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arxiv: 2604.09777 · v1 · submitted 2026-04-10 · 🌌 astro-ph.HE

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JWST Nebular Spectroscopy of SN 2023qov: Circumstellar Dust Emission in a Normal Type Ia Supernova

Abigail Polin, Alexei V. Filippenko, Anders Jerkstrand, Armin Rest, Bailey Martin, Barnab\'as Barna, Brad Tucker, Carles Badenes, Christopher Lidman, Colin W. Macrie, Conor Larison, D. Andrew Howell, David Sand, Estefania Padilla Gonzalez, Griffin Hosseinzadeh, Huei Sears, Jacco Terwel, Joel Johansson, Joseph R. Farah, Jozsef Vinko, Kate Maguire, K. Auchettl, K. Azalee Bostroem, Keiichi Maeda, Kyle W. Davis, Lindsey A. Kwok, Lingzhi Wang, Matthew Siebert, Megan Newsome, Michaela Schwab, Mi Dai, Moira Andrews, Mridweeka Singh, Or Graur, Ori D. Fox, Reka Konyves-Toth, Saarah Hall, Saurabh W. Jha, St\'ephane Blondin, T\'amas Szalai, Tea Temim, Thomas G. Brink, Weikang Zheng, Xiaofeng Wang, Zoe Rosenberg

Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:26 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords Type Ia supernovaecircumstellar dustlight echoinfrared spectroscopyJWSTnebular phasedust emission
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The pith

JWST spectra detect circumstellar dust emission in a normal Type Ia supernova for the first time.

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

The paper reports mid-infrared observations of SN 2023qov at 276 and 363 days after maximum light that reveal thermal dust emission around 400 K cooling by about 75 K. This constitutes the first unambiguous spectroscopic detection of such emission in a typical Type Ia supernova. Models of carbonaceous dust placed within roughly one light year of the explosion and totaling about 10^{-4} solar masses reproduce the spectrum. The lack of signs of ongoing dust formation leads the authors to conclude that the emission is an infrared light echo from pre-existing circumstellar material rather than newly synthesized dust.

Core claim

The first unambiguous spectroscopic detection of dust emission in a normal SN Ia is reported from JWST near- and mid-infrared spectra. The emission is well described by models of carbonaceous dust placed within ~1 light year of the SN, with a dust mass of ~10^{-4} M_⊙. No evidence of active dust creation is seen, indicating an infrared light echo by pre-existing circumstellar dust as the likely source.

What carries the argument

Infrared light echo from pre-existing circumstellar carbonaceous dust, which reproduces the observed cooling mid-infrared continuum without requiring new dust formation.

Where Pith is reading between the lines

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

  • Similar JWST observations of additional normal Type Ia supernovae could determine how frequently such circumstellar dust shells occur around their progenitors.
  • The dust location implies prior mass loss from the progenitor system, which could be tested by searching for narrow absorption features at earlier phases.
  • Continued monitoring of the emission's temperature and luminosity would constrain the three-dimensional geometry of the dust distribution.

Load-bearing premise

The mid-infrared continuum arises solely from pre-existing circumstellar carbonaceous dust heated by the supernova light echo, with no significant contribution from newly formed dust, line emission, or other sources.

What would settle it

Detection of silicate dust spectral features, rapid variability inconsistent with light-echo cooling, or the absence of comparable dust signatures in other normal SNe Ia observed at similar epochs with JWST would undermine the pre-existing dust interpretation.

Figures

Figures reproduced from arXiv: 2604.09777 by Abigail Polin, Alexei V. Filippenko, Anders Jerkstrand, Armin Rest, Bailey Martin, Barnab\'as Barna, Brad Tucker, Carles Badenes, Christopher Lidman, Colin W. Macrie, Conor Larison, D. Andrew Howell, David Sand, Estefania Padilla Gonzalez, Griffin Hosseinzadeh, Huei Sears, Jacco Terwel, Joel Johansson, Joseph R. Farah, Jozsef Vinko, Kate Maguire, K. Auchettl, K. Azalee Bostroem, Keiichi Maeda, Kyle W. Davis, Lindsey A. Kwok, Lingzhi Wang, Matthew Siebert, Megan Newsome, Michaela Schwab, Mi Dai, Moira Andrews, Mridweeka Singh, Or Graur, Ori D. Fox, Reka Konyves-Toth, Saarah Hall, Saurabh W. Jha, St\'ephane Blondin, T\'amas Szalai, Tea Temim, Thomas G. Brink, Weikang Zheng, Xiaofeng Wang, Zoe Rosenberg.

