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arxiv: 2604.18339 · v1 · submitted 2026-04-20 · 🌌 astro-ph.HE

Recognition: unknown

Probing the 3D Structures of Supernovae through IR Signatures of CO and SiO

T. Mera , P. Hoeflich , C. R. Burns , C. Ashall , K. Medler , E. Fereidouni , W. B. Hoogendam , M. Shahbandeh
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S. Shiber C. M. Pfeffer E. Baron J. Lu N. Morrell E. Y. Hsiao M. M. Phillips
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Pith reviewed 2026-05-10 04:08 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords supernovaeinfrared spectroscopyCOSiOmolecular emissionradiative transferclump structuresSN2024ggi
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The pith

A new fitting tool uses CO and SiO infrared bands to map three-dimensional clump structures in supernova ejecta.

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

The paper introduces MOFAT, a public tool that analyzes near- and mid-infrared spectra of supernovae by fitting them against time-independent radiative transfer models that incorporate multidimensional clump-like structures. This method is presented as necessary to reproduce the observed flux ratios between fundamental and overtone molecular bands, which simpler one-zone models cannot do without being distorted by optical depth effects. When applied to SN2024ggi at +285 and +385 days, the fits show that CO formation triggers SiO formation in inner layers, with the SiO-emitting region receding inward and its mass dropping by an order of magnitude, while most SiO flux comes from optically thin gas and no dust appears. Readers would care because these molecular zones and their small-scale structure connect the initial explosion to late-time chemistry and the possible origins of dust in the universe.

Core claim

MOFAT employs time-independent radiative transfer simulations that include multidimensional, clump-like structures to fit observed CO and SiO features in supernova spectra. This enables reconstruction of overall abundances and temperatures while determining parameterized small-scale structures associated with physical instabilities. Applied to SN2024ggi, CO formation triggers SiO formation in the inner layers of the CO-rich region. The inner edge of the SiO-emitting region recedes from velocities of 1500 to 1000 km/s, the SiO mass decreases from about (2-6) x 10^-3 solar masses by roughly an order of magnitude, SiO features indicate clumping but most flux originates from optically thin areas

What carries the argument

MOFAT, a spectral fitting tool that compares observations to radiative transfer models containing parameterized multidimensional clump-like structures in order to constrain abundances, temperatures, and small-scale ejecta instabilities.

Load-bearing premise

Time-independent radiative transfer simulations that add multidimensional clump-like structures can accurately reproduce the observed flux ratios between molecular bands and recover the true physical parameters without large optical-depth biases.

What would settle it

An independent determination of molecular column densities and spatial scales in a supernova, for example through high-resolution interferometry or fully time-dependent hydrodynamic-plus-chemistry simulations, that yields band flux ratios or abundances inconsistent with any MOFAT fit using clump structures.

Figures

Figures reproduced from arXiv: 2604.18339 by C. Ashall, C. M. Pfeffer, C. R. Burns, E. Baron, E. Fereidouni, E. Y. Hsiao, J. Lu, K. Medler, M. M. Phillips, M. Shahbandeh, N. Morrell, P. Hoeflich, S. Shiber, T. Mera, W. B. Hoogendam.

