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arxiv: 2606.28561 · v1 · pith:DXX4HMPQnew · submitted 2026-06-26 · 🌌 astro-ph.HE · astro-ph.SR

JWST observations of SN 2024abup: First Detection of CO in a broad-lined Type Ic Supernova and Constraints on r-process Nucleosynthesis

Manisha Shrestha , Lindsey A. Kwok , David J. Sand , Stan Bartmentloo , Collin Christy , Anders Jerkstrand , K. Azalee Bostroem , Jennifer E. Andrews
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Kate D. Alexander Yize Dong Carl E. Fields Emily Hoang Griffin Hosseinzadeh Brian Hsu Daryl Janzen Saurabh W. Jha Joel Johansson Jeniveve Pearson M. J. Lundquist Darshana Mehta Aidan Martas Maryam Modjaz Bernhard M\"uller Conor L. Ransome Aravind P. Ravi Mathieu Renzo Nicol\'as Meza Retamal Bhagya Subrayan Nathan Smith Stefano Valenti Sergiy Vasylyev Giacomo Ricigliano Peter J. Brown Moira Andrews Joseph Farah D. Andrew Howell Curtis McCully Megan Newsome Kathryn Wynn Ryan Chornock Natalie LeBaro Raffaella Margutti Melissa Shahbandeh Chris Ashall Peter Hoeflich
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Pith reviewed 2026-06-30 00:51 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords supernovaeType Ic supernovaeinfrared spectroscopycarbon monoxider-process nucleosynthesisdust productionJWST observations
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The pith

JWST spectra reveal carbon monoxide in broad-lined Type Ic supernova SN 2024abup

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

The paper reports the first JWST near- to mid-infrared observations of a broad-lined Type Ic supernova, SN 2024abup, at 41 days after maximum light. Spectral modeling with SUMO identifies broad features from carbon, oxygen, magnesium, and carbon monoxide, the earliest molecular detection in any core-collapse supernova. The spectrum shows possible dust continuum but no clear r-process element signatures amid the blends. These findings point to SNe Ic-bl as potential contributors to early-universe dust.

Core claim

Using the spectral synthesis code SUMO on JWST NIR+MIR data of SN 2024abup, the authors identify significant contributions from C, O, Mg, and CO in the broad IR line features, marking the earliest detection of molecules in a core-collapse supernova. No compelling infrared signatures of r-process elements are found due to blending with non-r-process features. The continuum at wavelengths greater than 1.5 micron could arise from dust.

What carries the argument

The spectral synthesis code SUMO, which models the contributions of elements and molecules to the observed broad infrared spectrum to identify specific species.

If this is right

  • SNe Ic-bl could be a contributor to early-universe dust production.
  • If r-process elements are produced, revealing their presence from spectra requires very high-quality data and models to disentangle blends.
  • Molecules such as CO can form in the ejecta of core-collapse supernovae as early as 54 days after explosion.

Where Pith is reading between the lines

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

  • Additional JWST observations of other SNe Ic-bl at similar epochs could test whether CO and dust features are common in this class.
  • Later-time or multi-epoch mid-IR data might separate potential r-process signals from the current blends.
  • The dust continuum opens questions about whether preexisting or newly formed dust dominates, testable with longer-wavelength follow-up.

Load-bearing premise

The spectral synthesis code SUMO correctly attributes the observed broad infrared features to C, O, Mg, and CO without significant contamination or misidentification from unmodeled lines or incorrect opacity assumptions.

What would settle it

Higher-resolution spectra or an independent model that cannot reproduce the features using C, O, Mg, and CO, or that instead matches r-process elements more closely, would challenge the identification.

Figures

Figures reproduced from arXiv: 2606.28561 by Aidan Martas, Anders Jerkstrand, Aravind P. Ravi, Bernhard M\"uller, Bhagya Subrayan, Brian Hsu, Carl E. Fields, Chris Ashall, Collin Christy, Conor L. Ransome, Curtis McCully, D. Andrew Howell, Darshana Mehta, Daryl Janzen, David J. Sand, Emily Hoang, Giacomo Ricigliano, Griffin Hosseinzadeh, Jeniveve Pearson, Jennifer E. Andrews, Joel Johansson, Joseph Farah, Kate D. Alexander, Kathryn Wynn, K. Azalee Bostroem, Lindsey A. Kwok, Manisha Shrestha, Maryam Modjaz, Mathieu Renzo, Megan Newsome, Melissa Shahbandeh, M. J. Lundquist, Moira Andrews, Natalie LeBaro, Nathan Smith, Nicol\'as Meza Retamal, Peter Hoeflich, Peter J. Brown, Raffaella Margutti, Ryan Chornock, Saurabh W. Jha, Sergiy Vasylyev, Stan Bartmentloo, Stefano Valenti, Yize Dong.