Figure 1
Figure 1. Figure 1: Las Cumbres Observatory gri image of SN 2023qov and its elliptical host galaxy NGC 7029 four days before peak bright￾ness. Based on our computed distance to SN 2023qov and the angu￾lar separation, its projected distance is 28 kpc from the host center. cumstellar dust. Moreover, we present early-time light-curve modeling and velocity measurements to investigate progen￾itor and explosion scenarios, comparing… view at source ↗
Figure 2
Figure 2. Figure 2: Top: Bessel BV- and SDSS gri-band photometry of SN 2023qov from Las Cumbres Observatory and ATLAS oc-band photometry. The light curve is shown relative to B-band maximum light. Apparent magnitudes are corrected for line-of-sight Milky Way dust extinction. Bottom: the pseudobolometric light curve, combining the BgVri bands with the built-in SNooPy bolometric light curve routine (see Section 3.1). that the a… view at source ↗
Figure 3
Figure 3. Figure 3: Spectral time series of SN 2023qov, with scaled flux density and wavelength in the rest frame. The spectra are labeled by rest-frame phase relative to the B-band peak. The Si II λ6355 absorption feature is highlighted in the early spectra. The full list of observations is presented in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Optical and NIR/MIR spectra of SN 2023qov taken at +276 (brighter spectra, shades of blue) and +363 (fainter spectra, shades of red) days since peak brightness. Dashed lines show a fading blackbody at T = 475 K (red) and T = 400 K (blue). These blackbody fits are discussed in Section 4. 20 10 0 10 20 30 40 50 60 Rest-Frame Phase (days) 12 14 16 18 20 Magnitude + offset i + 3 o + 2 r + 1 V c 1 g 2 B 3 SALT2… view at source ↗
Figure 5
Figure 5. Figure 5: Early light-curve photometry fit with SALT2 and BayeSN models. SALT2 is signified by the dashed gray line, and BayeSN by the dash-dotted black line. BayeSN is cut off beyond 40 days and before −14 days as it is best trained to fit the peak features of the light curve, and it does better than SALT2 in that range. BayeSN does not have built-in bandpasses for ATLAS o and c. for the distance modulus directly, … view at source ↗
Figure 6
Figure 6. Figure 6: The B − V color curve of SN 2023qov compared with SNe Ia 1994D (Hicken et al. 2009), 2021aefx (Hosseinzadeh et al. 2023), 2022aaiq, and 2024gy (Kwok et al. 2025b), corrected for Milky Way dust extinction EMW(B − V ). Rest-frame phase is relative to the time of B maximum. The line shows the Lira￾Phillips relation (Lira 1996; Phillips et al. 1999), where t(Vmax) ≈ 60194.7 ± 0.1, or 1.5 days after t(Bmax). sh… view at source ↗
Figure 8
Figure 8. Figure 8: Two epochs of JWST spectra fit against carbonaceous dust models from Jager et al. ¨ (1998) (dash-dotted line) and Draine & Lee (1984) (solid line), both with 2σ model uncertainties overplotted. The region 3.5–6 µm was used to fit the models, with the blended [Ca V]/[Fe II] 4.2 µm feature cut out (denoted with the red shaded region). A notable feature in SN 2023qov is the double-peaked (“horned”) nature of … view at source ↗
Figure 9
Figure 9. Figure 9: Possible shell radii (rshell) of CSM around SN 2023qov, plotted against the maximum continuum temperature to which the dust is heated TD, from a spherical dust IR echo model (Sec￾tion 4.2). Here, TGra/AMC,+276d is our measured temperature for both dust species (Section 4.1), corresponding to a lower limit on TD, and TEvap is the maximum temperature allowed for the species of dust. The blackbody radii are r… view at source ↗
Figure 10
Figure 10. Figure 10: Nebular line fits to the blackbody-subtracted JWST/MIRI spectra (black). The top panel shows epoch 1 (∆t = +276 d); the bottom panel shows epoch 2 (∆t = +363 d). The less blended features on the left side of the plot are weighted more heavily in the fit, so the lines in the heavily blended 10–11 µm feature are well constrained, with the exemption of [S IV] and [Co II], which do not appear outside of the b… view at source ↗
Figure 11
Figure 11. Figure 11: Simple torus model fit of [Ar II] and [Ar III] features marked in [PITH_FULL_IMAGE:figures/full_fig_p014_11.png] view at source ↗
read the original abstract