Figure 1
Figure 1. Figure 1: Left: The coordinate systems of (r, θ) and (p, z). rphoto is the photosphere, r1 and r1 + ∆r are the inner and outer radius of the molecular shell, respectively, and rj is some arbitrary radius. These locations coincide with the equivalent velocities in the right figure. Right: A cartoon graphic of how MOFAT works. The molecular clumps have semi-axes of rc and ra with a density enhancement factor of fc. Wh… view at source ↗
Figure 2
Figure 2. Figure 2: A schematic showing the iteration scheme used in MOFAT. The outermost loop loops through blocks, where each block closes particular switches for parameters it wants to test. Each selected parameter is then looped through, where temperature, NLTE, and total mass effects are iterated until the χ 2 statistic reaches a convergence criterion or a maximum number of iterations. This block can then be looped throu… view at source ↗
Figure 3
Figure 3. Figure 3: Temperature structures from select models from Tables 1 and 2 at days 285 (top) and 385 (bottom). For all of our models, the SiO molecules do not significant cool the ejecta at either epoch. tinguishable without sufficient time coverage (T. Mera et al. 2026). 3.1. Fitting Procedure The molecular forming region will have an outer edge that corresponds to the first instance of CO formation after the photosph… view at source ↗
Figure 4
Figure 4. Figure 4: Demonstrating the sensitivity of each parameter on the CO fundamental band of Model P at day 385 (see [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Demonstrating the χ 2 convergence for each of the seven parameters for Model P at day 385. For each panel, we keep the optimized parameters the same except for the parameter being varied. Panel A) shows temperature (T1) convergence for both the CO fundamental and overtone bands. For panels B-G we only show χ 2 of the fundamental band because the overtone does not show significant χ 2 differences between mo… view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Spectrum of Model P with and without clumping. are actively forming but mostly destroying SiO, with in￾conclusive results regarding the presence of clump-like structures. For future observations, we need low-latency observations during the CO formation period to probe mixing lengths and cooling regions conducive for SiO formation, and observations at late times to study small￾scale 3D morphologies in the S… view at source ↗
Figure 10
Figure 10. Figure 10: For given initial temperature structures of Models P (left) and O (right, [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Optical depth of Model PP at day 385 for the local peaks of the vibrational modes of the SiO fundamental band if clumps are not included. D. Vartanyan et al. 2025). MOFAT can only measure the average of these scales or the most dominant one, which limits the interpretation of the instability type and any potential separation of clump shape. Ideally, the surface to volume ratio difference between prolate a… view at source ↗
Figure 12
Figure 12. Figure 12: Demonstrating how the strength of decoupling between Trot and Tvib can change the ratios between the modes of the CO overtone and fundamental bands for T = 2000 K and no CO+. We show Tvib/Trot = 1, 0.8, 0.6, 0.3 and the NLTE correction factors when compared to LTE levels. (to first order T( 0v) ∼ v −0.5 ) and then use the molecular features as the driving force in temperature structure and NLTE correction… view at source ↗
Figure 13
Figure 13. Figure 13: Demonstrating the sensitivity of each parameter on the SiO fundamental band of Model PP at day 385. Panel A) shows the best-fit solution and continuum. Each of the following panels keeps the optimized parameters the same but shows the effect of the: B) total molecular mass (M), C) density structure (n), D) inner velocity edge (v1), E) width of molecular region (∆v), F) clump density contrast (fc), G) clum… view at source ↗
Figure 14
Figure 14. Figure 14: Demonstrating the χ 2 convergence for the fundamental band for each of the six primary parameters for Model PP at day 385. For each panel we keep the optimized parameters the same except for the parameter being varied. For panels A-F we only show χ 2 of the fundamental band because the overtone is virtually non-existent. Panel A) shows density structure (n), B) inner velocity edge (v1), C) width of the mo… view at source ↗
Figure 15
Figure 15. Figure 15: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Corner plot showing the distribution of parameters for 105 samples drawn from a normalizing flow model trained on 4000 randomly sampled models in the seven-dimensional parameter space. The flow learns an approximation to the underlying likelihood-weighted parameter distribution, which is then sampled to generate a smooth representation of the posterior. Darker regions indicate higher posterior density. Th… view at source ↗
read the original abstract

We present a new public-domain MOlecular Fitting Analysis Tool (MOFAT) designed to probe molecule-forming regions in supernovae (SNe) through analysis of molecular features in the near- and mid-infrared. MOFAT employs a novel data-driven approach to explore the physical properties of these regions using time-independent radiative transfer simulations that include multidimensional, clump-like structures, constrained by high-precision observations. Such structures are required to reproduce the flux ratio between fundamental and overtone bands, overcoming limitations of traditional one-zone forward-modeling, such as optical-depth effects and initial configurations. Our approach enables spectral fits that can reconstruct overall abundances and temperatures and determine parameterized small-scale structures associated with physical instabilities. We systematically study the relationship between physical parameters and the profiles of CO and SiO, showing that free parameters are constrained, while detection of small-scale structure requires optically thick bands. As a demonstration, MOFAT is applied to SN2024ggi at +285 and +385 days post-explosion. We find that CO formation triggers SiO formation in the inner layers of the CO-rich region previously studied. The inner edge of the SiO-emitting region recedes from velocities of v1 from 1500 to 1000 km/s, indicating continued SiO formation. The SiO mass decreases from about (2-6)E-3 Mo by roughly an order of magnitude, suggesting ongoing evaporation. SiO features indicate clumping, but most of the flux originates from optically thin regions. SiO contributes negligibly to cooling, and we find no evidence for dust formation. Finally, we discuss observational strategies to trace the evolution of molecule formation and its connection to dust formation.

