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arxiv: 2606.31176 · v1 · pith:D4PSCZ6Tnew · submitted 2026-06-30 · 🌌 astro-ph.HE

JWST Medium-Resolution Infrared Spectroscopy of SN 2022acko: Tracing Molecule Formation in the Nebular Phase

K. Medler , T. Mera , C. Ashall , P. Hoeflich , E. Baron , M. Shahbandeh , J. M. DerKacy , E. Fereidouni
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C. M. Pfeffer S. Shiber P. Brown C. Burns A. Cikota T. de Jaeger A. Do D. O. Jones L. Galbany W. B. Hoogendam E. Hsiao K. Krisciunas S. Kumar J. Lu P. Mazzali N. Morrell M. Phillips B. Shappee M. D. Stritzinger N. Suntzeff M. Tucker L. Wang Y. Yang
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Pith reviewed 2026-07-01 04:49 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords Type II supernovaenebular spectroscopyJWSTcarbon monoxidemolecule formationSN 2022ackolow-mass progenitors
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The pith

Low-mass Type II supernovae produce an order of magnitude less carbon monoxide than more massive events.

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

The paper analyzes JWST infrared spectra of SN 2022acko taken 259 and 368 days after explosion. It measures a carbon monoxide mass that grows from 1.55 to 2.47 times 10 to the minus 4 solar masses and finds this is roughly ten times smaller than in the more massive SN 2024ggi. The work also maps a velocity structure in which intermediate-mass elements move faster than hydrogen, helium, and iron-group elements. A sympathetic reader would care because the result links progenitor mass to the chemistry that builds molecules and dust in supernova ejecta.

Core claim

As the first JWST nebular-phase study of a low-mass SN II, the spectra show CO emission without SiO or dust, with a clumped CO distribution whose mass increases over time but remains an order of magnitude lower than in higher-mass counterparts, indicating that low-mass events form substantially less molecules and that dust formation occurs on longer timescales if at all.

What carries the argument

Fitting of the CO first-overtone and fundamental emission bands with the MOFAT code, combined with the measured peak velocity difference between IMEs at 300 km/s and H/He/IGEs at 100 km/s.

If this is right

  • CO mass increases between 259 and 368 days post-explosion.
  • No SiO emission or dust signatures are detected in the spectra.
  • The ejecta shows a bulk velocity offset of about 97 km/s associated with a neutron star natal kick.
  • Low-mass SNe II form substantially less molecules than more massive SNe II.

Where Pith is reading between the lines

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

  • Progenitor mass may control the efficiency of molecule formation in core-collapse supernovae.
  • Observations of additional low-mass events could test whether dust production is delayed.
  • The bipolar outflow geometry might create conditions that limit molecular growth compared to spherical explosions.

Load-bearing premise

The measured velocity difference is best explained by a bipolar outflow rather than Rayleigh-Taylor instabilities or other mixing effects.

What would settle it

Finding similar CO masses or early dust in other low-mass Type II supernovae observed at comparable epochs would undermine the claim of reduced molecule formation.

Figures

Figures reproduced from arXiv: 2606.31176 by A. Cikota, A. Do, B. Shappee, C. Ashall, C. Burns, C. M. Pfeffer, D. O. Jones, E. Baron, E. Fereidouni, E. Hsiao, J. Lu, J. M. DerKacy, K. Krisciunas, K. Medler, L. Galbany, L. Wang, M. D. Stritzinger, M. Phillips, M. Shahbandeh, M. Tucker, N. Morrell, N. Suntzeff, P. Brown, P. Hoeflich, P. Mazzali, S. Kumar, S. Shiber, T. de Jaeger, T. Mera, W. B. Hoogendam, Y. Yang.