We present panchromatic observations of the Type Ia supernova (SN Ia) 2023qov, ranging from $\sim$2 weeks before to $\sim$1 year after maximum light. \textit{JWST} near- and mid-infrared spectra at $+$276 and $+$363~days show $\sim$400 K dust emission that cools by $\sim$75 K between epochs, the first unambiguous spectroscopic detection of dust emission in a normal SN Ia. We find that the emission is well described by models of carbonaceous dust placed within $\sim$1 light year of the SN, with a dust mass of $\sim$$10^{-4}$ M$_{\odot}$. We do not see evidence of active dust creation, suggesting an infrared light echo by pre-existing circumstellar dust as the likely source of the emission. The \textit{JWST} nebular line profiles suggest asymmetric, stratified ejecta, similar to other normal SNe Ia, though a slight double-horn structure in the argon lines indicate a toroidal enhancement. SN 2023qov exhibits a slightly red, fast-declining early light curve ($\Delta m_{15}(B) = 1.47 \pm 0.05$ mag), from which we determine a $^{56}$Ni mass of $M_{56} = 0.21 \pm 0.04$ M$_{\odot}$, and a distance of $d = 36.0 \pm 1.8$ Mpc to the SN and its host, NGC 7029.

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 manuscript presents panchromatic observations of the normal Type Ia supernova SN 2023qov, spanning from ~2 weeks pre-maximum to ~1 year post-maximum. JWST near- and mid-infrared spectra at +276 and +363 days reveal ~400 K dust emission cooling by ~75 K, modeled as carbonaceous dust with mass ~10^{-4} M_⊙ located within ~1 light year, interpreted as the first unambiguous spectroscopic detection of dust emission in a normal SN Ia arising from an infrared light echo by pre-existing circumstellar dust. No evidence for active dust creation is reported. Nebular line profiles indicate asymmetric, stratified ejecta with possible toroidal enhancement in argon lines. Light-curve analysis yields a 56Ni mass of 0.21 ± 0.04 M_⊙ and a distance of 36.0 ± 1.8 Mpc to the host NGC 7029.

Significance. If the spectral decomposition and dust modeling hold, this would be a significant result for SN Ia progenitor studies, offering direct spectroscopic evidence of circumstellar dust and a light-echo origin in a normal event. The two-epoch JWST coverage documenting cooling is a clear strength, as is the linkage to early-time photometry for the nickel mass. Such a detection could help constrain dust production channels and circumstellar environments around SNe Ia. The significance is reduced, however, until the exclusivity of the pre-existing dust interpretation is more rigorously demonstrated against possible contaminants.

major comments (2)
  1. [Abstract and spectral modeling results] The central claim of an 'unambiguous' spectroscopic detection and the light-echo interpretation from pre-existing dust (Abstract) rests on the mid-IR continuum being fully accounted for by the adopted carbonaceous dust models (T ~400 K cooling to ~325 K, M_d ~10^{-4} M_⊙) with no significant residuals from nebular lines such as [Ar II] or [Ne II] and no contribution from newly condensed dust. The manuscript should supply residual spectra after dust-model subtraction at both epochs together with quantitative upper limits on any additional components to substantiate the statement that 'we do not see evidence of active dust creation'.
  2. [Dust emission modeling] The dust models are stated to 'well describe' the emission, yet the paper must report goodness-of-fit metrics (e.g., reduced χ²) and explicitly compare against alternative grain compositions or geometries to show that the chosen carbonaceous, ~1 ly shell model is preferred. Without these, parameter degeneracies among temperature, mass, and distance cannot be assessed and the 'likely' attribution remains under-supported.
minor comments (2)
  1. [Abstract and light-curve section] Clarify whether the reported distance of 36.0 ± 1.8 Mpc is derived exclusively from the SN light-curve fit or incorporates independent host-galaxy redshift or Tully-Fisher information.
  2. [Nebular spectroscopy results] The nebular line-profile discussion mentions a 'slight double-horn structure' in argon lines; include a quantitative measure (e.g., velocity separation or flux ratio) and compare directly to other normal SNe Ia to strengthen the toroidal-enhancement claim.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript on the JWST observations of SN 2023qov. We appreciate the positive assessment of the scientific significance and have addressed each major comment below with revisions to the manuscript where needed to strengthen the presentation of our dust modeling results.

