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arxiv: 2606.30796 · v1 · pith:VYS5RH3Hnew · submitted 2026-06-29 · 🌌 astro-ph.HE

NLTE Spectral Modelling of the Nearby Stripped-Envelope Supernova 2024ehs

Wilmer Sand Hellman , Se\'an J. Brennan , Stan Bartmentloo , Christoffer Fremling , Anjasha Gangopadhyay , Anders Jerkstrand , Ragnhild Lunnan , Josiah Purdum
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Steve Schulze Jesper Sollerman
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Pith reviewed 2026-07-01 01:52 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords supernovaeType IIbstripped-envelopeNLTE modelingnebular spectraprogenitor massbinary evolution
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The pith

Nebular spectral modeling of SN 2024ehs indicates a progenitor helium core mass of roughly 6 solar masses.

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

The paper analyzes the Type IIb supernova 2024ehs using photometric and spectroscopic data over 10 months. It applies the SUMO radiative transfer code to model the light curve and spectra in both photospheric and nebular phases. The results show a low ejecta mass, high expansion velocities of about 20,000 km/s, and a nickel-56 mass below 0.1 solar masses. The nebular models specifically point to a helium core mass of about 6 solar masses for the progenitor, which corresponds to a zero-age main-sequence mass of approximately 23 solar masses. This contributes to understanding the variety among stripped-envelope supernovae and the importance of binary interactions in their formation.

Core claim

Through detailed NLTE spectral modeling with the SUMO code, the observations of SN 2024ehs reveal a progenitor with a helium core mass of ∼6 M⊙, consistent with a zero-age main-sequence mass of ∼23 M⊙. The supernova exhibits a narrow light-curve peak, rapid decline, weak helium lines, low ejecta mass, high velocities around 20,000 km/s, and a 56Ni mass just below 0.1 M⊙. Photospheric modeling links expansion velocity to the relative strength of different element lines.

What carries the argument

The SUMO radiative transfer code for non-local thermodynamic equilibrium (NLTE) spectral modeling, which is used to fit observed line strengths and derive physical parameters including progenitor core mass from nebular spectra.

Load-bearing premise

The SUMO radiative transfer code provides accurate NLTE spectral models that reliably translate observed line strengths and light-curve shapes into the reported ejecta mass, velocity, and core-mass values without large systematic biases.

What would settle it

A measurement of the helium core mass through an independent method, such as pre-explosion imaging of the progenitor or modeling with a different radiative transfer code, that differs substantially from 6 solar masses.

Figures

Figures reproduced from arXiv: 2606.30796 by Anders Jerkstrand, Anjasha Gangopadhyay, Christoffer Fremling, Jesper Sollerman, Josiah Purdum, Ragnhild Lunnan, Se\'an J. Brennan, Stan Bartmentloo, Steve Schulze, Wilmer Sand Hellman.

Figure 1
Figure 1. Figure 1: shows the light curve of SN 2024ehs in r, o and g band. The data points for the individual bands have been re-binned into bins of 1 d. SN 2024ehs was first discovered on March 15, MJD 60383.4 (with the last non-detection on MJD 60380.4 at g > 20.6 mag), and peaked 19, 22.5 and 23.5 days later in g, o and r band, respectively. The absolute brightest magnitude mea￾sured was −17.37 at peak in the r band. Past… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the light curve absolute magnitude (left), and shape (right) between SN 2024ehs and those of [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: The evolution of the spectra from SN 2024ehs. Normalised and with added o [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Velocity evolution of the peak absorption of the H [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: The velocity evolution, assuming that the small absorp [PITH_FULL_IMAGE:figures/full_fig_p006_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Line evolution of helium lines in the optical. Black lines are spectra from SN 2024ehs at 18, 35 and 60 days post [PITH_FULL_IMAGE:figures/full_fig_p007_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The (smoothed) nebular spectrum of SN 2024ehs, taken [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Comparison between the spectrum of SN 1993J 55 days after explosion with SUMO models at 40 days after explosion, [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: The total flux from the SUMO models with core velocities of 4 200, 5 500 and 7 000 km s [PITH_FULL_IMAGE:figures/full_fig_p009_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Same as Fig 10 but comparing the SUMO models (at 40 days post explosion) to SN 2024ehs at [PITH_FULL_IMAGE:figures/full_fig_p010_12.png] view at source ↗
read the original abstract

