{"id":"4e1df7bf-44b2-4968-a7d6-50dd9e939ad1","arxiv_id":"2607.12028","paper_version":1,"verdict":"CONDITIONAL","confidence":"LOW","novelty_score":5.5,"correctness_risk":"medium","formal_verification":"none","parameter_count":3,"one_line_summary":"Observed CCSN rates match dust-corrected UV+IR star-formation histories for plausible progenitor masses, recover a peak near z~2, and imply a rising fraction of dust-obscured supernovae toward high redshift.","lead":"This paper links core-collapse supernova rates from JWST JADES to cosmic star-formation rates out to redshift 5. It tests how well supernovae track star formation under different assumptions about stellar mass ranges and the initial mass function, and estimates how many supernovae surveys miss due to dust.","discovery_kind":"extension","skeptic_critique":{"model":"grok-4.5","headline":"Abstract-only review cannot verify the efficiency constraint or the obscured-fraction inference that carry the central claim; the load-bearing step remains uncheckable without rate tables, selection functions, and efficiency formulas.","rationale":"The Reader correctly identified the weakest link: treating CCSN production efficiency as sufficiently well constrained by low-z/theoretical priors so that high-z residuals can be read as missing dust-obscured events. With only the abstract, that premise cannot be stress-tested further; no rate tables, efficiency formulas, or selection functions are present. The concern is therefore real but already captured by the Reader's CONDITIONAL / LOW-confidence verdict. No new load-bearing flaw is introduced by the abstract text itself, nor is the existing one resolved. Verdict remains CONDITIONAL pending full-text verification of the efficiency constraint and the obscured-fraction calculation. Agreement with the Reader is complete on the identity of the soft spot.","tokens_in":2144,"tokens_out":512,"duration_ms":5732,"concrete_test":"When the full paper appears, extract the adopted CCSN production efficiency (events per solar mass formed) and the progenitor mass range used in the main comparison; recompute the implied missing fraction at z~2 and z~4 under a 20% shift in that efficiency (or under a Salpeter vs. Chabrier IMF). If the missing-fraction curve changes by more than ~30% or loses its z~2 peak, the attribution of residual tension primarily to dust obscuration is not robust.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's central claim rests on using observed CCSN rates to constrain the production efficiency that converts SFRD into CCSN rate, then interpreting residual tension with higher (mm-source-inclusive) SFRDs as an increasing fraction of dust-obscured missing CCSNe. Because only the abstract is available, the actual efficiency values, the progenitor-mass and IMF assumptions that set them, the completeness corrections applied to the JADES rates, and the quantitative comparison that yields the rising missing fraction cannot be inspected. The abstract asserts consistency with UV+IR SFRDs for 'plausible' progenitor masses and a peak missing fraction near z~2, but without the supporting numbers or selection functions it is impossible to confirm that residual mismatches are dominated by dust rather than by evolving efficiency, IMF variation, or survey systematics. This is the same soft spot the Reader flagged; the abstract alone does not resolve it.","agreement_with_reader":"agree"},"referee_report":{"model":"grok-4.5","summary":"The manuscript investigates how core-collapse supernova (CCSN) rates trace cosmic star-formation rate densities (SFRDs) over 0 ≤ z ≤ 5, combining new high-redshift results from the JADES Transient Survey with published CCSN rates. Observed rates are used to constrain the CCSN production efficiency that relates SFRDs to CCSN rates, and the dependence of that connection on the IMF and the adopted progenitor mass range is examined. The abstract reports consistency with dust-corrected UV+IR SFRDs for plausible progenitor masses, a reconstructed star-formation history peaking near z ∼ 2, only modest impact from redshift-evolving IMF when SFRDs are treated consistently, and—when higher SFRDs that include faint millimeter sources are adopted—a substantial and increasing fraction of missing, dust-obscured CCSNe that peaks near z ∼ 2 and remains large toward z ∼ 5.","tokens_in":2392,"tokens_out":782,"duration_ms":17667,"significance":"If the quantitative results hold, the work would supply an independent, rate-based reconstruction of the cosmic star-formation history and a redshift-dependent estimate of the dust-obscured CCSN fraction, both of clear interest for supernova surveys and galaxy evolution. Explicit treatment of IMF evolution and progenitor mass range, together with the use of new JWST/JADES high-z rates, would be a useful contribution provided the efficiency constraints, completeness corrections, and residual-tension interpretation are robust and