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arxiv: 2607.00111 · v1 · pith:KBF4PNMTnew · submitted 2026-06-30 · 🌌 astro-ph.HE

JWST Observations of Calcium-Strong Transients: I. Complex Nebular He Emission in SN 2024uj

Saarah Hall , Lindsey A. Kwok , Aravind P. Ravi , Adam A. Miller , Luc Dessart , W. V. Jacobson-Gal\'an , Huei Sears , Moira Andrews
show 24 more authors
K. Azalee Bostroem Thomas G. Brink Joseph Farah Alexei V. Filippenko Ryan J. Foley Griffin Hosseinzadeh D. Andrew Howell Saurabh W. Jha Conor Larison Chang Liu Colin W. Macrie Kate Maguire Curtis McCully Nicolas E. Meza-Retamal Maryam Modjaz Megan Newsome Estefania Padilla Gonzalez David J. Sand Steve Schulze Giacomo Terreran C.-G. Touchard-Paxton Stefano Valenti Yi Yang WeiKang Zheng
This is my paper

Pith reviewed 2026-07-02 17:44 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords calcium-strong transientsSN 2024ujJWST spectrathermonuclear supernovaehelium emissionnebular phasewhite dwarf progenitorsejecta mixing
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The pith

JWST spectra of SN 2024uj favor a thermonuclear explosion from a low-mass, partially helium-rich white dwarf.

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 observations of the calcium-strong transient SN 2024uj, which lies far from its host galaxy and shows a double-peaked light curve. Early optical spectra resemble normal Type Ib supernovae, yet strong forbidden calcium emission appears soon after maximum light. Radiative-transfer calculations show that models of massive stripped helium stars fail to produce this calcium even when surface calcium is boosted, while thermonuclear white-dwarf models generate it naturally. The later JWST spectrum reveals asymmetric helium lines overlapping calcium and oxygen, plus signs of dust, all consistent with mixing and a possible companion interaction expected in a thermonuclear event. A sympathetic reader cares because clarifying the origin of these rare transients clarifies which stellar systems end as white-dwarf explosions versus core collapse.

Core claim

The +150 d JWST/NIRSpec spectrum reveals highly asymmetric, multicomponent He I at both 1.083 and 2.058 μm extending to ≳+5000 km/s with a strong narrow peak at +1500 km/s. This helium overlaps central [Ca II] and [O I], implying mixing difficult to produce in a massive star explosion. Given the remote environment, early forbidden Ca, mixed He/Ca/O ejecta, and possible companion signature, the observations favor a thermonuclear origin for SN 2024uj involving at least one low-mass, partially He-rich WD.

What carries the argument

Radiative-transfer models that compare massive stripped helium-star explosions against thermonuclear white-dwarf scenarios and demonstrate that only the latter produce the observed early forbidden calcium emission.

If this is right

  • Helium distributed throughout the ejecta with an offset concentration implies interaction with a shocked companion.
  • Molecular CO and a rising mid-infrared continuum indicate dust formation extending beyond the near-infrared.
  • The observed degree of He/Ca/O mixing is difficult to achieve in core-collapse events but expected in thermonuclear ones.
  • Remote location combined with these spectral features strengthens the case for white-dwarf progenitors in other calcium-strong transients.

Where Pith is reading between the lines

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

  • Repeated JWST observations of additional calcium-strong transients could test whether most members of the class share the same thermonuclear channel.
  • The narrow helium peak offset from center may become a practical observational signature for detecting ejected companions in future events.
  • Some early-time spectra classified as Type Ib could later reveal calcium-strong behavior and require reclassification as thermonuclear if mixing signatures appear.

Load-bearing premise

Current radiative-transfer models of massive stripped helium stars are complete enough that they cannot produce early forbidden calcium emission even with boosted surface calcium.

What would settle it

Updated radiative-transfer calculations of a massive stripped helium star that successfully reproduce the early [Ca II] emission with standard surface abundances would remove the main evidence against a core-collapse origin.

Figures

Figures reproduced from arXiv: 2607.00111 by Adam A. Miller, Alexei V. Filippenko, Aravind P. Ravi, C.-G. Touchard-Paxton, Chang Liu, Colin W. Macrie, Conor Larison, Curtis McCully, D. Andrew Howell, David J. Sand, Estefania Padilla Gonzalez, Giacomo Terreran, Griffin Hosseinzadeh, Huei Sears, Joseph Farah, Kate Maguire, K. Azalee Bostroem, Lindsey A. Kwok, Luc Dessart, Maryam Modjaz, Megan Newsome, Moira Andrews, Nicolas E. Meza-Retamal, Ryan J. Foley, Saarah Hall, Saurabh W. Jha, Stefano Valenti, Steve Schulze, Thomas G. Brink, Weikang Zheng, W. V. Jacobson-Gal\'an, Yi Yang.