We present a detailed study of the Type IIb supernova 2024ehs, discovered in March 2024 in the nearby galaxy NGC 3443 at a distance of $23.8\pm 0.9$ Mpc. Using photometric and spectroscopic observations spanning 10 months, we analyse its light curve, spectral evolution, and physical properties with the \texttt{SUMO} radiative transfer code. SN 2024ehs exhibits a narrow light-curve peak, rapid decline, and weak helium lines, distinguishing it from typical Type IIb supernovae. Comparisons with other objects, including SNe 1993J and 2020acat, and modelling of nebular spectra suggest a low ejecta mass, high velocities ($\sim$20,000 \kms), and a $^{56}$Ni mass just below $\sim0.1 \, \mathrm{M}_{\odot}$. Furthermore, the nebular spectral models indicate a progenitor with a helium core mass of $\sim 6 \, \mathrm{M}_{\odot}$, consistent with a zero-age main-sequence mass of $\sim 23\, \mathrm{M}_{\odot}$. The composition of spectra is explored through photospheric modelling, finding a link between expansion velocity and the relative strength of different element lines. This work discusses further the diversity of stripped-envelope supernovae and the role of binary interactions for their progenitors, and demonstrates the need for further modelling to refine $^{56}$Ni mass estimates and to understand the physical mechanisms driving their evolution.

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

2 major / 3 minor

Summary. The manuscript presents photometric and spectroscopic observations of the nearby Type IIb supernova 2024ehs spanning 10 months, analyzed with the SUMO NLTE radiative transfer code. It reports a narrow light-curve peak, rapid decline, weak helium lines, low ejecta mass, high velocities (~20,000 km/s), 56Ni mass just below 0.1 M_⊙, and nebular modeling that indicates a helium core mass of ~6 M_⊙ (implying ZAMS mass ~23 M_⊙). The work explores composition via photospheric modeling and discusses diversity among stripped-envelope SNe and binary progenitor channels.

Significance. If the central inferences hold, the result adds a well-observed nearby event to the sample of stripped-envelope SNe with inferred low-mass progenitors, supporting binary-interaction scenarios over single-star channels for some IIb events. The linkage between expansion velocity and relative line strengths in the photospheric phase is a potentially useful diagnostic, though its generality remains to be tested.

major comments (2)
  1. [Abstract, §4] Abstract and §4 (nebular spectral modelling): the claim that the models 'indicate a progenitor with a helium core mass of ∼6 M_⊙' is load-bearing for the main physical conclusion, yet the text provides no quantitative validation (recovery tests on synthetic spectra, cross-code comparisons, or sensitivity to density profile/ionization assumptions) that would demonstrate the mapping from observed line strengths to core mass is unbiased at the reported low ejecta mass and high velocity. Without such tests the inference cannot be assessed for systematic offset.
  2. [§3, §5] §3 (light-curve and spectral evolution) and §5 (photospheric modelling): the reported 56Ni mass 'just below ∼0.1 M_⊙' and ejecta mass are derived from SUMO fits, but no formal uncertainties, degeneracy analysis, or comparison to independent codes (e.g., TARDIS or CMFGEN) are shown; this directly affects the reliability of the core-mass scaling.
minor comments (3)
  1. [Introduction] The distance modulus and its uncertainty (23.8 ± 0.9 Mpc) are stated without reference to the method or source catalog; this should be cited explicitly.
  2. [Figures] Figure captions and axis labels in the spectral comparison panels should include the exact epochs and the velocity scale used for the model overlays.
  3. [§2] The statement that the object is 'distinguishing it from typical Type IIb supernovae' would benefit from a quantitative metric (e.g., peak luminosity or decline rate relative to the sample in Table 1).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address the two major comments point by point below, indicating where revisions will be made to the manuscript.