reproducible.","major_comments":[{"comment":"Abstract (central efficiency claim): The load-bearing step is that observed CCSN rates constrain the production efficiency and are consistent with dust-corrected UV+IR SFRDs for “plausible” progenitor masses. Without the efficiency formula, the adopted progenitor mass range, IMF assumptions, rate tables with uncertainties, and selection/completeness functions, this consistency cannot be verified. Residual mismatches could equally arise from evolving efficiency or survey systematics rather than being absorbed into the efficiency prior.","section":null},{"comment":"Abstract (missing-fraction inference): The claim of a substantial and increasing fraction of dust-obscured CCSNe relative to higher (mm-source-inclusive) SFRDs reuses the same production efficiency constrained from the rates. The abstract itself notes that the missed fraction “depends on the adopted CCSN production efficiency.” This introduces a circularity risk: residual tension is attributed primarily to dust obscuration rather than to efficiency evolution, IMF variation, or selection effects. A clean separation of the efficiency constraint from the residual-tension interpretation is required for the claim to hold.","section":null},{"comment":"Abstract (IMF-evolution result): The statement that allowing the IMF to evolve with redshift has “only a modest impact when SFRD estimates are treated consistently” is important for the paper’s interpretation of CCSN-rate sensitivity, but is uncheckable from the abstract alone. The specific IMF-evolution models, the consistent SFRD treatment, and the quantitative impact on efficiency and the missing fraction must be inspectable in the full analysis before this conclusion can be accepted.","section":null}],"minor_comments":[],"recommendation":"uncertain","confidential_remarks":"This is an abstract-only review; a definitive recommendation is not possible without the full manuscript (rate tables, selection functions, efficiency formulas, progenitor-mass and IMF assumptions, and the quantitative missing-fraction analysis). The main load-bearing issue to check once the full text is available is the circularity risk flagged above—using rates both to constrain efficiency and to interpret residual tension as dust-obscured missing events. Scope appears appropriate for an astrophysics journal covering high-z transients and cosmic star formation, but the full paper is required before accept/revise/reject can be decided."},"author_rebuttal":null,"desk_editor":{"model":"grok-4.5","letter":"The one thing to know is that this is a solid observational synthesis paper, not a conceptual leap: new JADES Transient Survey high-z CCSN rates plus literature rates, used to test consistency with UV+IR SFRDs and to estimate a rising dust-obscured missing fraction out to z~5. That is worth having; it is not a new framework.\n\nWhat they do well is the empirical framing. They constrain production efficiency from the rates themselves, check that the rates recover a star-formation history peaking near z~2, and show that modest IMF evolution does not wreck the comparison when SFRDs are treated consistently. The abstract’s claim of consistency with dust-corrected UV+IR SFRDs for plausible progenitor masses is the right kind of result for this series, and the multi-author JADES context gives the rates some weight.\n\nThe soft spot is real and load-bearing, and the stress-test is right about it. They use the rates both to set efficiency and then to interpret residual tension with higher (mm-source-inclusive) SFRDs as missing obscured events. Without the rate tables, selection functions, completeness corrections, and the actual efficiency numbers, you cannot tell whether residual mismatches are dominated by dust rather than by evolving efficiency, IMF choices, or survey systematics. The abstract says the missing fraction depends on the adopted efficiency and still rises toward z~2 and stays high to z~5; that is honest, but it also means the central quantitative claim is not yet inspectable. Circularity risk is moderate, not fatal, and free parameters (efficiency, mass range, IMF) are the usual ones for this problem.\n\nThis is for people who work on high-z transients, cosmic SFRD, or dust-obscured star formation. A serious referee should see the full paper; the abstract alone is not enough to accept or reject the numbers. I would not cite it yet from the abstract, but I would send it to peer review. Bring it to reading group only if someone is already deep in JADES or CCSN rate work; otherwise wait for the figures.","headline":"Useful JADES-era synthesis of high-z CCSN rates vs SFRD, but the efficiency-to-obscured-fraction step is uncheckable from the abstract alone.","tokens_in":3105,"tokens_out":529,"would_cite":false,"duration_ms":5806,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"grok-4.5","headline":"Observed core-collapse supernova rates match