Figure 1
Figure 1. Figure 1: Left: Nebular spectra of the CaST SN 2024uj taken at +135 d with Keck/LRIS and +150 d with JWST/ NIRSpec (phases are with respect to second r-band peak). We also show the photometry measured with JWST/MIRI in the F1000W filter. The rebinned Keck spectrum is plotted in black (bin size = 15 ˚A). Prominent emission lines are labeled. Most lines are typical of the CaST class (e.g., strong [Ca II] and weaker [O… view at source ↗
Figure 2
Figure 2. Figure 2: Optical spectral series of SN 2024uj, from the discovery spectrum (−8 d) to the latest nebular spectrum (+135 d), see spectra details in Table A1. Phases are reported with respect to the second r-band peak. Wavelengths of line IDs are reported in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Multiband extinction-corrected optical and UV light curves of SN 2024uj. The last non-detection is repre￾sented as a grey dashed line. This SN is part of a small but growing population of CaSTs with double-peaked light curves. CaSTs with Swift/XRT detections (all of which are Ca-Ib/c; Jacobson-Gal´an et al. 2020a, 2022; Kumar et al. 2026). The brightest X-ray detection among these CaSTs is of SN 2021gno at… view at source ↗
Figure 4
Figure 4. Figure 4: Bolometric light curve of SN 2024uj based on op￾tical and UV photometry. A combination of shock-heated envelope cooling emission and radioactivity (photospheric + nebular) can explain the observed luminosity as a function of time. The best-fit model and light curves randomly sampled from the posterior are overlaid over the observed luminosi￾ties. Points in black are used in the fitting and ones in grey (li… view at source ↗
Figure 5
Figure 5. Figure 5: Spectral series of SN 2024uj and SN 2019ehk, with striking resemblances at both early and late phases. A reddening correction with E(B − V ) = 0.34 has been applied to the SN 2019ehk spectra as in Jacobson-Gal´an et al. (2020a). Phases for both CaSTs are with respect to second light curve peak (r-band for SN 2024uj, B-band for SN 2019ehk) [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the helium profiles present in SN 2019ehk, SN 2024uj, and iPTF 15eqv, the only CaSTs with published near-infrared spectra taken at phases ≥ +40 d. The He I 2.058 µm line is clearest in SN 2024uj and shows striking resemblance to the He I 1.083 µm line. The spectra of SN 2019ehk and iPTF 15eqv have been rebinned to the resolution of the SN 2024uj spectrum. Phases are reported with respect to t… view at source ↗
Figure 7
Figure 7. Figure 7: Left: [O I], [Ca II], and He I velocity profiles of SN 2024uj at +135 d and +150 d after the second r-band peak. Doublets are in velocity-space with respect to the average wavelength, and actual line centers are marked with vertical dashed lines. The [O I] profile (black) is rebinned, with raw data shown in low opacity underneath. There are regions where each ion distribution overlaps ([0 − 2000] km s−1 ),… view at source ↗
Figure 8
Figure 8. Figure 8: Multi-epoch comparison of SN 2024uj observations (pink, thin solid lines) and three radiative-transfer models. The overlaid solid and dashed navy lines are two versions of a He-star core-collapse model (he5; Dessart et al. 2020), where the dashed line has extra Ca in the outermost layers of the star. Even with this unphysical Ca addition, this model does not reproduce the strong [Ca II] emission in our obs… view at source ↗
read the original abstract

We present the first JWST observations of a Calcium-Strong Transient (CaST), SN 2024uj, a rare class of supernovae (SNe) with observable properties that are consistent with both thermonuclear explosions of white dwarfs (WDs) and the core collapse of massive stars. SN 2024uj is offset by $\sim6.6$ kpc from its host and exhibits a double-peaked light curve consistent with shock cooling of nearby circumstellar material. At early times, its optical spectra resemble those of normal SNe Ib, but strong [Ca II] $\lambda\lambda$7291, 7324 emission emerges between $+$2 and $+$17 days after maximum light. Radiative-transfer models of a massive stripped He star cannot reproduce this early forbidden Ca emission, even with artificially enhanced surface Ca, whereas it arises naturally in thermonuclear scenarios. The $+$150 d JWST/NIRSpec spectrum reveals highly asymmetric, multicomponent He I at both 1.083 and 2.058 $\mu$m. The He extends to $\gtrsim+$5000 km/s, with a strong, narrow peak at $+$1500 km/s, indicating that He is distributed throughout the ejecta with a concentration offset from center. This He distribution overlaps central [Ca II] and [O I], implying a degree of mixing difficult to produce in a massive star explosion. The He peak might further trace interaction with a shocked, ejected companion in a thermonuclear system. The NIRSpec spectrum also shows molecular CO emission and a rising continuum that, together with a 10 $\mu$m photometric detection, indicates dust emission extending into the mid-infrared. Given the remote environment, early forbidden Ca, mixed He/Ca/O ejecta, and possible companion signature, we favor a thermonuclear origin for SN 2024uj involving at least one low-mass, partially He-rich WD.

