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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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Works this paper leans on

138 extracted references · 121 canonical work pages · 8 internal anchors

  1. [1]

    2024, Monthly Notices of the Royal Astronomical Society, 527, 11970, 10.1093/mnras/stad3776

    Aamer, A., Nicholl, M., Jerkstrand, A., et al. 2024, Monthly Notices of the Royal Astronomical Society, 527, 11970, 10.1093/mnras/stad3776

    work page doi:10.1093/mnras/stad3776 2024

  2. [2]

    Arnett , W. D. 1982, , 253, 785, 10.1086/159681

    work page doi:10.1086/159681 1982

  3. [3]

    2024, The Astrophysical Journal, 975, 203, 10.3847/1538-4357/ad6608

    Ashall, C., Hoeflich, P., Baron, E., et al. 2024, The Astrophysical Journal, 975, 203, 10.3847/1538-4357/ad6608

    work page doi:10.3847/1538-4357/ad6608 2024

  4. [4]

    M., & Banerjee, D

    Ashok, N. M., & Banerjee, D. P. K. 2003, Astronomy & Astrophysics, 409, 1007. https://www.aanda.org/articles/aa/abs/2003/39/aah4263/aah4263.html

    2003

  5. [5]

    P., Tollerud, E

    Astropy Collaboration , Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, 10.1051/0004-6361/201322068

    work page doi:10.1051/0004-6361/201322068 2013

  6. [6]

    M., Sip Hocz, B

    Astropy Collaboration , Price-Whelan, A. M., Sip Hocz, B. M., et al. 2018, aj, 156, 123, 10.3847/1538-3881/aabc4f

    work page doi:10.3847/1538-3881/aabc4f 2018

  7. [7]

    2025, The Astrophysical Journal, 983, 101, 10.3847/1538-4357/adc00a

    Baer-Way, R., Chandra, P., Modjaz, M., et al. 2025, The Astrophysical Journal, 983, 101, 10.3847/1538-4357/adc00a

    work page doi:10.3847/1538-4357/adc00a 2025

  8. [8]

    J., Weinberg, N

    Bildsten, L., Shen, K. J., Weinberg, N. N., & Nelemans, G. 2007, The Astrophysical Journal, 662, L95, 10.1086/519489

    work page doi:10.1086/519489 2007

  9. [9]

    M., Giardino, G., Sirianni, M., et al

    Birkmann, S. M., Giardino, G., Sirianni, M., et al. 2022, in Proceedings of SPIE , Volume 12180, Vol. 12180, eprint: arXiv:2208.12686, 121802P, 10.1117/12.2629545

    work page doi:10.1117/12.2629545 2022

  10. [10]

    J., Ramsbottom, C

    Blondin, S., Dessart, L., Hillier, D. J., Ramsbottom, C. A., & Storey, P. J. 2023, Astronomy & Astrophysics, 678, A170, 10.1051/0004-6361/202347147

    work page doi:10.1051/0004-6361/202347147 2023

  11. [11]

    A., Hachinger, S., & Kerzendorf, W

    Boyle, A., Sim, S. A., Hachinger, S., & Kerzendorf, W. 2017, Astronomy & Astrophysics, 599, A46. https://www.aanda.org/articles/aa/full_html/2017/03/aa29712-16/aa29712-16.html

    2017

  12. [12]

    , keywords =

    Breeveld , A. A., Curran , P. A., Hoversten , E. A., et al. 2010, , 406, 1687, 10.1111/j.1365-2966.2010.16832.x

    work page doi:10.1111/j.1365-2966.2010.16832.x 2010

  13. [13]

    M., Baliber, N., Bianco, F

    Brown, T. M., Baliber, N., Bianco, F. B., et al. 2013, Publications of the Astronomical Society of the Pacific, 125, 1031, 10.1086/673168

    work page internal anchor Pith review doi:10.1086/673168 2013

  14. [14]