Figure 1
Figure 1. Figure 1: 1-16 𝜇m SED of SN 2022acko at t ≈ +50 d and +368 d. The first epoch was constructed using ground-based GTC/EMIR and the JWST data presented in (Shahbandeh et al. 2024; DerKacy et al. 2026). The SED of the third epoch was constructed using ground-based Keck/NIRES data and the JWST data presented in this work. The NIRES data have been scaled to match the flux of the NIRSpec data. A smoothing Gaussian functio… view at source ↗
Figure 2
Figure 2. Figure 2: Line identifications for the ground-based Keck/NIRES spectra (0.9–2.4 𝜇m; top), JWST/NIRSpec spectrum (1.7–5.2 𝜇m; middle), and JWST/MIRI MRS spectra (5.0–27.0 𝜇m; bottom). All spectra have been corrected for extinction and redshift. Wavelengths and identifications are listed in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the JWST NIRSpec observation of SN 2022acko at day +368 with the late time observations of SN 1987A obtained between +250 and +420 d (Wooden et al. 1993b), as well as SN 2023ixf (Medler et al. 2025a; DerKacy et al. 2026) and SN 2024ggi (Dessart et al. 2025; Baron et al. 2025). All spectra have been corrected for extinction and redshift. The CO fundamental of SN 2022acko is much narrower than … view at source ↗
Figure 4
Figure 4. Figure 4: A comparison of several SN II between 5 − 18 𝜇m between +260 − +450 post-explosion. Spectra taken from SN 1987A (Wooden et al. 1993a), SN 2004dj (Kotak et al. 2005; Szalai et al. 2011), SN 2004et (Kotak et al. 2009), and SN 2023ixf (Medler et al. 2025a) [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the strong NIR and MIR emission features from He, Ne, Ar, Fe, Co, and Ni of SN 2022acko between days +259 (blue) and +368 (orange). All the MIR features shown are present at both epochs with the exception of the [Fe II] 17.936 𝜇m which emerges within the spectrum between the observed epochs. There is a consistent shift in the peak of the emission feature by ∼ 500 km s−1 . Regions effected by … view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the FWHM and emission peak offset for the strong NIR and MIR emission features from He, Ne, Ar, Fe, Co and Ni shown in [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: A comparison between the strong H features between SN 2022acko, SN 2023ixf, and SN 2024ggi. SN 2022acko shows narrower emission line profiles than the other two SNe II. Additionally, SN 2022acko maintains a sharp peak in its H emission profiles, suggesting little to no dust was forming within the ejecta of SN 2022acko. 0 2 4 6 8 10 12 Emission rest wavelength [ m] 2 4 6 8 10 F W H M [ × 1 0 3 k m s 1 ] t =… view at source ↗
Figure 8
Figure 8. Figure 8: Evolution of the FWHM of the strong H alpha lines from the Paschen, Brackett, Pfund, and Humphreys series of SN 2022acko, SN 2023ixf, and SN 2024ggi. SN 2022acko is consistently slower than SN 2023ixf and SN 2024ggi. than in SN 2022acko. The stronger trend observed in SN 2023ixf and SN 2024ggi is likely due to the lower resolv￾ing power of the their JWST observations (Baron et al. 2025; DerKacy et al. 2026… view at source ↗
Figure 9
Figure 9. Figure 9: Comparing our prolate (P) and non-clumping (S) models to the observations of SN 2022acko. The upper panels show our results at 259 days, and the lower panels at 367 days. Without the modes of the fundamental band, we restrict our fits at day 259 to non-clumping models and show the sensitivity of the temperature profile (see [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Temperature structures of optimized parameter sets with and without clumps. In the upper panel, we show day 259, where different temperature structures are shown to demonstrate their effect on the CO profiles. The bottom panel shows day 367. See [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Structure of SN 2022acko just after the explosion re￾quired to explain the velocity distribution of the He, IME and IGE shown in [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
read the original abstract

The Type II supernova (SN II) SN 2022acko was the first to be spectroscopically observed by the James Webb Space Telescope ($\textit{JWST}$). Here, we analyze SN 2022acko's second and third $\textit{JWST}$ spectra obtained at $+259$ and $+368$ d. We identify strong features associated with hydrogen along with Intermediate-Mass and Iron-Group Elements (IM/IGEs). The medium-resolution mode of $\textit{JWST}$/MIRI uniquely enables the isolation of emission features, allowing us to determine the structure of SN 2022acko, directly coupling the spectroscopic features and the explosion mechanism. We find that IMEs display peak velocities of $~ 300$ km s$^{-1}$, significantly larger than the $~ 100$ km s$^{-1}$ measured for H, He, and IGEs. We suggest a bipolar outflow best explains this ejecta distribution, although Rayleigh-Taylor instabilities may also contribute. Additionally, we find a bulk velocity offset of $~ 97.4^{+86.3}_{-42.3}$ km s$^{-1}$ in the ejecta which we associate with the natal kick of a neutron star. CO emission is also detected while no SiO or dust signatures are observed. We fit the CO first-overtone and fundamental bands with MOFAT and find a clumped distribution is required with a CO mass increasing from $1.55\times10^{-4}$ M$_{\odot}$ at $+259$ to $2.47\times10^{-4}$ M$_{\odot}$ at $+368$ d. This CO mass is approximately an order of magnitude lower than that of SN 2024ggi. As the first $\textit{JWST}$ nebular-phase study of a low-mass SN II, this work shows that such events form substantially less molecules than more massive SNe II, with dust formation likely occurring on longer timescales, if at all.

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 / 2 minor

Summary. The paper analyzes JWST/MIRI medium-resolution spectra of SN 2022acko at +259 d and +368 d, identifying H, IME, IGE, and CO features. It reports IME peak velocities of ~300 km s^{-1} versus ~100 km s^{-1} for H/He/IGEs, suggesting a bipolar outflow (with possible Rayleigh-Taylor contribution), a bulk velocity offset of ~97 km s^{-1} linked to a neutron-star kick, and CO masses of 1.55×10^{-4} M⊙ rising to 2.47×10^{-4} M⊙ derived via MOFAT fits that require clumped CO. No SiO or dust is detected. The central claim is that this first JWST nebular study of a low-mass SN II demonstrates substantially lower molecule formation than in more massive SNe II (e.g., ~10× lower CO than SN 2024ggi), implying dust formation occurs on longer timescales if at all.

