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Metallicity differences between Type IIP and stripped-envelope supernova environments

T0 review · 3 major / 5 minor · reviewed 2026-08-04 · deepseek-v4-flash

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Pith's one-line read This paper claims that stripped-envelope (Type Ib/Ic) supernovae are born in systematically more metal-rich environments than Type IIP supernovae, a separation its statistical tests place above 99% confidence.

desk verdict Calibration scatter undercuts the headline p-values, but the enlarged sample and careful checks make this a valuable paper that deserves refereeing. read the letter →

arxiv 2509.06526 v1 pith:QPQPBEF5 submitted 2025-09-08 astro-ph.GA

R. Ganss , J. L. Pledger , A. E. Sansom , P. A. James , J. Puls , S. M. Habergham-Mawson This is my paper · ORCID
classification astro-ph.GA
keywords core-collapsesupernovaeTypeIIPstripped-envelope(Ib/Ic)HII-regionmetallicityN2/O3N2strong-lineindicatorsgas-phaseoxygenabundancesupernovaprogenitorscumulativedistributionfunctions
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to settle a long-standing question: do the different classes of core-collapse supernova—hydrogen-retaining Type IIP and hydrogen-stripped Type Ib and Ic—arise from the same kinds of stars? The authors' answer, from the largest spectroscopic sample of supernova explosion sites assembled to date (238 environments with the N2 indicator, 205 with O3N2), is that they do not. Stripped-envelope supernovae sit in more metal-rich neighborhoods than Type IIP by 0.05–0.07 dex, and two-sample statistical tests reject the idea that both types are drawn from one parent population with better than 1% confidence—and better than 0.1% confidence when all stripped-envelope events are combined. If correct, the claim matters because it ties a supernova's observed type to the chemical environment of its birthplace, giving stellar-wind and binary models a sharp new constraint. The paper finds no significant environmental difference between Type Ib and Type Ic themselves.

What carries the argument

The argument runs on two cumulative distribution functions (CDFs) of gas-phase oxygen abundance—one built from the N2 line ratio and one from O3N2, both calibrated with the Marino et al. (2013) strong-line relations (M13-N2 and M13-O3N2)—and on two permutation-based two-sample tests, the Kolmogorov-Smirnov and Anderson-Darling tests, applied to those CDFs. The CDFs localize where the subtypes differ: below 12+log(O/H) ≈ 8.5, where Type IIP has a longer tail toward low metallicity. The tests convert the visual separation into p-values for the null hypothesis that the subtype samples share a parent population, which is the paper's central statistical object.

What would settle it

Re-run the two-sample KS and AD tests with the full ±0.16/±0.18 dex calibration dispersion added as independent per-object errors rather than the ±0.04 dex observational noise used in the paper's Monte Carlo—if the resulting p-values rise above 0.01, the claimed separation is not established. Independently, direct (Te-based, auroral-line) oxygen abundances on a subset of the same 238 sites, or a targeted search for Type Ib events in hosts with 12+log(O/H) below 8.2, would settle whether the offset is physical.

Watch

Extended reading notes

Core claim

On the paper's own terms, the core discovery is that the oxygen abundance of the local HII region at a supernova site depends on the supernova's type. Type Ib and Ic environments have higher mean metallicities than Type IIP sites—by about 0.05 dex with the N2 indicator and 0.07 dex with O3N2—and their cumulative distributions part ways below 12+log(O/H) ≈ 8.5, where Type IIP shows a larger low-metallicity tail. Permutation-based Kolmogorov-Smirnov and Anderson-Darling tests reject the null hypothesis that the Ib/Ic and IIP samples share a parent population at better than 1% significance (better than 0.1% for the combined Ib+Ic sample versus IIP), while Ib versus Ic is consistent with a commo

Load-bearing premise

The load-bearing premise is that the calibration's per-object scatter (about ±0.16 dex for N2, ±0.18 dex for O3N2) is small or partially shared between supernova subtypes, so the measured 0.05–0.07 dex separation between Ib/Ic and IIP environments is signal, not noise; with that scatter treated as independent per object, the paper's own t-test gives p=0.053 and the claimed better-than-1% significance does not hold.