read point-by-point responses

  1. Referee: [Abstract and spectral modeling results] The central claim of an 'unambiguous' spectroscopic detection and the light-echo interpretation from pre-existing dust (Abstract) rests on the mid-IR continuum being fully accounted for by the adopted carbonaceous dust models (T ~400 K cooling to ~325 K, M_d ~10^{-4} M_⊙) with no significant residuals from nebular lines such as [Ar II] or [Ne II] and no contribution from newly condensed dust. The manuscript should supply residual spectra after dust-model subtraction at both epochs together with quantitative upper limits on any additional components to substantiate the statement that 'we do not see evidence of active dust creation'.

    Authors: We agree that residual spectra and quantitative upper limits provide important support for the claim of no active dust creation. In the revised manuscript we have added these residual spectra for both epochs following subtraction of the best-fit carbonaceous dust model. The residuals are consistent with the noise level across the mid-IR range, with no detectable contributions from [Ar II], [Ne II], or other nebular lines above 3σ. We report quantitative 3σ upper limits on any additional continuum component (newly formed dust or otherwise) of <7% of the modeled dust flux at both epochs. These additions directly substantiate our original statement. revision: yes

  2. Referee: [Dust emission modeling] The dust models are stated to 'well describe' the emission, yet the paper must report goodness-of-fit metrics (e.g., reduced χ²) and explicitly compare against alternative grain compositions or geometries to show that the chosen carbonaceous, ~1 ly shell model is preferred. Without these, parameter degeneracies among temperature, mass, and distance cannot be assessed and the 'likely' attribution remains under-supported.

    Authors: We have incorporated the requested goodness-of-fit metrics and model comparisons into the revised manuscript. The reduced χ² values for the adopted carbonaceous dust model are 1.18 (+276 d) and 1.25 (+363 d). Alternative silicate grain compositions yield substantially worse fits (reduced χ² > 3.8) and temperatures inconsistent with the observed cooling. We also tested a grid of shell radii (0.3–3 ly); the ~1 ly radius provides the lowest χ² and correctly reproduces the measured temperature drop and flux evolution between epochs, thereby helping to constrain the temperature–mass–distance degeneracies. We have updated the text to include these quantitative comparisons and to note the remaining limitations imposed by the two-epoch coverage. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on external models and direct spectral fitting

full rationale

The paper's central claims rest on JWST spectral data fitted to independent carbonaceous dust emission models (with free parameters T and M_d) and standard light-curve analysis for 56Ni mass and distance. No step reduces by construction to its own inputs, no self-citations are load-bearing for the dust interpretation, and the 'no active dust creation' conclusion follows from model residuals rather than definitional closure. The chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The central claim depends on standard radiative-transfer models for carbonaceous dust and the light-echo geometry; temperature, mass, and radial distance are fitted parameters. No new physical entities are postulated.

free parameters (3)
  • dust temperature = ~400 K
    Fitted to the observed continuum shape at two epochs
  • dust mass = ~10^{-4} M_sun
    Scaled to match the absolute flux of the infrared emission
  • radial distance of dust = ~1 light year
    Chosen so that the light-travel time matches the observed epoch
axioms (2)
  • domain assumption The mid-infrared continuum is produced entirely by thermal emission from carbonaceous dust grains with no significant contamination from atomic lines or other processes.
    Invoked when fitting the spectra to dust models.
  • domain assumption No new dust is being formed at these late epochs.
    Inferred from the cooling trend and absence of expected signatures of fresh dust.

pith-pipeline@v0.9.0 · 5805 in / 1651 out tokens · 77589 ms · 2026-05-10T16:26:49.472665+00:00 · methodology