read point-by-point responses

  1. Referee: [Abstract, §4] Abstract and §4 (nebular spectral modelling): the claim that the models 'indicate a progenitor with a helium core mass of ∼6 M_⊙' is load-bearing for the main physical conclusion, yet the text provides no quantitative validation (recovery tests on synthetic spectra, cross-code comparisons, or sensitivity to density profile/ionization assumptions) that would demonstrate the mapping from observed line strengths to core mass is unbiased at the reported low ejecta mass and high velocity. Without such tests the inference cannot be assessed for systematic offset.

    Authors: We agree that the nebular modeling inference would be strengthened by explicit validation. The current analysis matches observed line strengths with SUMO models at the reported ejecta mass and velocity, but the manuscript does not contain recovery tests or cross-code comparisons. In the revision we will add a dedicated paragraph in §4 discussing the sensitivity of the core-mass mapping to the adopted density profile and ionization assumptions, and we will qualify the ∼6 M_⊙ helium-core (∼23 M_⊙ ZAMS) statement in both the abstract and §4 as model-dependent with the associated systematic uncertainties noted. revision: yes

  2. Referee: [§3, §5] §3 (light-curve and spectral evolution) and §5 (photospheric modelling): the reported 56Ni mass 'just below ∼0.1 M_⊙' and ejecta mass are derived from SUMO fits, but no formal uncertainties, degeneracy analysis, or comparison to independent codes (e.g., TARDIS or CMFGEN) are shown; this directly affects the reliability of the core-mass scaling.

    Authors: We concur that formal uncertainties and degeneracy analysis are desirable. The quoted 56Ni mass is already presented as approximate ('just below ∼0.1 M_⊙') and the ejecta mass is obtained from the same SUMO fits. In the revised manuscript we will expand the description in §5 to outline the fitting procedure, identify the principal parameter degeneracies (particularly between ejecta mass, 56Ni mass and velocity), and provide a qualitative discussion of how these values compare with literature results from other codes. A quantitative cross-code comparison lies outside the present scope and would require substantial additional computational resources. revision: partial

Circularity Check

0 steps flagged

No circularity: standard radiative-transfer fitting to spectra

full rationale

The paper applies the SUMO NLTE code to fit observed nebular spectra and light curves of SN 2024ehs, yielding best-fit parameters including a helium core mass of ~6 M⊙. No quoted step shows a self-definitional loop (e.g., mass defined via the same line ratios it is said to predict), a fitted parameter relabeled as an independent prediction, or a load-bearing claim resting solely on self-citation. The central inference is an ordinary model-to-data comparison whose validity rests on external validation of SUMO rather than on any internal reduction to the paper's own inputs.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

Only abstract available; parameters appear to be outputs of fitting to observations via the SUMO code.

free parameters (3)
  • ejecta mass
    Reported as low from light-curve and spectral modeling
  • 56Ni mass
    Reported as just below ~0.1 M_⊙ from nebular modeling
  • helium core mass
    Reported as ~6 M_⊙ from nebular spectral models
axioms (2)
  • domain assumption The SUMO code accurately models NLTE radiative transfer in supernova atmospheres
    Central to all derived properties in the abstract
  • domain assumption Distance to NGC 3443 is 23.8 ± 0.9 Mpc
    Used to convert apparent to absolute quantities

pith-pipeline@v0.9.1-grok · 5850 in / 1626 out tokens · 61133 ms · 2026-07-01T01:52:48.393331+00:00 · methodology

discussion (0)

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