    Buckley, D. A. H., Swart, G. P., & Meiring, J. G. 2006, in Proceedings of SPIE , Volume 6267, Vol. 6267, 62670Z, 10.1117/12.673750

    work page doi:10.1117/12.673750 2006

  15. [15]

    B., Nordsieck, K

    Burgh, E. B., Nordsieck, K. H., Kobulnicky, H. A., et al. 2003, in Proceedings of SPIE , Volume 4841, Vol. 4841, 1463--1471, 10.1117/12.460312

    work page doi:10.1117/12.460312 2003

  16. [16]

    N., Hill, J

    Burrows, D. N., Hill, J. E., Nousek, J. A., et al. 2005, Space Science Reviews, 120, 165, 10.1007/s11214-005-5097-2

    work page internal anchor Pith review doi:10.1007/s11214-005-5097-2 2005

  17. [17]

    2022, JWST Calibration Pipeline , Zenodo, 10.5281/zenodo.7041998

    Bushouse, H., Eisenhamer, J., Dencheva, N., et al. 2022, JWST Calibration Pipeline , Zenodo, 10.5281/zenodo.7041998

    work page doi:10.5281/zenodo.7041998 2022

  18. [18]

    1984, The Messenger, 38, 9

    Buzzoni, B., Delabre, B., Dekker, H., et al. 1984, The Messenger, 38, 9. https://ui.adsabs.harvard.edu/abs/1984Msngr..38....9B

    1984

  19. [19]

    L., Birkmann, S

    Böker, T., Beck, T. L., Birkmann, S. M., et al. 2023, Publications of the Astronomical Society of the Pacific, 135, 038001, 10.1088/1538-3873/acb846

    work page doi:10.1088/1538-3873/acb846 2023

  20. [20]

    P., Collins, C

    Callan, F. P., Collins, C. E., Sim, S. A., et al. 2025 a , Monthly Notices of the Royal Astronomical Society, 539, 1404, 10.1093/mnras/staf539

    work page doi:10.1093/mnras/staf539 2025

  21. [21]

    P., Holas, A., Morán-Fraile, J., et al

    Callan, F. P., Holas, A., Morán-Fraile, J., et al. 2025 b , NLTE spectral modelling for a carbon-oxygen and helium white-dwarf merger as a Ca -rich transient candidate, arXiv, 10.48550/arXiv.2503.12105

    work page doi:10.48550/arxiv.2503.12105 2025

  22. [22]

    R., Cook, D., & Vreeswijk, P

    Cao, Y., Kulkarni, S. R., Cook, D., & Vreeswijk, P. 2015, The Astronomer's Telegram, 8428, 1. https://ui.adsabs.harvard.edu/abs/2015ATel.8428....1C

    2015

  23. [23]

    A., Chugai, N., Milisavljevic, D., & Fransson, C

    Chandra, P., Chevalier, R. A., Chugai, N., Milisavljevic, D., & Fransson, C. 2020, The Astrophysical Journal, 902, 55, 10.3847/1538-4357/abb460

    work page doi:10.3847/1538-4357/abb460 2020

  24. [24]

    2025, SN 2025coe: A Triple - Peaked Calcium - Strong Transient from A White - Dwarf Progenitor , arXiv, 10.48550/arXiv.2510.00135

    Chen, C., Sun, N.-C., Xi, Q., et al. 2025, SN 2025coe: A Triple - Peaked Calcium - Strong Transient from A White - Dwarf Progenitor , arXiv, 10.48550/arXiv.2510.00135

    work page doi:10.48550/arxiv.2510.00135 2025

  25. [25]

    C., Crain, J

    Clemens, J. C., Crain, J. A., & Anderson, R. 2004, in Proceedings of SPIE , Volume 5492, Vol. 5492, 331--340, 10.1117/12.550069

    work page doi:10.1117/12.550069 2004

  26. [26]

