD samples, supporting a substantial obscured contribution to early SMBH growth.","tokens_in":31440,"tokens_out":1083,"duration_ms":10643,"significance":"If the number densities hold under the stated SED assumptions, the work supplies a concrete mid-IR census of obscured (including Type II) AGN at z≳5 that is largely complementary to broad-line searches, with five spectroscopically confirmed narrow-line systems and a carefully constructed V_eff (Eqs. 1–2, Fig. 4). The survey design, dual-filter depths, spectroscopic confirmation rate, and MCMC LF with L_bol resampling are strengths that make the result a useful benchmark for multi-wavelength AGN censuses. Residual model dependence (fixed type-2 skirtor inclination, f_AGN thresholds) is typical of IR SED work and is already partially tested by color-color tracks (Fig. 5) and the narrow-line subsample.","major_comments":[{"comment":"§4.2.1 and Table 2: the skirtor viewing angle is fixed to type-2 only (θ_AGN=70°) and pure-AGN vs composite classification rests on Bayesian f_AGN cuts (≥0.5 / 0.1–0.5). Because L_bol and the LF (Table 4, Fig. 9) inherit these choices, a short sensitivity test (e.g., free inclination or alternate torus library, and LF recomputed for pure-AGN only vs f_AGN>0.1) is needed to show that the claimed comparability to BL/LRD densities is not driven by the fixed type-2 prior or the threshold placement.","section":null},{"comment":"§5.5 / Fig. 9: the LF comparison to BL AGN and LRDs is central, yet bolometric corrections for BL samples and empirical LRD luminosities differ in method from the CIGALE accretion-power L_bol used here. The text should quantify (or bound) how much of the apparent agreement could arise from inconsistent L_bol definitions, especially given the paper’s own note that LRD luminosities may be overestimated by canonical corrections.","section":null}],"minor_comments":[{"comment":"§6.1: the non-overlap with the 15 SMILES z>4.5 candidates of Lyu et al. (2024) is useful; a one-sentence statement of how many of those sources fall below the MEOW F2100W completeness would help readers assess filter-set vs depth differences.","section":null},{"comment":"Fig. 3 caption and §4.1.2: the text states 12 spectroscopic redshifts; ensure the figure legend and the count of objects inside the FRESCO Hα/[OIII] windows are fully consistent.","section":null},{"comment":"Appendix B / Fig. 13: field-to-field LF panels are helpful; note explicitly whether the mild GOODS-N excess at L_bol≳10^46 is consistent with the known z≈5.2 overdensity cited in the text.","section":null},{"comment":"Table 3: alternative IDs are valuable; a compact flag column for BL / NL / LRD status would make the sample easier to cross-match with Matthee, Zhang, and Greene et al.","section":null},{"comment":"Minor typography: abstract and §1 use both z≳5 and z>6; keep a single convention. Check “phot-z” vs “photo-z” consistency in Fig. 3.","section":null}],"recommendation":"minor_revision","confidential_remarks":"The central claim is observationally well supported under the paper’s stated assumptions; the two major points are standard model-dependence and L_bol-systematics checks that can be addressed without new data. Fit for ApJ is clear. No novelty or citation-pattern concerns."},"author_rebuttal":null,"desk_editor":{"model":"grok-4.5","letter":"This is the first wide dual-filter MIRI census that actually delivers a statistical sample of z≳5 obscured AGN and a bolometric luminosity function. The headline numbers are real: 16 sources (12 new), five spectroscopically confirmed narrow-line systems that BL searches miss, and ϕ values at z=4.5–6 that sit next to the Matthee/Lin/Zhang BL and Greene LRD LFs rather than the pre-JWST Shen curve.\n\nWhat they did well is straightforward. Survey design is clean (95 arcmin^{2} over FRESCO, F1000W+F2100W depths 0.5/3.6 µJy). Completeness is measured by injection, then folded into V_eff with empirical stacked templates split by f_AGN bin. Twelve of sixteen have spectroscopic redshifts. The MCMC LF resamples L_bol uncertainties and handles Poisson properly. Color-color tracks and the five NL objects give independent evidence that the MIRI excess is not pure star formation. Field-to-field checks in the appendix show nothing alarming. The discussion of circumnuclear versus host-scale obscuration is measured and useful.\n\nThe soft spot is exactly the one the reader flagged: pure-AGN versus composite classification rides on Bayesian f_AGN thresholds from CIGALE skirtor models with viewing angle fixed to type-2. That is standard practice, but it is load-bearing. If the templates systematically mis-attribute hot-dust luminosity, both sample purity and the LF shift. Only two MIRI filters (versus eight in SMILES) also limits SED leverage, and energy balance is assumed. None of this invents a contradiction; the central claim still holds under the stated assumptions, and the authors are transparent about the model dependence.\n\nThis paper is for anyone working on early SMBH growth, obscured fractions, or multi-wavelength AGN selection. It is not a methods revolution, but it is the observational step that was missing. I would bring it to reading group, cite the sample and LF, and send it to peer review without hesitation.","headline":"Solid new MIRI sample of high-z obscured AGN with a usable bolometric LF; model-dependent f_AGN cuts are the main caveat but do not sink the result.","tokens_in":32211,"tokens_out":514,"would_cite":true,"duration_ms":6533,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"grok-4.5","headline":"JWST/MIRI imaging uncovers a population of dust-obscured AGN at z≳5 whose number densities match those of broad-line AGN, showing that hidden growth is a major channel for early black holes.","keywords":["active galactic nuclei","high-redshift galaxies","supermassive black holes","JWST/MIRI","obscured AGN","bolometric