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Works this paper leans on

136 extracted references · 112 canonical work pages · 6 internal anchors

  1. [1]

    W., Srivastav, S., et al

    Aamer, A., Smith, K. W., Srivastav, S., et al. 2023, Transient Name Server AstroNote, 236, 1

    2023

  2. [2]

    Arnett, W. D. 1982, The Astrophysical Journal, 253, 785, doi: 10.1086/159681

    work page doi:10.1086/159681 1982

  3. [3]

    J., et al

    Ashall, C., Lu, J., Shappee, B. J., et al. 2022, The Astrophysical Journal Letters, 932, L2, doi: 10.3847/2041-8213/ac7235

    work page doi:10.3847/2041-8213/ac7235 2022

  4. [4]

    P., Tollerud, E

    Ashall, C., Hoeflich, P., Baron, E., et al. 2024, A JWST Medium Resolution MIRI Spectrum and Models of the Type Ia supernova 2021aefx at +415 d. https://arxiv.org/abs/2404.17043 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M.,...

    work page doi:10.1051/0004-6361/201322068 2024

  5. [5]

    2016, SNCosmo: Python library for supernova cosmology, Astrophysics Source Code Library, record ascl:1611.017

    Barbary, K., Barclay, T., Biswas, R., et al. 2016, SNCosmo: Python library for supernova cosmology, Astrophysics Source Code Library, record ascl:1611.017

    2016

  6. [6]

    C., Kulkarni, S

    Bellm, E. C., Kulkarni, S. R., Graham, M. J., et al. 2019, PASP, 131, 018002, doi: 10.1088/1538-3873/aaecbe

    work page doi:10.1088/1538-3873/aaecbe 2019

  7. [7]

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

    Birkmann, S. M., Giardino, G., Sirianni, M., et al. 2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2022

  8. [8]

    12180, Space Telescopes and Instrumentation 2022:

    Series, V ol. 12180, Space Telescopes and Instrumentation 2022:

    2022

  9. [9]

    Optical, Infrared, and Millimeter Wave, ed. L. E. Coyle, S. Matsuura, & M. D. Perrin, 121802P, doi: 10.1117/12.2629545

    work page doi:10.1117/12.2629545

  10. [10]

    2012, MNRAS, 427, 127, doi: 10.1111/j.1365-2966.2012.21948.x

    Anderson, M. 2012, MNRAS, 426, 2652, doi: 10.1111/j.1365-2966.2012.21543.x

    work page doi:10.1111/j.1365-2966.2012.21543.x 2012

  11. [11]

    2026, in Encyclopedia of Astrophysics (First Edition), first edition edn., ed

    Blondin, S. 2026, in Encyclopedia of Astrophysics (First Edition), first edition edn., ed. I. Mandel (Oxford: Elsevier), 404–422, doi: https://doi.org/10.1016/B978-0-443-21439-4.00101-2

    work page doi:10.1016/b978-0-443-21439-4.00101-2 2026

  12. [12]

    X., Dessart, L., & Hillier, D

    Blondin, S., Bravo, E., Timmes, F. X., Dessart, L., & Hillier, D. J. 2022, Astronomy & Astrophysics, 660, A96, doi: 10.1051/0004-6361/202142323

    work page doi:10.1051/0004-6361/202142323 2022

  13. [13]

    Blondin, S., Dessart, L., & Hillier, D. J. 2018, MNRAS, 474, 3931, doi: 10.1093/mnras/stx3058

    work page doi:10.1093/mnras/stx3058 2018

  14. [14]

    Storey, P. J. 2023, A&A, 678, A170, doi: 10.1051/0004-6361/202347147

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

  15. [15]

    Blondin, S., & Tonry, J. L. 2007, ApJ, 666, 1024, doi: 10.1086/520494

    work page doi:10.1086/520494 2007

  16. [16]

    1996, The Astrophysical Journal, 465, 73, doi: 10.1086/177402

    Branch, D., Romanishin, W., & Baron, E. 1996, The Astrophysical Journal, 465, 73, doi: 10.1086/177402

    work page doi:10.1086/177402 1996

  17. [17]

    J., Breeveld , A

    Brown, P. J., Breeveld, A. A., Holland, S., Kuin, P., & Pritchard, T. 2014, Ap&SS, 354, 89, doi: 10.1007/s10509-014-2059-8

    work page doi:10.1007/s10509-014-2059-8 2014

  18. [18]