    A., Modjaz, M., et al

    Crawford, A., Pritchard, T. A., Modjaz, M., et al. 2025, The Astrophysical Journal, 989, 192, 10.3847/1538-4357/adea3a

    work page doi:10.3847/1538-4357/adea3a 2025

  27. [27]

    2024, Transient Name Server Classification Report, 2024-521, 1

    Davis, K., Arunachalam, P., Foley, R., & Kwok, L. 2024, Transient Name Server Classification Report, 2024-521, 1. https://ui.adsabs.harvard.edu/abs/2024TNSCR.521....1D

    2024

  28. [28]

    C., Gal-Yam, A., et al

    De, K., Fremling, U. C., Gal-Yam, A., et al. 2021, The Astrophysical Journal, 907, L18, 10.3847/2041-8213/abd627

    work page doi:10.3847/2041-8213/abd627 2021

  29. [29]

    M., Cantwell, T., et al

    De, K., Kasliwal, M. M., Cantwell, T., et al. 2018, The Astrophysical Journal, 866, 72, 10.3847/1538-4357/aadf8e

    work page doi:10.3847/1538-4357/aadf8e 2018

  30. [30]

    M., Tzanidakis, A., et al

    De, K., Kasliwal, M. M., Tzanidakis, A., et al. 2020, The Astrophysical Journal, 905, 58, 10.3847/1538-4357/abb45c

    work page doi:10.3847/1538-4357/abb45c 2020

  31. [31]

    M., Ashall, C., Hoeflich, P., et al

    DerKacy, J. M., Ashall, C., Hoeflich, P., et al. 2023, The Astrophysical Journal Letters, 945, L2, 10.3847/2041-8213/acb8a8

    work page doi:10.3847/2041-8213/acb8a8 2023

  32. [32]

    2024, The Astrophysical Journal, 961, 187, 10.3847/1538-4357/ad0b7b

    ---. 2024, The Astrophysical Journal, 961, 187, 10.3847/1538-4357/ad0b7b

    work page doi:10.3847/1538-4357/ad0b7b 2024

  33. [33]

    M., Ashall, C., Baron, E., et al

    DerKacy, J. M., Ashall, C., Baron, E., et al. 2026, The Astrophysical Journal, 997, 179, 10.3847/1538-4357/ae1f87

    work page doi:10.3847/1538-4357/ae1f87 2026

  34. [34]

    Dessart, L., & Hillier, D. J. 2015, Monthly Notices of the Royal Astronomical Society, 447, 1370, 10.1093/mnras/stu2520

    work page doi:10.1093/mnras/stu2520 2015

  35. [35]

    J., Sukhbold, T., Woosley, S

    Dessart, L., Hillier, D. J., Sukhbold, T., Woosley, S. E., & Janka, H.-T. 2021, Astronomy and Astrophysics, 656, A61, 10.1051/0004-6361/202141927

    work page doi:10.1051/0004-6361/202141927 2021

  36. [36]

    J., Woosley, S., et al

    Dessart, L., Hillier, D. J., Woosley, S., et al. 2015. https://ui.adsabs.harvard.edu/abs/2015MNRAS.453.2189D/abstract

    2015

  37. [37]

    2025, An optical to infrared study of type II SN2024ggi at nebular times, arXiv, 10.48550/arXiv.2507.05803

    Dessart, L., Kotak, R., Jacobson-Galan, W., et al. 2025, An optical to infrared study of type II SN2024ggi at nebular times, arXiv, 10.48550/arXiv.2507.05803

    work page doi:10.48550/arxiv.2507.05803 2025

  38. [38]

    R., & Langer, N

    Dessart, L., Yoon, S.-C., Aguilera-Dena, D. R., & Langer, N. 2020, Astronomy and Astrophysics, 642, A106, 10.1051/0004-6361/202038763

    work page doi:10.1051/0004-6361/202038763 2020

  39. [39]

    R., et al

    Dimitriadis, G., Maguire, K., Karambelkar, V. R., et al. 2023, Monthly Notices of the Royal Astronomical Society, 521, 1162, 10.1093/mnras/stad536

    work page doi:10.1093/mnras/stad536 2023

  40. [40]