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 / 1 minor

Summary. The manuscript introduces MOFAT, a public-domain tool for fitting near- and mid-IR spectra of supernovae that employs time-independent radiative transfer simulations incorporating multidimensional clump-like structures. It claims these structures are required to reproduce observed flux ratios between fundamental and overtone bands of CO and SiO, overcoming optical-depth limitations inherent to traditional one-zone models. The tool is applied to SN2024ggi at +285 and +385 days post-explosion, yielding results that CO formation triggers SiO in inner layers, the SiO-emitting region's inner edge recedes from 1500 to 1000 km/s, SiO mass decreases by an order of magnitude from (2-6)×10^{-3} M_⊙, SiO shows clumping but is mostly optically thin, SiO contributes negligibly to cooling, and there is no evidence for dust formation.

Significance. If the central claims hold, MOFAT would provide a new framework for constraining parameterized small-scale structures and molecular abundances in supernova ejecta via IR observations, with direct implications for linking molecule formation to dust production. The public release of the tool and its application to a recent, well-observed event like SN2024ggi represent concrete strengths that could enable reproducible follow-up studies.

major comments (3)
  1. [Abstract] Abstract: the assertion that multidimensional clump-like structures are required to reproduce the fundamental/overtone flux ratios (overcoming one-zone optical-depth effects) is not supported by any explicit comparison to flexible one-zone alternatives, such as models with radial temperature gradients, velocity-dependent excitation, or adjusted optical-depth scaling; without this, the necessity claim remains untested.
  2. [Abstract] Abstract and application section: the reported evolutionary changes in SiO mass, inner-edge velocity recession, and clumping are derived from fits in which clump structure parameters, abundances, and temperatures are simultaneously adjusted to match the same observed band ratios, creating a circularity risk that is not mitigated by independent constraints or synthetic recovery tests.
  3. [Abstract] Abstract: the time-independent radiative transfer assumption is adopted without discussion of how it might alias temporal evolution between the +285 d and +385 d epochs into the derived clump parameters or SiO recession; this is load-bearing for the evolutionary conclusions.
minor comments (1)
  1. [Abstract] The abstract refers to 'high-precision observations' and 'systematic study' of parameter relationships but does not identify the specific IR datasets, instruments, or reduction procedures used for SN2024ggi.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have identified areas where the manuscript can be strengthened. We address each major comment point by point below, indicating the revisions we will implement.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that multidimensional clump-like structures are required to reproduce the fundamental/overtone flux ratios (overcoming one-zone optical-depth effects) is not supported by any explicit comparison to flexible one-zone alternatives, such as models with radial temperature gradients, velocity-dependent excitation, or adjusted optical-depth scaling; without this, the necessity claim remains untested.

    Authors: We agree that the necessity claim in the abstract would be more robust with an explicit side-by-side comparison. The manuscript discusses the optical-depth limitations of standard one-zone models in the introduction and methods, but does not include a direct test against one-zone models incorporating radial gradients or velocity-dependent effects. We will add a dedicated comparison subsection (likely in the results or methods) that runs equivalent one-zone models with these flexibilities against the same SN2024ggi data to demonstrate that clump structures remain necessary to reproduce the observed band ratios. revision: yes

  2. Referee: [Abstract] Abstract and application section: the reported evolutionary changes in SiO mass, inner-edge velocity recession, and clumping are derived from fits in which clump structure parameters, abundances, and temperatures are simultaneously adjusted to match the same observed band ratios, creating a circularity risk that is not mitigated by independent constraints or synthetic recovery tests.