Figure 2
Figure 2. Figure 2: Extinction corrected optical spectrum of SN 2024abup from FLOYDS around Vmax on 60649.40 MJD compared to SN 2012ap, the best fit SN Ic-bl (D. Milisavlje￾vic et al. 2015) according to SNID-SAGE (F. Stoppa & S. J. Smartt 2026), near peak in V band. The similarity between the two objects provides confirmation of SN 2024abup’s clas￾sification as a SN Ic-bl (C. Balcon 2024). through Director’s Discretionary pro… view at source ↗
Figure 3
Figure 3. Figure 3: SN 2024abup spectrum spanning optical (FLOYDS) to MIR (JWST) + 41 days after the V band maximum. The top panel covers 0.4 to 14 µ m and subsequent panels zoom in on the optical spectrum, the third covers 1 to 2.6 µ m, the fourth is for 2.5 to 5 µ m, and the last one covers 5 to 14 µm. All the major lines identified using the SUMO model (see Section 5.1 and [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Multi-wavelength extinction corrected photome￾try of SN 2024abup spanning UV to optical observed using Swfit and LCO. The light-curve is well sampled to 80 days after the peak in the V band. 20 10 0 10 20 30 phase (days) 20 19 18 17 16 15 Absolute Magnitude V SN1998bw SN2002ap SN2007bg SN2009bb SN2003jd SN2024abup [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of extinction corrected abso￾lute V band magnitudes for a few different SN Ic-bl with (SN 1998bw) and without an associated GRB. The phases are given with respect to the date of Vmax. SN 2024abup (black circle) falls within a reasonable range with SN 1998bw, which is associated with a low-luminosity GRB, being the brightest [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: SN 2024abup compared to model from SUMO. The model is able to reproduce several observed spectral features. However, there are differences in the strength, which is expected as this model is not fine-tuned for this particular case. Overall, the observed continuum is higher than the model for wavelengths greater than ∼3 µm, which could be due to the presence of dust in the SN or the host galaxy or both, whi… view at source ↗
Figure 7
Figure 7. Figure 7: JWST spectrum of SN 2024abup at +41 days after V band maximum, overlaid with r-process element lines from G. Ricigliano et al. (2025) (solid red) and light element lines (colored dashed). The spectral features are more consistent with light elements, though line broadening may produce blending that complicates this identification. Insets show zoomed views of each individual feature. Wavelength Candidate Lo… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the NIR spectrum of SN 2024abup at +41 days with SN 1998bw (F. Patat et al. 2001), AT 2017gfo (E. Pian et al. 2017), and GRB 230307A (A. J. Levan et al. 2024). Similar lines are seen for both SN 1998bw and SN 2024abup. The [Te III] line is identified in AT2017gfo and GRB230307A as a signature of r-process element production. There is a bump in SN 2024abup near the [Te III] line, but it is bet… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of the JWST NIR + MIR spectra of SN (+41 days) and SN Ic 2023dbc (+36 days) (M. Shahbandeh et al. 2023). Major lines that are different between the two are shown in shaded gray regions. Lines from light and heavy species are indicated by dashed and solid lines, respectively. One of the major differences is the presence of prominent He I features in SN 2023dbc, which are absent in the case of SN … view at source ↗
Figure 10
Figure 10. Figure 10: SN 2024abup spectrum (black) along with the model of graphite, silicate, and PAH contribution (blue) and the host galaxy (orange). The prominent PAH lines, contributed mainly by the host galaxy, are identified by dashed teal lines. There is a clear excess in the continuum of SN 2024abup compared to the host galaxy spectrum. [Te III] in the case of AT 2017gfo and GRB 230307A. We see a feature at the same w… view at source ↗
Figure 11
Figure 11. Figure 11: Radio light curve of SN 2024abup at frequen￾cies shown in [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
read the original abstract