Editorial extensions

If this is right

  • Stellar evolution models must reproduce a metallicity preference: stripped-envelope SNe form in more metal-rich gas, pointing to metallicity-dependent mass loss (stronger winds at higher metallicity) as a driver of hydrogen-envelope stripping.
  • The physics distinguishing Type Ib from Type Ic is not visible in environment metallicity: the two samples are statistically indistinguishable, so helium stripping needs other diagnostics.
  • Clean subtype classification is load-bearing: including ambiguous Type II SNe in the IIP sample weakens the separation, so future surveys must keep Type IIP distinct from IIL, IIn, and IIb.
  • Supplementary CDFs place Type IIb and IIn environments between IIP and Ib/Ic, suggesting a continuous progression of stripping with metallicity that a larger IIb/IIn sample could confirm.
  • Binary-only explanations of subtype diversity face a new test: a purely orbital-period-driven picture must explain why Ib/Ic events preferentially occur in metal-rich environments, which is more naturally explained by single-star wind stripping.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A testable extension follows directly: wide-field transient surveys in dwarf and low-mass galaxies should find the Ib/Ic-to-IIP ratio dropping with host mass if metal-rich birth sites are genuinely required to produce observable stripped-envelope events.
  • The calibration caveat cuts both ways: if the ±0.16–0.18 dex scatter is largely common-mode (an overall scale shift), the relative subtype offset stands; if it is independent per object, the significance collapses. Te-based direct metallicities on a subset of the same 238 sites would discriminate the two regimes.
  • The paper's appendix data imply the classical 'Ic-BL are metal-poor' association does not extend to normal Type Ic: the seven Ic-BL in the archives all fall at 8.3–8.6 dex, between the IIP and Ic distributions, so subtype mixing of this kind is not what drives the Ib/Ic–IIP offset.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper presents the largest spectroscopic sample to date of local HII-environment metallicities for Type IIP, Type Ib, and Type Ic supernovae (238 targets with N2, 205 with O3N2), combining new INT/IDS observations with archival MUSE, MaNGA, and PISCO data. Metallicities are derived with the Marino et al. (2013) N2 and O3N2 calibrations. The central claim is that the cumulative metallicity distributions of Type Ib and Ic environments differ from those of Type IIP, with two-sample Kolmogorov-Smirnov and Anderson-Darling permutation tests giving p<0.01 for Ib-IIP and Ic-IIP and p<0.001 for the combined Ib+Ic versus IIP comparison. The authors interpret this as evidence for a different physical nature or formation channel of stripped-envelope versus Type IIP progenitors.

Significance. If the claimed statistical significance is robust, this is a valuable observational result: it is based on a much larger and more carefully classified sample than previous work, uses two independent emission-line fitting tools, checks long-slit versus IFU consistency, and examines host-galaxy biases. The paper also makes pragmatic choices such as restricting to clean Type IIP classifications and excluding Ic-BL events. The main result is plausible and would challenge stellar evolution models. However, the central claim rests entirely on the permutation-test p-values, and those p-values are computed on point estimates that do not include the dominant M13 calibration scatter. The paper's own t-test with calibration uncertainty gives p=0.053 for the Ib-IIP O3N2 mean difference, so the headline significance is not yet established.

major comments (3)
  1. [§4.3, §4.6, Table 4, §5.6] The headline p-values are computed on the M13 point estimates without propagating the calibration dispersion quoted in §4.3 (±0.16 dex for N2, ±0.18 dex for O3N2). The Monte Carlo in §5.6 adds only ±0.04 dex observational noise, which is far smaller than the calibration scatter. The paper itself shows in §4.4 that applying ±0.18 dex to all O3N2 values turns the Ib-IIP mean-difference t-test into p=0.053. Because the KS/AD tests are the load-bearing evidence for the abstract and §6 conclusions, the authors must repeat the permutation tests with per-object Gaussian scatter of 0.16/0.18 dex and report the resulting p-value distributions. If the significance does not survive, the central claim is not supported.
  2. [§4.2, §4.1, Table A.2, Figure 3] SN1961V is the only target that lies outside the HII region in the BPT diagram (Figure 3), yet it is retained in the IIP sample (Table A.2), while SN2012cw is excluded in §4.1 for LINER-like emission. This is inconsistent with the stated AGN/LINER exclusion criterion. Please either justify retaining SN1961V on physical grounds or show that the statistical results are unchanged after its removal.
  3. [§5.11, §6] The conclusion that the results give 'high statistical confidence of a different physical progenitor nature' goes beyond what a test on strong-line metallicity estimates can establish. The M13 calibration has intrinsic scatter, so the point estimates are noisy proxies for true oxygen abundance. The p-values test the distributions of the derived M13 estimates, not directly the distributions of true metallicities. The discussion should be revised to state this limitation explicitly and to frame the result as evidence that the strong-line metallicity indicator distributions differ, unless the calibration-scatter propagation requested above shows the result is robust.
minor comments (5)
  1. [Abstract, §1] The abstract renders 'H ii' as 'Hiienvironment'; please fix the LaTeX spacing.
  2. [Figure 9 caption] Typo: 'whne' should be 'when'.
  3. [§5.5] Typo: 'PPO4-O3N2' should be 'PP04-O3N2'.
  4. [Data Availability] The statement 'will be shared on reasonable request' and 'in due course' is vague for MNRAS; please provide a stable repository link or at least a clear availability statement.
  5. [Table 4, §4.6] No multiple-testing correction is applied across the several KS/AD tests, two calibrations, and sample combinations. The combined Ib+Ic p<0.001 would survive a Bonferroni correction, but the pairwise p-values near 0.005-0.008 should be interpreted with this in mind.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: central p-values derive from measured line ratios under an external metallicity calibration.