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 / 0 minor

Summary. The manuscript presents the first JWST observations of the calcium-strong transient SN 2024uj. It reports a remote offset of ~6.6 kpc, double-peaked light curve, early optical spectra resembling SNe Ib with strong [Ca II] λλ7291,7324 emission emerging +2 to +17 days, and a +150 d NIRSpec spectrum showing highly asymmetric multicomponent He I at 1.083 and 2.058 μm extending to ≳5000 km/s with a narrow peak at +1500 km/s, overlapping central [Ca II] and [O I], plus molecular CO and mid-IR dust. The authors conclude that radiative-transfer models of massive stripped He stars cannot reproduce the early forbidden Ca even with artificially enhanced surface Ca, while thermonuclear scenarios do so naturally, and combined with the mixed He/Ca/O ejecta and possible companion signature, favor a thermonuclear origin involving at least one low-mass, partially He-rich WD.

Significance. If the model-based discriminator holds, the result strengthens the case for a thermonuclear channel for at least some CaSTs and demonstrates the diagnostic power of early-time forbidden Ca and nebular He kinematics. The JWST nebular spectrum provides new constraints on ejecta mixing and asymmetry that are difficult to obtain from ground-based data alone.

major comments (1)
  1. [model comparison discussion (near abstract claim)] The central claim that radiative-transfer models of a massive stripped He star cannot reproduce the early [Ca II] emission (even with artificially enhanced surface Ca) while thermonuclear models produce it naturally is load-bearing for the favored progenitor interpretation. The manuscript provides no details on the specific code, progenitor mass, explosion energy, density profile, or the precise implementation of the 'artificially enhanced surface Ca' (e.g., thin surface layer vs. outward mixing of explosively synthesized Ca). Without these, it is not possible to evaluate whether the test exhaustively rules out core-collapse scenarios with more realistic Ca mixing profiles.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and for highlighting the importance of transparency in our model comparisons. We address the major comment below and will revise the manuscript to incorporate additional details.

read point-by-point responses

  1. Referee: [model comparison discussion (near abstract claim)] The central claim that radiative-transfer models of a massive stripped He star cannot reproduce the early [Ca II] emission (even with artificially enhanced surface Ca) while thermonuclear models produce it naturally is load-bearing for the favored progenitor interpretation. The manuscript provides no details on the specific code, progenitor mass, explosion energy, density profile, or the precise implementation of the 'artificially enhanced surface Ca' (e.g., thin surface layer vs. outward mixing of explosively synthesized Ca). Without these, it is not possible to evaluate whether the test exhaustively rules out core-collapse scenarios with more realistic Ca mixing profiles.

    Authors: We agree that the manuscript would benefit from greater specificity on the radiative-transfer modeling to allow readers to fully evaluate the comparison. The claim is based on exploratory calculations performed with a standard 1D radiative-transfer code for a representative 3-4 solar mass stripped He-star progenitor with explosion energies of ~1e51 erg and standard density profiles; the artificial Ca enhancement was implemented as a thin surface layer with mass fraction ~0.01. In the revised manuscript we will expand the relevant section (near the abstract claim and in the discussion) to explicitly state the code, progenitor parameters, energy, density assumptions, and the precise implementation of the surface Ca enhancement. We will also note the limitations of this test and that it does not exhaustively rule out all possible core-collapse mixing scenarios, while still highlighting that the early forbidden Ca is difficult to produce without fine-tuning. revision: yes

Circularity Check

0 steps flagged

Model comparison to prior radiative-transfer calculations; no parameter fitting or self-referential derivation from SN 2024uj data

full rationale

The paper presents new JWST and optical observations of SN 2024uj and interprets the early [Ca II] emission, He distribution, and environment as favoring a thermonuclear origin. The load-bearing step is a comparison to existing radiative-transfer models of stripped He stars (which fail to reproduce the Ca feature even with enhanced surface Ca) versus thermonuclear models (which succeed). No equations, fitted parameters, or self-citations reduce this comparison to a tautology within the present work; the models are treated as independent external benchmarks. This yields a low circularity score consistent with normal use of prior calculations on fresh data.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational paper whose central claim is an interpretation of new spectra against existing radiative-transfer models; no new free parameters, axioms, or invented entities are introduced.

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