    2022, The Astrophysical Journal, 927, 199, 10.3847/1538-4357/ac5257

    Dong, Y., Milisavljevic, D., Leja, J., et al. 2022, The Astrophysical Journal, 927, 199, 10.3847/1538-4357/ac5257

    work page doi:10.3847/1538-4357/ac5257 2022

  41. [41]

    2023, Monthly Notices of the Royal Astronomical Society, 526, 279, 10.1093/mnras/stad2705

    Ertini, K., Folatelli, G., Martinez, L., et al. 2023, Monthly Notices of the Royal Astronomical Society, 526, 279, 10.1093/mnras/stad2705

    work page doi:10.1093/mnras/stad2705 2023

  42. [42]

    A., Beardmore, A

    Evans, P. A., Beardmore, A. P., Page, K. L., et al. 2007, Astronomy and Astrophysics, 469, 379, 10.1051/0004-6361:20077530

    work page doi:10.1051/0004-6361:20077530 2007

  43. [43]

    , keywords =

    ---. 2009, Monthly Notices of the Royal Astronomical Society, 397, 1177, 10.1111/j.1365-2966.2009.14913.x

    work page doi:10.1111/j.1365-2966.2009.14913.x 2009

  44. [44]

    Filippenko, A. V. 1982, Publications of the Astronomical Society of the Pacific, 94, 715, 10.1086/131052

    work page doi:10.1086/131052 1982

  45. [45]

    V., Chornock, R., Swift, B., et al

    Filippenko, A. V., Chornock, R., Swift, B., et al. 2003, International Astronomical Union Circular, 8159, 2. https://ui.adsabs.harvard.edu/abs/2003IAUC.8159....2F

    2003

  46. [46]

    Foley, R. J. 2015, Monthly Notices of the Royal Astronomical Society, 452, 2463, 10.1093/mnras/stv789

    work page doi:10.1093/mnras/stv789 2015

  47. [47]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, pasp, 125, 306, 10.1086/670067

    work page doi:10.1086/670067 2013

  48. [48]

    2000, 10.1086/317361

    Fryxell, B., Olson, K., Ricker, P., et al. 2000, 10.1086/317361

    work page doi:10.1086/317361 2000

  49. [49]

    , keywords =

    Gal-Yam, A., Ofek, E. O., & Shemmer, O. 2002, Monthly Notices of the Royal Astronomical Society, 332, L73, 10.1046/j.1365-8711.2002.05535.x

    work page doi:10.1046/j.1365-8711.2002.05535.x 2002

  50. [50]

    2019, Astronomy and Astrophysics, 630, A76, 10.1051/0004-6361/201935537

    Galbany, L., Ashall, C., Höflich, P., et al. 2019, Astronomy and Astrophysics, 630, A76, 10.1051/0004-6361/201935537

    work page doi:10.1051/0004-6361/201935537 2019

  51. [51]

    2004, 10.1086/422091

    Gehrels, N., Chincarini, G., Giommi, P., et al. 2004, 10.1086/422091

    work page doi:10.1086/422091 2004

  52. [52]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, nat, 585, 357, 10.1038/s41586-020-2649-2

    work page doi:10.1038/s41586-020-2649-2 2020

  53. [53]

    2014, HEAsoft : Unified Release of FTOOLS and XANADU

    HEASARC . 2014, HEAsoft : Unified Release of FTOOLS and XANADU

    2014

  54. [54]

    A., Templeton, M., Terrell, D., et al

    Henden, A. A., Templeton, M., Terrell, D., et al. 2016, VizieR Online Data Catalog: AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016), VizieR On-line Data Catalog: II/336. Originally published in: 2015AAS...22533616H. https://ui.adsabs.harvard.edu/abs/2016yCat.2336....0H

    2016

  55. [55]