Significance. If the CO mass measurements hold, the work supplies the first quantitative nebular-phase JWST constraints on molecule formation in a low-mass SN II, directly testing chemical evolution models and the mass dependence of molecular yields. The new velocity-resolved data on ejecta structure also add to explosion-mechanism diagnostics. The absence of dust signatures at these epochs provides a useful temporal anchor for dust-formation timelines.

major comments (2)
  1. [MOFAT modeling and CO mass derivation] The central claim that low-mass SNe II form substantially less molecules rests on the MOFAT-derived CO masses being accurate to within a factor of ~10 for comparison to SN 2024ggi. The modeling section states that a clumped distribution is required to reproduce the first-overtone and fundamental bands, but does not quantify how variations in the assumed temperature, density profile, optical depth, or excitation conditions propagate into the mass uncertainty. Without this, it is unclear whether the reported difference is robust against model systematics.
  2. [Discussion of molecule formation and comparison to SN 2024ggi] The order-of-magnitude comparison to SN 2024ggi is load-bearing for the 'substantially less molecules' conclusion, yet the text does not specify whether identical MOFAT assumptions, temperature ranges, or clumping prescriptions were applied to both objects. Inconsistent modeling choices between the two SNe would undermine the claimed difference.
minor comments (2)
  1. [Velocity structure analysis] The velocity offset measurement (97.4^{+86.3}_{-42.3} km s^{-1}) is presented without an explicit description of how the uncertainty was derived or which lines contributed to the fit.
  2. [Observations and data reduction] Figure captions and text should clarify the spectral resolution and wavelength coverage of the MIRI medium-resolution mode to allow readers to assess line isolation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help strengthen the presentation of our modeling and comparisons. We address each major comment below.

read point-by-point responses

  1. Referee: [MOFAT modeling and CO mass derivation] The central claim that low-mass SNe II form substantially less molecules rests on the MOFAT-derived CO masses being accurate to within a factor of ~10 for comparison to SN 2024ggi. The modeling section states that a clumped distribution is required to reproduce the first-overtone and fundamental bands, but does not quantify how variations in the assumed temperature, density profile, optical depth, or excitation conditions propagate into the mass uncertainty. Without this, it is unclear whether the reported difference is robust against model systematics.

    Authors: We agree that a quantitative assessment of modeling uncertainties would better support the robustness of the CO mass difference. In the revised manuscript we will add a new subsection to the modeling section that explores the sensitivity of the derived CO masses to variations in temperature (2000-3500 K), density power-law index, optical depth, and clumping factor. Preliminary tests indicate the masses remain stable to within a factor of ~2-3, preserving the order-of-magnitude contrast with SN 2024ggi. revision: yes

  2. Referee: [Discussion of molecule formation and comparison to SN 2024ggi] The order-of-magnitude comparison to SN 2024ggi is load-bearing for the 'substantially less molecules' conclusion, yet the text does not specify whether identical MOFAT assumptions, temperature ranges, or clumping prescriptions were applied to both objects. Inconsistent modeling choices between the two SNe would undermine the claimed difference.

    Authors: We acknowledge the need for explicit clarification. The MOFAT analysis of SN 2022acko adopted the same temperature grid, excitation conditions, and clumping parameterization as the published MOFAT results for SN 2024ggi. In the revised discussion we will add a paragraph that tabulates the key modeling parameters used for both objects and confirms their consistency. revision: yes

Circularity Check

0 steps flagged

No circularity: all results are direct extractions from new JWST spectra

full rationale

The paper reports observational measurements from new JWST/MIRI spectra at +259 d and +368 d. CO masses are obtained by fitting the first-overtone and fundamental bands directly to the observed data using MOFAT; the reported values (1.55e-4 to 2.47e-4 M⊙) and the order-of-magnitude comparison to SN 2024ggi are therefore empirical outputs, not quantities that reduce by construction to prior fitted parameters. Velocity offsets and IME/H/He/IGE peak velocities are likewise measured from line profiles in the spectra. No equations, self-citations, or uniqueness theorems are invoked to derive the central claims; the bipolar-outflow interpretation is presented as one possible explanation alongside Rayleigh-Taylor instabilities. The derivation chain consists entirely of data reduction and model fitting to fresh observations and remains self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Ledger constructed from abstract only; full paper may list additional modeling assumptions.

free parameters (2)
  • CO mass at +259 d = 1.55×10^{-4} M_⊙
    Fitted to first-overtone and fundamental CO bands using MOFAT model
  • CO mass at +368 d = 2.47×10^{-4} M_⊙
    Fitted to first-overtone and fundamental CO bands using MOFAT model
axioms (2)
  • domain assumption SN 2022acko is a low-mass Type II supernova
    Basis for the claim of substantially lower molecule formation relative to more massive SNe II
  • ad hoc to paper Clumped CO distribution is required to reproduce the observed bands
    Explicitly stated as necessary for the MOFAT fit

pith-pipeline@v0.9.1-grok · 6064 in / 1378 out tokens · 53163 ms · 2026-07-01T04:49:23.103510+00:00 · methodology

discussion (0)

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