full rationale

The paper's central claim is a statistical comparison of measured SN-environment metallicities. The metallicities come from emission-line flux ratios converted through the Marino et al. (2013) calibration, which is external to this work and not fitted here. The KS/AD permutation tests are applied directly to these externally calibrated values; no parameter of the paper is fitted to the subtype CDFs and then renamed a prediction. The only self-citation is to Ganss et al. (2022, Paper I) for data-reduction details, classification procedures, and the earlier smaller sample; this is an extension rather than a load-bearing assumption that forces the present result. The paper's own caveat that including the ±0.18 dex calibration uncertainty makes a particular t-test marginally insignificant (§4.4) is an honest limitation about uncertainty propagation, not a circular dependency. No equation or definition in the paper reduces the result to its inputs. The central statistical significance is therefore self-contained conditional on the adopted external calibration, and any weakness lies in calibration-error treatment, not circularity.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The paper fits no new parameters and postulates no new physical entities. Its central inputs are external metallicity calibrations, literature classifications, and standard assumptions about HII region physics. The strongest implicit input, the representative-ness of local HII metallicity for the progenitor, is a domain assumption shared with prior work.

assumptions (4)
  • domain assumption Marino et al. (2013) N2 and O3N2 strong-line calibrations accurately trace gas-phase oxygen abundance of the SN environment HII regions.
    Section 3.3 and Section 4.1: all metallicities are derived from these external calibrations; the calibration scatter of plus/minus 0.16 to 0.18 dex is not propagated into the KS/AD tests.
  • domain assumption The metallicity of the HII region at the SN position is representative of the progenitor's birth metallicity.
    Section 1 argues massive stars live only 3 to 50 Myr and therefore do not migrate far from their natal environment, but this is not directly verified for individual targets.
  • domain assumption The literature classifications used to assign Type IIP, Ib, and Ic are accurate and clean.
    Section 2.1 and Section 5.10 describe extensive checks, but the authors themselves note residual issues such as hidden helium, IIb/Ib transitions, and ambiguous Type II classifications.
  • standard math Case B recombination (H-alpha/H-beta ratio of 2.86) and the adopted extinction curves provide a correct interstellar extinction correction.
    Section 3.1: Balmer decrement correction is applied assuming case B recombination and Osterbrock/Ferland extinction curves.

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Cite this review

Pith. "Pith review of Metallicity differences between Type IIP and stripped-envelope supernova environments." pith.science (2026). https://pith.science/paper/QPQPBEF5

@misc{pith2026250906526,
  author       = {Pith},
  title        = {Pith review of: Metallicity differences between Type IIP and stripped-envelope supernova environments},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QPQPBEF5}},
  note         = {Machine review of arXiv:2509.06526}
}
abstract