    2016, Astronomy and Astrophysics, 594, A116, 10.1051/0004-6361/201629178

    HI4PI Collaboration , Ben Bekhti, N., Flöer, L., et al. 2016, Astronomy and Astrophysics, 594, A116, 10.1051/0004-6361/201629178

    work page doi:10.1051/0004-6361/201629178 2016

  56. [56]

    Monthly Notices of the Royal Astronomical Society , volume =

    Hillier, D. J., & Dessart, L. 2012, Monthly Notices of the Royal Astronomical Society, 424, 252, 10.1111/j.1365-2966.2012.21192.x

    work page doi:10.1111/j.1365-2966.2012.21192.x 2012

  57. [57]

    M., Jørgensen, I., Allington-Smith, J

    Hook, I. M., Jørgensen, I., Allington-Smith, J. R., et al. 2004, Publications of the Astronomical Society of the Pacific, 116, 425, 10.1086/383624

    work page doi:10.1086/383624 2004

  58. [58]

    A., & Gomez, S

    Hosseinzadeh, G., Bostroem, K. A., & Gomez, S. 2023, Light Curve Fitting, v0.8.0, Zenodo, 10.5281/zenodo.7872772

    work page doi:10.5281/zenodo.7872772 2023

  59. [59]

    2019, in American Astronomical Society Meeting Abstracts, Vol

    Howell , D. 2019, in American Astronomical Society Meeting Abstracts, Vol. 233, American Astronomical Society Meeting Abstracts \#233, 258.16

    2019

  60. [60]

    Hunter, J. D. 2007, Computing in Science and Engineering, 9, 90, 10.1109/MCSE.2007.55

    work page doi:10.1109/mcse.2007.55 2007

  61. [61]

    2017, Monthly Notices of the Royal Astronomical Society, 468, 4642, 10.1093/mnras/stx834

    Inserra, C., Nicholl, M., Chen, T.-W., et al. 2017, Monthly Notices of the Royal Astronomical Society, 468, 4642, 10.1093/mnras/stx834

    work page doi:10.1093/mnras/stx834 2017

  62. [62]

    2025, Transient Name Server AstroNote, 21, 1

    Jacobson-Galán, W. 2025, Transient Name Server AstroNote, 21, 1. https://ui.adsabs.harvard.edu/abs/2025TNSAN..21....1J

    2025

  63. [63]

    Mapping 3-D Explosive Nucleosynthesis with Type II Supernova Infrared Emission Lines

    Jacobson-Galán, W. V., Dessart, L., & Vartanyan, D. 2026, Mapping 3- D Explosive Nucleosynthesis with Type II Supernova Infrared Emission Lines , arXiv, 10.48550/arXiv.2605.18951

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.18951 2026

  64. [64]

    V., Foley, R

    Jacobson-Galán, W. V., Foley, R. J., Schwab, J., et al. 2019, Monthly Notices of the Royal Astronomical Society, 487, 2538, 10.1093/mnras/stz1305

    work page doi:10.1093/mnras/stz1305 2019

  65. [65]

    V., Margutti, R., Kilpatrick, C

    Jacobson-Galán, W. V., Margutti, R., Kilpatrick, C. D., et al. 2020 a , The Astrophysical Journal, 898, 166, 10.3847/1538-4357/ab9e66

    work page doi:10.3847/1538-4357/ab9e66 2020

  66. [66]

    V., Polin, A., Foley, R

    Jacobson-Galán, W. V., Polin, A., Foley, R. J., et al. 2020 b , The Astrophysical Journal, 896, 165, 10.3847/1538-4357/ab94b8

    work page doi:10.3847/1538-4357/ab94b8 2020

  67. [67]

    V., Margutti, R., Kilpatrick, C

    Jacobson-Galán, W. V., Margutti, R., Kilpatrick, C. D., et al. 2021, The Astrophysical Journal, 908, L32, 10.3847/2041-8213/abdebc

    work page doi:10.3847/2041-8213/abdebc 2021

  68. [68]