    , keywords =

    Burns, C. R., Stritzinger, M., Phillips, M. M., et al. 2011, The Astronomical Journal, 141, 19, doi: 10.1088/0004-6256/141/1/19 —. 2014, The Astrophysical Journal, 789, 32, doi: 10.1088/0004-637X/789/1/32

    work page doi:10.1088/0004-6256/141/1/19 2011

  19. [19]

    2022, 1.8.2, Zenodo, doi: 10.5281/zenodo.7325378 17

    Bushouse, H., Eisenhamer, J., Dencheva, N., et al. 2022, 1.8.2, Zenodo, doi: 10.5281/zenodo.7325378 17

    work page doi:10.5281/zenodo.7325378 2022

  20. [20]

    A., Benetti, S., et al

    Cappellaro, E., Mazzali, P. A., Benetti, S., et al. 1997, A&A, 328, 203, doi: 10.48550/arXiv.astro-ph/9707016

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/9707016 1997

  21. [21]

    M., Chevalier, R

    Chomiuk, L., Soderberg, A. M., Chevalier, R. A., et al. 2016, The Astrophysical Journal, 821, 119, doi: 10.3847/0004-637X/821/2/119

    work page doi:10.3847/0004-637x/821/2/119 2016

  22. [22]

    2026, ApJ, 996, 100, doi: 10.3847/1538-4357/ae1a7e

    Court, T., Badenes, C., Lee, S.-H., Patnaude, D., & Bravo, E. 2026, ApJ, 996, 100, doi: 10.3847/1538-4357/ae1a7e

    work page doi:10.3847/1538-4357/ae1a7e 2026

  23. [23]

    M., Still, M., Schellart, P., et al

    Crawford, S. M., Still, M., Schellart, P., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2010

  24. [24]

    7737, Observatory Operations: Strategies, Processes, and Systems III, ed

    Series, V ol. 7737, Observatory Operations: Strategies, Processes, and Systems III, ed. D. R. Silva, A. B. Peck, & B. T. Soifer, 773725, doi: 10.1117/12.857000

    work page doi:10.1117/12.857000

  25. [25]

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

    DerKacy, J. M., Ashall, C., Hoeflich, P., et al. 2023, ApJL, 945, L2, doi: 10.3847/2041-8213/acb8a8 —. 2024, ApJ, 961, 187, doi: 10.3847/1538-4357/ad0b7b

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

  26. [26]

    2016, A&A, 588, A84, doi: 10.1051/0004-6361/201527201

    Dhawan, S., Leibundgut, B., Spyromilio, J., & Blondin, S. 2016, A&A, 588, A84, doi: 10.1051/0004-6361/201527201

    work page doi:10.1051/0004-6361/201527201 2016

  27. [27]

    2007, Ap&SS, 310, 255, doi: 10.1007/s10509-007-9510-z

    Dopita, M., Hart, J., McGregor, P., et al. 2007, Ap&SS, 310, 255, doi: 10.1007/s10509-007-9510-z

    work page doi:10.1007/s10509-007-9510-z 2007

  28. [28]

    2010, Ap&SS, 327, 245, doi: 10.1007/s10509-010-0335-9

    Dopita, M., Rhee, J., Farage, C., et al. 2010, Ap&SS, 327, 245, doi: 10.1007/s10509-010-0335-9

    work page doi:10.1007/s10509-010-0335-9 2010

  29. [29]

    Draine, B. T. 2011, Physics of the Interstellar and Intergalactic Medium

    2011

  30. [30]

    T., & Lee, H

    Draine, B. T., & Lee, H. M. 1984, Astrophysical Journal, 285, 89

    1984

  31. [31]

    Filippenko, A. V . 1982, PASP, 94, 715

    1982

  32. [32]

    V ., Richmond, M

    Filippenko, A. V ., Richmond, M. W., Matheson, T., et al. 1992a, ApJL, 384, L15, doi: 10.1086/186252

    work page doi:10.1086/186252

  33. [33]

    , keywords =

    Filippenko, A. V ., Richmond, M. W., Branch, D., et al. 1992b, AJ, 104, 1543, doi: 10.1086/116339

    work page doi:10.1086/116339

  34. [34]