luminosity function","little red dots"],"falsifier":"A deeper multi-band MIRI campaign that recovers the same sources with full 5–25 micron coverage and re-fits them with free inclination and alternative dust models, checking whether the high-f_AGN objects remain classified as AGN and whether the luminosity function stays comparable to the broad-line samples.","tokens_in":32074,"feed_emoji":"🌌","tokens_out":1029,"duration_ms":9601,"temperature":0.7,"pith_summary":"Early supermassive black holes must grow rapidly, yet short observed quasar lifetimes and high dust columns suggest most of that growth is hidden. This paper presents MEOW, a wide JWST/MIRI imaging survey of the GOODS fields in the 10 and 21 micron filters, designed to catch the hot dust that surrounds accreting black holes even when optical and X-ray light is blocked. Combining the new mid-infrared photometry with existing HST, NIRCam and submillimeter data, the authors isolate 16 AGN at redshifts 4.5–7.2, twelve of them previously unknown and at least five of them narrow-line (Type II) systems invisible to broad-line spectroscopy. Their bolometric luminosity function at z=4.5–6 has number densities comparable to those of broad-line AGN and little red dots, implying that the obscured population is not a small minority but a major part of the early AGN census. The hosts show a range of dust content, pointing to both circumnuclear and galaxy-scale obscuration. The result establishes mid-infrared imaging as essential, alongside spectroscopy, for a complete accounting of how the first black holes assembled their mass.","feed_headline":"Hidden black holes match visible ones at cosmic dawn","feed_subtitle":"MIRI finds dust-obscured AGN at z>5 whose numbers equal broad-line systems, rewriting the early census","key_machinery":"The Bayesian AGN fraction f_AGN measured from CIGALE SED fits that include the skirtor2016 clumpy torus; sources with f_AGN≥0.5 are classified as pure AGN and 0.1≤f_AGN<0.5 as composites, and this fraction, together with the MIRI F1000W/F2100W photometry that samples rest-frame hot-dust emission, selects the sample and supplies the bolometric luminosities used for the luminosity function.","core_discovery":"A sample of 16 MIRI-selected AGN at z=4.5–7.2 (12 spectroscopically confirmed) yields a bolometric luminosity function at z=4.5–6 whose number densities are comparable to those of broad-line AGN and little red dots, demonstrating that dust-obscured systems contribute significantly to the total AGN population and therefore to early supermassive black hole growth.","pith_inferences":["If the MIRI and broad-line populations remain largely distinct at fainter luminosities, the total black-hole accretion density at z~5 may be roughly double previous spectroscopic estimates.","The diversity of host E(B–V) among the narrow-line sources suggests that galaxy-scale dust fractions evolve with redshift and should be measurable with ALMA continuum maps of the same objects.","A joint MIRI-plus-NIRCam grism survey strategy could eliminate both the pre-selection bias of slit spectroscopy and the LRD incompleteness of pure MIRI selection."],"forward_implications":["Obscured accretion must be included in any complete census of z≳5 black-hole growth; broad-line samples alone undercount the population.","Multiple obscuration channels (circumnuclear torus and host-galaxy dust) operate at these redshifts, so unified torus models alone cannot explain the full Type II population.","MIRI imaging can separate little red dots that are weak in the mid-infrared from typical dust-obscured AGN that are bright at 10–21 microns.","Future deeper MIRI surveys will be required to test whether the same number-density match continues into the lower-luminosity regime where most little red dots reside."],"fun_headline_variants":["MIRI finds dust-hidden AGN matching broad-line counts at z>5","Obscured AGN rival broad-line systems in early-universe density","JWST/MIRI sample shows hidden AGN equal little red dots at cosmic dawn","16 MIRI AGN at z=4.5-7.2 prove obscured growth rivals visible SMBHs","Dust-obscured AGN contribute as much as broad-line ones by z~5"],"cache_read_input_tokens":16512,"weakest_assumption_plain":"The division into pure AGN, composites and star-forming galaxies rests on thresholds in the model-derived AGN fraction f_AGN; if the torus templates or the fixed type-2 viewing angle systematically mis-assign the hot-dust luminosity, both the sample membership and the luminosity function change.","fun_headline_variants_meta":{"raw":{"variants":["MIRI finds dust-hidden AGN matching broad-line counts at z>5","Obscured AGN rival broad-line systems in early-universe density","JWST/MIRI sample shows hidden AGN equal little red dots at cosmic dawn","16 MIRI AGN at z=4.5-7.2 prove obscured growth rivals visible SMBHs","Dust-obscured AGN contribute as much as broad-line ones by z~5"]},"model":"grok-4.5","effort":"low","cost_usd":0.004714,"raw_usage":{"total_tokens":1447,"prompt_tokens":992,"num_sources_used":0,"completion_tokens":112,"cost_in_usd_ticks":47140000,"prompt_tokens_details":{"text_tokens":992,"audio_tokens":0,"image_tokens":0,"cached_tokens":0},"completion_tokens_details":{"audio_tokens":0,"reasoning_tokens":343,"accepted_prediction_tokens":0,"rejected_prediction_tokens":0}},"tokens_in":992,"tokens_out":112,"duration_ms":3477,"temperature":1.0,"reasoning_tokens":343,"cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-07-12T07:51:03.930565+00:00","model_set":{"reader":"grok-4.5"},"falsifier":"A deeper multi-band MIRI campaign that recovers the same sources with full 5–25 micron coverage and re-fits them with free inclination and alternative dust models, checking whether the high-f_AGN objects remain classified as AGN and whether the luminosity function stays comparable to the broad-line samples.","supporting_citations":[],"review_version":1}