dust-corrected star-formation densities and recover a cosmic peak near redshift 2.","keywords":["core-collapse supernovae","star-formation rate density","cosmic star-formation history","dust obscuration","initial mass function","JWST","JADES Transient Survey","high-redshift supernovae"],"falsifier":"A complete, dust-unbiased census of core-collapse supernovae at z~2 that either recovers the full rate predicted by the higher millimeter-based SFRDs or continues to fall short by the same large factor reported here.","tokens_in":3060,"feed_emoji":"⭐","tokens_out":664,"duration_ms":4870,"temperature":0.7,"pith_summary":"This paper asks whether core-collapse supernova rates can serve as a reliable tracer of cosmic star formation from the present day out to redshift 5. Combining new high-redshift rates from the JWST JADES Transient Survey with published lower-redshift samples, the authors treat the observed supernova rates as a constraint on the conversion efficiency that turns star-formation rate density into supernova rate. They show that, for plausible progenitor mass ranges and a standard initial mass function, the measured rates sit comfortably on the dust-extinction-corrected ultraviolet-plus-infrared star-formation history. Reconstructing the star-formation history directly from the supernova rates recovers the well-known peak near redshift 2. When higher star-formation densities that include faint millimeter sources are adopted instead, a growing fraction of dust-obscured supernovae is required to reconcile the two, rising from modest values at low redshift to a substantial fraction near the peak of cosmic star formation and remaining large out to redshift 5. Allowing the initial mass function to evolve with redshift produces only modest changes once the star-formation densities are treated consistently, suggesting that supernova rates are less sensitive to IMF variations than is often assumed.","feed_headline":"Supernova rates recover the cosmic star-formation peak at z~2","feed_subtitle":"JWST rates match dust-corrected UV+IR histories; higher mm-based SFRDs imply many missing obscured events","key_machinery":"The CCSN production efficiency that converts star-formation rate density into core-collapse supernova rate, set by the adopted initial mass function and the progenitor mass range that explode as CCSNe; this efficiency is constrained by the observed rates and then used either to test consistency with independent SFRDs or to reconstruct the star-formation history itself.","core_discovery":"Observed core-collapse supernova rates are consistent with dust-extinction-corrected UV+IR star-formation rate densities for plausible progenitor masses; using those rates to reconstruct the cosmic star-formation history recovers a peak at z~2, while higher SFRDs that include faint millimeter sources imply a substantial and increasing fraction of missing, dust-obscured supernovae toward higher redshifts.","pith_inferences":[],"forward_implications":[],"fun_headline_variants":["CCSN rates recover star-formation peak at z~2 from JWST data","Observed supernova rates match dust-corrected UV+IR SFRDs","Reconstructing cosmic SFH with CCSNe shows peak at z~2","Higher mm SFRDs imply rising fraction of missing obscured SNe","CCSN production efficiency ties rates to star formation to z=5"],"cache_read_input_tokens":128,"weakest_assumption_plain":"The conversion efficiency from star formation into core-collapse supernovae can be fixed by low-redshift or theoretical priors so that residual mismatches at high redshift are attributed mainly to dust obscuration rather than to evolving efficiency or survey selection effects.","fun_headline_variants_meta":{"raw":{"variants":["CCSN rates recover star-formation peak at z~2 from JWST data","Observed supernova rates match dust-corrected UV+IR SFRDs","Reconstructing cosmic SFH with CCSNe shows peak at z~2","Higher mm SFRDs imply rising fraction of missing obscured SNe","CCSN production efficiency ties rates to star formation to z=5"]},"model":"grok-4.5","effort":"low","cost_usd":0.00518,"raw_usage":{"total_tokens":1524,"prompt_tokens":895,"num_sources_used":0,"completion_tokens":99,"cost_in_usd_ticks":51800000,"prompt_tokens_details":{"text_tokens":895,"audio_tokens":0,"image_tokens":0,"cached_tokens":256},"completion_tokens_details":{"audio_tokens":0,"reasoning_tokens":530,"accepted_prediction_tokens":0,"rejected_prediction_tokens":0}},"tokens_in":895,"tokens_out":99,"duration_ms":4041,"temperature":1.0,"reasoning_tokens":530,"cache_read_input_tokens":256,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-07-15T08:20:53.263329+00:00","model_set":{"reader":"grok-4.5"},"falsifier":"A complete, dust-unbiased census of core-collapse supernovae at z~2 that either recovers the full rate predicted by the higher millimeter-based SFRDs or continues to fall short by the same large factor reported here.","supporting_citations":[],"review_version":1}