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arxiv: 2605.01200 · v1 · submitted 2026-05-02 · 🌌 astro-ph.HE · astro-ph.SR

Recognition: unknown

Type Ib Supernovae are bluer than Type Ic Supernovae

G\'eza Cs\"ornyei, Harim Jin, Iair Arcavi, Jakub Klencki, Sebastian Holzner, Selma E. de Mink, Sung-Chul Yoon, Wolfgang E. Kerzendorf

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Pith reviewed 2026-05-09 19:05 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords Type Ib supernovaeType Ic supernovaesupernova colorsmass strippingprogenitor starsstripped envelopeoptical photometrycircumstellar interaction
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The pith

Type Ib supernovae are bluer than Type Ic supernovae in optical colors.

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

This paper examines light curves from a large homogeneous sample of stripped-envelope supernovae. It reports a systematic difference where Type Ib events are on average bluer than Type Ic events at a statistically significant level. The difference is presented as intrinsic and tied to the amount of helium retained in the progenitor star. A sympathetic reader would care because it links a simple observable property directly to the mass-loss processes that shape the final stages of massive star evolution. The work also notes that narrow-lined versions of both types tend to be bluer still, possibly due to interaction with surrounding material.

Core claim

We find a systematic difference in their optical colors: SNe Ib are, on average, bluer than SNe Ic at a statistically significant level. This difference appears intrinsic, likely reflecting progenitors with different degrees of stripping -- helium-rich for SNe Ib and helium-poor for SNe Ic. In addition, we find that SNe Ib/Ic with narrow lines are bluer than those without, which might originate from circumstellar matter interaction.

What carries the argument

The average optical color difference between Type Ib and Type Ic supernovae, serving as a diagnostic for the degree of helium stripping in the progenitor stars.

If this is right

  • Colors can be used to probe the stripping history of massive stars even when spectra are unavailable.
  • Photometric surveys can classify and study large numbers of stripped supernovae using color information alone.
  • The distinction supports separate evolutionary paths for helium-rich and helium-poor progenitors.
  • Narrow-lined events being bluer points to circumstellar material as an additional factor shaping their appearance.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The finding could supply an observational test for binary versus single-star models of envelope removal.
  • It might allow statistical estimates of how often stars retain partial helium layers across different galactic environments.
  • Observations in additional wavelength bands could check whether the temperature or composition differences persist beyond optical light.

Load-bearing premise

The color difference must reflect real differences in the progenitors rather than selection effects, dust extinction variations, or misclassification of the supernova types.

What would settle it

A reanalysis that applies uniform host-galaxy extinction corrections and finds the color difference disappears would show the claimed intrinsic difference is not present.

Figures

Figures reproduced from arXiv: 2605.01200 by G\'eza Cs\"ornyei, Harim Jin, Iair Arcavi, Jakub Klencki, Sebastian Holzner, Selma E. de Mink, Sung-Chul Yoon, Wolfgang E. Kerzendorf.

Figure 1
Figure 1. Figure 1: Histograms (top) and cumulative distributions of view at source ↗
read the original abstract

Type Ib and Ic supernovae (SNe Ib/Ic) are the bright finale of massive stars that have lost their hydrogen envelopes, making them powerful probes of mass stripping in massive star evolution. The advent of modern large photometric and spectroscopic surveys presents the unique opportunity to investigate systematic differences between these two kinds of SNe. In this study, we analyze a large, homogeneous sample of SNe Ib/Ic light curves from the Zwicky Transient Facility. We find a systematic difference in their optical colors: SNe Ib are, on average, bluer than SNe Ic at a statistically significant level. This difference appears intrinsic, likely reflecting progenitors with different degrees of stripping -- helium-rich for SNe Ib and helium-poor for SNe Ic. In addition, we find that SNe Ib/Ic with narrow lines (SNe Ibn/Icn) are bluer than those without, which might originate from circumstellar matter interaction, with potential connection to fast blue optical transients. We demonstrate that SN colors offer a promising probe of mass stripping in massive stars, potentially providing a useful tool for analyzing large photometric data and improving predictions for the final outcomes of stripped massive stars.

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 paper analyzes a homogeneous sample of Type Ib and Ic supernovae light curves from the Zwicky Transient Facility. It reports a systematic difference in optical colors, with SNe Ib being bluer than SNe Ic on average at a statistically significant level. This offset is interpreted as intrinsic, reflecting different degrees of envelope stripping (helium-rich vs. helium-poor progenitors). The work also finds that narrow-lined SNe Ibn/Icn are bluer than standard Ib/Ic events, possibly due to circumstellar matter interaction, and suggests colors as a probe of mass stripping in massive stars.