    V., Venkatraman, P., Margutti, R., et al

    Jacobson-Galán, W. V., Venkatraman, P., Margutti, R., et al. 2022, The Astrophysical Journal, 932, 58, 10.3847/1538-4357/ac67dc

    work page doi:10.3847/1538-4357/ac67dc 2022

  69. [69]

    V., Dessart, L., Kilpatrick, C

    Jacobson-Galán, W. V., Dessart, L., Kilpatrick, C. D., et al. 2025, The Astrophysical Journal, 994, L14, 10.3847/2041-8213/ae157a

    work page doi:10.3847/2041-8213/ae157a 2025

  70. [70]

    Jakobsen, P., Ferruit, P., Oliveira, C. A. d., et al. 2022, Astronomy & Astrophysics, 661, A80. https://www.aanda.org/articles/aa/full_html/2022/05/aa42663-21/aa42663-21.html

    2022

  71. [71]

    2017, in Handbook of Supernovae (Springer), 795--842, 10.1007/978-3-319-21846-5_29

    Jerkstrand, A. 2017, in Handbook of Supernovae (Springer), 795--842, 10.1007/978-3-319-21846-5_29

    work page doi:10.1007/978-3-319-21846-5_29 2017

  72. [72]

    J., Fraser, M., et al

    Jerkstrand, A., Smartt, S. J., Fraser, M., et al. 2014, Monthly Notices of the Royal Astronomical Society, 439, 3694, 10.1093/mnras/stu221

    work page doi:10.1093/mnras/stu221 2014

  73. [73]

    2021, ApJ, 923, L8, doi: 10.3847/2041-8213/ac375f

    Jiang, J.-a., Maeda, K., Kawabata, M., et al. 2021, The Astrophysical Journal Letters, 923, L8, 10.3847/2041-8213/ac375f

    work page doi:10.3847/2041-8213/ac375f 2021

  74. [74]

    O., Foley, R

    Jones, D. O., Foley, R. J., Narayan, G., et al. 2021, The Astrophysical Journal, 908, 143, 10.3847/1538-4357/abd7f5

    work page doi:10.3847/1538-4357/abd7f5 2021

  75. [75]

    M., Kulkarni, S

    Kasliwal, M. M., Kulkarni, S. R., Gal-Yam, A., et al. 2012, The Astrophysical Journal, 755, 161, 10.1088/0004-637X/755/2/161

    work page doi:10.1088/0004-637x/755/2/161 2012

  76. [76]

    S., Maeda, K., Nomoto, K., et al

    Kawabata, K. S., Maeda, K., Nomoto, K., et al. 2010, Nature, 465, 326, 10.1038/nature09055

    work page doi:10.1038/nature09055 2010

  77. [77]

    Kleiser, I. K. W., & Kasen, D. 2014, Monthly Notices of the Royal Astronomical Society, 438, 318, 10.1093/mnras/stt2191

    work page doi:10.1093/mnras/stt2191 2014

  78. [78]

    A., Nordsieck, K

    Kobulnicky, H. A., Nordsieck, K. H., Burgh, E. B., et al. 2003, in Proceedings of SPIE , Volume 4841, Vol. 4841, 1634--1644, 10.1117/12.460315

    work page doi:10.1117/12.460315 2003

  79. [79]

    P., et al

    Kumar, S., Baer-Way, R., Ravi, A. P., et al. 2026, A multiwavelength view of the nearby Calcium - Strong Transient SN 2025coe in the X - Ray , Near - Infrared , and Radio Wavebands , arXiv, 10.48550/arXiv.2601.19018

    work page doi:10.48550/arxiv.2601.19018 2026

  80. [80]

    V., et al

    Kwok, L., Dessart, L., Filippenko, A. V., et al. 2024 a , JWST Proposal. Cycle 2, 6591. https://ui.adsabs.harvard.edu/abs/2024jwst.prop.6591K

    2024

Showing first 80 references.