SN 2024abup is a nearby broad-lined Type Ic supernova (SN Ic-bl) in NGC 0681 at a distance of 23.3 \pm 1.6 Mpc. As energetic explosions of massive stars, SNe Ic-bl are considered a plausible site for rapid-neutron capture nucleosynthesis (r-process) and chemical enrichment from short-lived progenitors. They may also contribute to dust production in the early Universe. We present JWST near- to mid-infrared (NIR+MIR) observations (1-14 micron) of SN Ic-bl 2024abup at +41 days after the V band maximum (+54 days after explosion), the first-ever JWST+MIR observation of a SN Ic-bl along with radio and optical data. Using the spectral synthesis code SUMO, we identify the observed broad IR line features in SN 2024abup and find significant contributions from C, O, Mg, and carbon monoxide (CO) -- the earliest detection of molecules in a core-collapse SN so far. The spectrum shows continuum emission at wavelengths greater than 1.5 micron, which could be explained by dust -- preexisting, newly formed, or a combination-heated by the SN. We do not find compelling evidence for infrared signatures of r-process elements, though our search is hampered by the presence of many broad and blended features from the non-r-process elements. These new observations indicate that SNe Ic-bl could be a contributor to early-universe dust production, and suggest that if r-process elements are produced, revealing their presence from spectra requires very high-quality data and models to disentangle blends.

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

1 major / 1 minor

Summary. The manuscript reports JWST NIR+MIR (1-14 micron) observations of the nearby broad-lined Type Ic supernova SN 2024abup at +41 days after V-band maximum (+54 days post-explosion), supplemented by radio and optical data. Using the spectral synthesis code SUMO, the authors attribute the observed broad IR features to significant contributions from C, O, Mg, and CO—the earliest claimed molecular detection in a core-collapse SN. They note possible dust continuum emission at >1.5 micron and find no compelling IR signatures of r-process elements, attributing this partly to blending with non-r-process lines. The work suggests SNe Ic-bl as potential contributors to early-universe dust production.

Significance. The new JWST data on an SN Ic-bl represent a valuable observational advance, providing the first mid-IR coverage for this class and enabling searches for molecules and dust. If the CO identification is robust, the result would carry significance for chemical enrichment timelines and dust formation in energetic core-collapse events. The paper explicitly notes limitations from blending when discussing the non-detection of r-process signatures.

major comments (1)
  1. [Spectral modeling and feature identification] Modeling and line identification (description of SUMO application): The central claim of CO detection rests on SUMO attribution of blended 1-14 micron features without reported quantitative fit statistics (e.g., chi-squared or likelihood metrics), error bars on derived line strengths or abundances, or explicit sensitivity tests (e.g., fits excluding CO while retaining C/O/Mg). This directly affects the robustness of the 'earliest detection' assertion and the interpretation of the spectrum.
minor comments (1)
  1. [Abstract] The abstract states that SUMO 'identifies' contributions but provides no example wavelengths or specific feature assignments for CO, which would aid immediate assessment of the claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for recognizing the value of the first JWST mid-IR observations of an SN Ic-bl. We address the single major comment on spectral modeling below.

read point-by-point responses

  1. Referee: The central claim of CO detection rests on SUMO attribution of blended 1-14 micron features without reported quantitative fit statistics (e.g., chi-squared or likelihood metrics), error bars on derived line strengths or abundances, or explicit sensitivity tests (e.g., fits excluding CO while retaining C/O/Mg). This directly affects the robustness of the 'earliest detection' assertion and the interpretation of the spectrum.

    Authors: We acknowledge that the original manuscript does not include formal goodness-of-fit statistics or explicit sensitivity tests. SUMO is a spectral synthesis code that generates model spectra from specified abundances, temperature, and density profiles rather than performing automated statistical fitting; line identifications are therefore based on the requirement that specific features (particularly the broad 4.5-5 micron complex) cannot be reproduced without CO while retaining the observed C, O, and Mg contributions. To address the referee's concern, the revised manuscript will add (i) direct model comparisons with and without CO, (ii) a discussion of the parameter ranges that still provide acceptable visual matches, and (iii) approximate uncertainties on the CO and elemental abundances derived from those ranges. These additions will be presented in a new subsection on modeling robustness. revision: yes

Circularity Check

0 steps flagged

No significant circularity: observational attribution via external code on new data

full rationale

The paper's central claim rests on applying the pre-existing spectral synthesis code SUMO to new JWST NIR+MIR observations of SN 2024abup at +41 days. No equations, fitted parameters, or derivations are presented that reduce the reported line identifications (C, O, Mg, CO) to quantities defined from the same spectrum or to self-citations whose validity depends on the present result. The analysis is an interpretation step on external data using an independent tool; the reader's score of 2.0 reflects only routine code citation, not load-bearing circularity. No self-definitional, fitted-input, or uniqueness-imported patterns appear in the provided text.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Abstract-only review provides no explicit list of fitted parameters or ad-hoc assumptions beyond standard use of an existing spectral code; no invented entities are described.

axioms (1)
  • domain assumption Standard assumptions in supernova spectral modeling regarding atomic and molecular opacities and level populations
    Invoked when applying the SUMO code to match observed features.

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