    Authors: The two epochs are fitted independently, and the multiple band ratios (fundamental and overtone for both CO and SiO) provide several independent constraints on the parameter space. However, we acknowledge the value of additional validation to address potential circularity. We will add synthetic recovery tests in a new subsection of the methods or results: mock spectra will be generated with known input parameters (including clump properties and SiO mass), noise-added to match the observations, and then recovered with MOFAT to quantify biases and demonstrate that the reported evolutionary trends are robust. revision: yes

  3. Referee: [Abstract] Abstract: the time-independent radiative transfer assumption is adopted without discussion of how it might alias temporal evolution between the +285 d and +385 d epochs into the derived clump parameters or SiO recession; this is load-bearing for the evolutionary conclusions.

    Authors: The time-independent radiative transfer is adopted because the dynamical timescale at these late epochs greatly exceeds the 100-day interval between observations, making the approximation reasonable for the spectral modeling. We agree, however, that the potential for aliasing should be explicitly discussed given its importance to the evolutionary claims. We will expand the methods section with a paragraph (and possibly a short appendix) that quantifies the approximation's validity, estimates possible biases on the SiO inner-edge recession and clump parameters, and notes how future time-dependent extensions could refine the results. revision: yes

Circularity Check

1 steps flagged

Fitted clump parameters and band-ratio matches presented as evidence that multidimensional structures are required, without shown necessity vs. one-zone alternatives

specific steps
  1. fitted input called prediction [Abstract]
    "Such structures are required to reproduce the flux ratio between fundamental and overtone bands, overcoming limitations of traditional one-zone forward-modeling, such as optical-depth effects and initial configurations. Our approach enables spectral fits that can reconstruct overall abundances and temperatures and determine parameterized small-scale structures associated with physical instabilities. ... We find that CO formation triggers SiO formation in the inner layers of the CO-rich region previously studied. The inner edge of the SiO-emitting region recedes from velocities of v1 from 1500 "

    The model is constructed with clump-like structures as free parameters; fitting them to match the observed fundamental/overtone ratios then yields the reported SiO masses, velocities, and clumping. The claim that the structures are 'required' follows directly from the success of this fit rather than from an independent test that no one-zone reparameterization can achieve equivalent ratios.

full rationale

The paper's core chain fits a time-independent RT model that already incorporates parameterized multidimensional clump-like structures to observed CO/SiO band ratios in SN2024ggi spectra. It then reports the resulting SiO masses, velocities, and clumping as physical findings while asserting that such structures are required to overcome one-zone optical-depth biases. This reduces the necessity claim to the modeling ansatz itself: the fit succeeds by construction when clumps are included, but no explicit comparison demonstrates that flexible one-zone reparameterizations (e.g., radial gradients or adjusted optical-depth scaling) cannot reproduce the same flux ratios within uncertainties. The specific results (inner-edge recession from 1500 to 1000 km/s, SiO mass drop by ~order of magnitude) are direct outputs of the same constrained fits rather than independent derivations. This produces moderate circularity confined to the justification step; the parameter-recovery procedure itself remains standard and self-contained once the model is adopted.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The modeling rests on fitted clump-structure parameters and physical quantities (abundances, temperatures) plus the assumption that time-independent radiative transfer suffices at late epochs; no new physical entities are postulated.

free parameters (2)
  • clump structure parameters
    Parameterized small-scale structures required to match fundamental-to-overtone band flux ratios.
  • abundances and temperatures
    Overall values reconstructed from spectral fits to CO and SiO features.
axioms (1)
  • domain assumption Time-independent radiative transfer accurately describes late-time (+285 d, +385 d) molecular emission
    Invoked for the simulations applied to SN2024ggi spectra.

pith-pipeline@v0.9.0 · 5687 in / 1420 out tokens · 55774 ms · 2026-05-10T04:08:53.253338+00:00 · methodology

discussion (0)

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Reference graph

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