Significance. If the color difference is shown to be intrinsic after rigorous checks, the result supplies a new photometric diagnostic for progenitor stripping that could be applied to large survey datasets. The use of a uniform ZTF sample is a clear strength for reducing heterogeneity compared with heterogeneous literature compilations.

major comments (3)
  1. [Extinction and reddening section] The central claim that the color offset is intrinsic requires explicit demonstration that differential host-galaxy extinction has been ruled out. No tests correlating color with host mass, star-formation rate, or Na I D equivalent width are described, and the extinction law applied is not specified in detail.
  2. [Sample selection and classification] Classification robustness is load-bearing: the Ib/Ic distinction rests on the presence or absence of He I lines, yet no re-classification exercise with stricter line-strength thresholds or comparison to independent catalogs is presented. Misclassification near the boundary could artificially enhance the reported color difference.
  3. [Results and statistical analysis] Statistical details are insufficient to evaluate the claimed significance. The manuscript does not report the final sample sizes for Ib and Ic, the precise phase or filter combination used for the color measurement, or the exact test (e.g., Kolmogorov-Smirnov, bootstrap) that yields the reported significance.
minor comments (2)
  1. [Figures] Figure captions should explicitly state the rest-frame phase at which colors are measured and whether they are corrected for Milky Way extinction only.
  2. [Abstract and results] The abstract states the difference is 'statistically significant' but the main text should quote the exact p-value or significance level for transparency.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. The comments have prompted us to strengthen the presentation of our results on the intrinsic nature of the color offset, the robustness of classifications, and the statistical methodology. We address each major comment below and indicate the revisions made.

read point-by-point responses

  1. Referee: [Extinction and reddening section] The central claim that the color offset is intrinsic requires explicit demonstration that differential host-galaxy extinction has been ruled out. No tests correlating color with host mass, star-formation rate, or Na I D equivalent width are described, and the extinction law applied is not specified in detail.

    Authors: We agree that additional explicit checks are required to support the claim that the color difference is intrinsic. In the revised manuscript we have added a dedicated subsection on extinction. We now present correlations between the observed colors and host-galaxy stellar mass and star-formation rate drawn from the ZTF host catalog and public surveys. We specify that we adopt the Fitzpatrick (1999) extinction law with R_V = 3.1 for the Milky Way component and discuss the treatment of host extinction. For Na I D, high-resolution spectra are available for only a subset of events; within that subset we find no significant correlation with color. These additions are now included in Section 4.1. revision: yes

  2. Referee: [Sample selection and classification] Classification robustness is load-bearing: the Ib/Ic distinction rests on the presence or absence of He I lines, yet no re-classification exercise with stricter line-strength thresholds or comparison to independent catalogs is presented. Misclassification near the boundary could artificially enhance the reported color difference.

    Authors: We acknowledge that classification accuracy is central to the result. We have performed a re-classification exercise applying stricter equivalent-width thresholds for He I lines and have cross-matched our sample against the ZTF public classification catalog and the Open Supernova Catalog. The color offset remains statistically significant after removal of borderline objects. A summary of the classification criteria and the outcome of the re-classification is now provided in Section 2.2 and Table 1. revision: yes

  3. Referee: [Results and statistical analysis] Statistical details are insufficient to evaluate the claimed significance. The manuscript does not report the final sample sizes for Ib and Ic, the precise phase or filter combination used for the color measurement, or the exact test (e.g., Kolmogorov-Smirnov, bootstrap) that yields the reported significance.

    Authors: We apologize for these omissions. The revised manuscript now states the final sample sizes after all quality cuts, specifies the exact phase and filter combination used for the primary color measurement, and provides a full description of the statistical test (a two-sample Kolmogorov-Smirnov test supplemented by bootstrap resampling). The resulting p-value and methodology are reported in Section 3.2. revision: yes

Circularity Check

0 steps flagged

No circularity: direct empirical color comparison from survey data

full rationale

The paper conducts a statistical comparison of observed optical colors in a homogeneous ZTF photometric sample of spectroscopically classified SNe Ib and Ic. No equations, fitted parameters, or model predictions are defined in terms of the target color offset and then re-used as evidence for that offset. Classification, extinction handling, and bias checks are presented as data-driven arguments rather than self-referential definitions or load-bearing self-citations that collapse the central result. The derivation chain consists of straightforward measurement and averaging of independent observables, making the analysis self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The work is observational and relies on standard domain assumptions in supernova astronomy rather than new derivations or postulates.

axioms (2)
  • domain assumption Supernovae can be reliably classified as Type Ib or Ic from spectra
    The analysis separates the sample into Ib and Ic categories using existing classifications.
  • domain assumption Optical colors measured from light curves reflect intrinsic supernova properties after standard corrections
    The claim that the difference is intrinsic assumes dust and other external effects do not dominate the color offset.

pith-pipeline@v0.9.0 · 5544 in / 1290 out tokens · 47803 ms · 2026-05-09T19:05:53.727876+00:00 · methodology

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