REVIEW 3 major objections 1 cited by
Observed core-collapse supernova rates match dust-corrected star-formation densities and recover a cosmic peak near redshift 2.
Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →
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.
T0 review reviewed 2026-07-15 challenge →
load-bearing objection Useful JADES-era synthesis of high-z CCSN rates vs SFRD, but the efficiency-to-obscured-fraction step is uncheckable from the abstract alone. the 3 major comments →
The JADES Transient Survey III: Linking Core-Collapse Supernova Rates to Cosmic Star Formation
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
Core claim
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.
What carries the argument
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.
Load-bearing premise
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.
What would settle it
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.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
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.
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 (3)
- 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.
- 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.
- 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.
Circularity Check
Abstract-only review finds no demonstrable by-construction circularity; results are framed as external SFRD comparisons.
full rationale
Only the abstract is available; no equations, rate tables, efficiency formulas, selection functions, or full derivation chain can be inspected. The abstract states that observed CCSN rates are used to constrain production efficiency relative to independent dust-corrected UV+IR SFRDs for plausible progenitor masses/IMF choices, that reconstructing the SFH from those rates recovers a peak at z~2 in agreement with galaxy luminosity-based determinations, and that higher mm-source-inclusive SFRDs imply a rising missing (dust-obscured) CCSN fraction. These are presented as consistency checks and residual comparisons against external benchmarks, not as self-definitional identities. Without the paper's equations it is impossible to exhibit a specific reduction of the form 'Eq. X equals Eq. Y by construction' or 'fitted parameter renamed as prediction.' Per the analysis rules requiring quoted, specific reductions rather than speculation about possible fitting procedures, no circular step is established. Score 0 is the warranted honest non-finding for an abstract-only review of a paper that claims external grounding.
Axiom & Free-Parameter Ledger
free parameters (3)
- CCSN production efficiency
- CCSN progenitor mass range
- IMF shape / redshift evolution
axioms (3)
- domain assumption CCSN rates are proportional to the massive-star formation rate via a production efficiency set by the IMF and progenitor mass range.
- domain assumption Dust extinction-corrected UV+IR SFRDs are a reliable baseline tracer of cosmic star formation against which CCSN rates can be compared.
- ad hoc to paper Higher SFRDs that include faint millimeter sources imply missing dust-obscured CCSNe rather than a failure of the rate measurements or efficiency model.
Cite this review
Pith. "Pith review of The JADES Transient Survey III: Linking Core-Collapse Supernova Rates to Cosmic Star Formation." pith.science (2026). https://pith.science/paper/EVNDRDD5
@misc{pith2026260712028,
author = {Pith},
title = {Pith review of: The JADES Transient Survey III: Linking Core-Collapse Supernova Rates to Cosmic Star Formation},
year = {2026},
howpublished = {\url{https://pith.science/paper/EVNDRDD5}},
note = {Machine review of arXiv:2607.12028}
}
abstract
We investigate how core-collapse supernova (CCSN) rates trace the star-formation rate densities (SFRDs) over the redshift range $0 \le z \le 5$. For this we use new high-redshift results from the James Webb Space Telescope Advanced Deep Extragalactic Survey (JADES) Transient Survey (JTS, see the companion paper by DeCoursey et al. 2026), together with published CCSN rates. Using the observed CCSN rates to constrain the CCSN production efficiency relating SFRDs to CCSN rates, we examine how the inferred connection between star formation rates and CCSN production efficiency depends on the stellar initial mass function (IMF) and the adopted CCSN progenitor mass range. We find that the observed CCSN rates are consistent with dust extinction-corrected UV+IR based SFRDs for plausible CCSN progenitor masses. Using the observed CCSN rates to directly reconstruct the cosmic star-formation history, we recover a peak at z $\sim2$, in agreement with galaxy luminosity-based determinations. Allowing the IMF to evolve with redshift has only a modest impact when SFRD estimates are treated consistently, indicating that CCSN rates are not as sensitive to the change of IMF as might be assumed. Adopting higher SFRDs that include a dust-obscured population of faint millimeter sources implies a substantial and increasing fraction of missing, dust-obscured CCSNe at higher redshifts. Although the inferred fraction of CCSNe missed by the surveys depends on the adopted CCSN production efficiency, we find an increasing fraction of supernovae missed due to obscuration, rising from modest values at low redshift to a peak at z $\sim2$, and remaining substantial toward z $\sim5$.
Forward citations
Cited by 1 Pith paper
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A Type Ia Supernova Candidate at $z\sim4.3$: A Transient Interloper in the Search for $z\sim14$ Galaxies
A JWST candidate z~14 galaxy is reclassified as a Type Ia supernova at z~4.3, implying SN Ia minimum delay times shorter than 1 Gyr.
This paper was first reviewed by grok-4.5 on July 15, 2026.
discussion (0)
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