This work presents measurements of local HII environment metallicities of core-collapse supernovae (SNe) in hosts with redshifts up to z$\sim$0.025. 139 SNe environments were observed at the Isaac Newton Telescope and data of an additional 268 SNe environments were found in archival data of MUSE, MaNGA and PISCO. The project focuses on SNe with clean Type IIP, Type Ib and Type Ic classifications. We present the largest spectroscopic sample to date, evaluating environment metallicities of 79 Type Ib, 66 Type Ic and 93 Type IIP by N2 and O3N2 strong emission line methods. The cumulative distribution functions (CDFs) of the SN environment metallicities show Type Ib and Type Ic SNe tending towards higher metallicity than Type IIP. We test the null hypothesis that Type Ib/Ic/IIP progenitors are drawn from the same parent population. There is no statistically significant difference between progenitors of Type Ib and Type Ic SNe. However, when comparing Ib/Ic with IIP SNe, the tests indicate strong statistical significance (significance level better than 1\%) to reject our null hypothesis suggesting that the samples are not drawn from the same parent population. The significance is even higher (level better 0.1\%) when testing Type IIP vs. the combined Type Ib+Ic sample. These results support a different physical nature of Type IIP and Types Ib/Ic progenitors. It challenges stellar evolution and SNe explosion models to reproduce the distinct CDFs found.

Figures

Figures reproduced from arXiv: 2509.06526 by the authors.

Figure 1
Figure 1. Obtained INT/IDS spectrum of Type Ib SN2006dn environment as an example for the extracted 1D environment spectra. The figure shows the most prominent emission lines of which Hα, [N ii]λ6583, Hβ and [O iii]λ5007 have been used for the metallicity estimation. age Reduction and Analysis Facility; Tody 1986) and Star￾link (Currie et al. 2014), we processed the observational data with bias subtraction, flat correction an… view at source ↗
Figure 2
Figure 2. Example of PPXF emission line fit. The figure shows the PPXF fit of the explosion site spectrum of SN2001B obtained by INT/IDS. The obtained spectrum is shown in blue. The orange line is the best PPXF fit to the continuum including underlying stellar absorption lines. Green is the PPXF emission line fit. The light gray regions are masked to avoid any fitting issues by sky line residuals. The two inlays are zoomed Hβ… view at source ↗
Figure 3
Figure 3. BPT-diagram of all targets with O3N2 calibration (blue diamonds). The red solid line is the decision line between the H ii region and the AGN/LINER region as given by Kewley et al. (2001), equation (5). All targets but one (SN1961V) are well within the H ii region of the Kewley et al. (2001) decision line [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: CDFs of the SNe environment metallicities measured with the M13-N2 (left) and M13-O3N2 (right) calibration. Binning width for CDF calculation: 0.0125 dex. 4.3 Uncertainties The observational uncertainties of our observed data by pho￾ton noise and data reduction process…
Figure 6
Figure 6. Figure 6: Comparison of metallicities of targets observed by both IFU and by INT/IDS instruments for M13-N2 (blue diamonds) and M13-O3N2 (red squares). The dashed line represents the 1:1 line. There is no significant difference in the metallicities between the results obtained b…
Figure 7
Figure 7. Figure 7: Comparison of M13-O3N2 vs. M13-N2 calibration for all targets where both results are available. The black and blue over￾laid crosses represent the calibration uncertainties and the typical observational uncertainty, respectively. The dashed line is the 1:1 line. This f…
Figure 8
Figure 8. Figure 8: CDF scatter range of the Monte-Carlo simulations (20000 runs) for uncertainty ∆ = ±0.04 dex of M13-O3N2 samples. The solid lines are the undisturbed CDFs of [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]
Figure 9
Figure 9. Figure 9: Example of the effect of metallicity uncertainty on the p-value distribution based on Monte-Carlo (MC) simulations. The figures shown are the MC AD-test p-value distributions for the M13-N2 Ib sample vs. M13-N2 IIP sample (left) and vs. M13-N2 Ic sample (right). The up…
Figure 10
Figure 10. Figure 10: Explosion site of SN2012cw in NGC 3166 and the obtained emission lines at Hα (observer frame). The [NII] flux is stronger than Hα indicating low-ionisation LINER-like emission at a large distance from the host centre (projected distance: ∼5.1 kpc). low-ionisation exci…
Figure 11
Figure 11. Figure 11: Supplementary CDFs of the Type IIb (dark red) and Type IIn (gold) environment metallicities derived from archival envi￾ronment spectra. The CDFs are created with M13-N2 (left) and M13-O3N2 (right) calibrations. The dashed lines are the CDFs of our combined Type Ib+Ic …
Figure 12
Figure 12. Figure 12: CDFs of the SNe environment metallicities measured with the M13-N2 (left) and M13-O3N2 (right) calibration for the extended Type IIP+II sample (green solid line) and the clean Type IIP CDF (green dashdot line). The magenta dashed line is the combined Type Ib plus Type…

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Pith tools

Reviewed August 4, 2026 · model on record in the stance chip above.