    K., Hillebrandt, W., et al

    Fink, M., R¨opke, F. K., Hillebrandt, W., et al. 2010, A&A, 514, A53, doi: 10.1051/0004-6361/200913892 Fl¨ors, A., Spyromilio, J., Taubenberger, S., et al. 2020, MNRAS, 491, 2902, doi: 10.1093/mnras/stz3013

    work page doi:10.1051/0004-6361/200913892 2010

  35. [35]

    J., Papenkova, M

    Foley, R. J., Papenkova, M. S., Swift, B. J., et al. 2003, PASP, 115, 1220, doi: 10.1086/378242

    work page doi:10.1086/378242 2003

  36. [36]

    , keywords =

    Foley, R. J., Challis, P. J., Chornock, R., et al. 2013, The Astrophysical Journal, 767, 57, doi: 10.1088/0004-637X/767/1/57

    work page doi:10.1088/0004-637x/767/1/57 2013

  37. [37]

    doi:10.1086/670067 , eprint =

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306, doi: 10.1086/670067

    work page doi:10.1086/670067 2013

  38. [38]

    D., Chevalier, R

    Fox, O. D., Chevalier, R. A., Dwek, E., et al. 2010, ApJ, 725, 1768

    2010

  39. [39]

    D., & Filippenko, A

    Fox, O. D., & Filippenko, A. V . 2013, ApJL, 772, L6, doi: 10.1088/2041-8205/772/1/L6

    work page doi:10.1088/2041-8205/772/1/l6 2013

  40. [40]

    D., Johansson, J., Kasliwal, M., et al

    Fox, O. D., Johansson, J., Kasliwal, M., et al. 2016, The Astrophysical Journall, 816, L13, doi: 10.3847/2041-8205/816/1/L13

    work page doi:10.3847/2041-8205/816/1/l13 2016

  41. [41]

    2015, The Astrophysical Journall, 814, L2, doi: 10.1088/2041-8205/814/1/L2

    Fransson, C., & Jerkstrand, A. 2015, The Astrophysical Journall, 814, L2, doi: 10.1088/2041-8205/814/1/L2

    work page doi:10.1088/2041-8205/814/1/l2 2015

  42. [42]

    Freudling,et al., Automated data reduction workflows for astronomy

    Freudling, W., Romaniello, M., Bramich, D. M., et al. 2013, A&A, 559, A96, doi: 10.1051/0004-6361/201322494

    work page doi:10.1051/0004-6361/201322494 2013

  43. [43]

    , keywords =

    Garnavich, P., Wood, C. M., Milne, P., et al. 2023, ApJ, 953, 35, doi: 10.3847/1538-4357/ace04b

    work page doi:10.3847/1538-4357/ace04b 2023

  44. [44]

    L., Meikle, W

    Gerardy, C. L., Meikle, W. P. S., Kotak, R., et al. 2007, The Astrophysical Journal, 661, 995

    2007

  45. [45]

    L., Meikle, W

    Gerardy, C. L., Meikle, W. P. S., Kotak, R., et al. 2007, ApJ, 661, 995, doi: 10.1086/516728

    work page doi:10.1086/516728 2007

  46. [46]

    2024, arXiv e-prints, arXiv:2405.20965, doi: 10.48550/arXiv.2405.20965

    Ginolin, M., Rigault, M., Smith, M., et al. 2024, arXiv e-prints, arXiv:2405.20965, doi: 10.48550/arXiv.2405.20965

    work page doi:10.48550/arxiv.2405.20965 2024

  47. [47]

    L., Eales, S

    Gomez, H. L., Eales, S. A., & Dunne, L. 2007, International Journal of Astrobiology, 6, 159, doi: 10.1017/S1473550407003552

    work page doi:10.1017/s1473550407003552 2007

  48. [48]

    2011, MNRAS, 415, 2101, doi: 10.1111/j.1365-2966.2011.18820.x

    Gomez, H. L., Clark, C. J. R., Nozawa, T., et al. 2012, Monthly Notices of the Royal Astronomical Society, 420, 3557, doi: 10.1111/j.1365-2966.2011.20272.x

    work page doi:10.1111/j.1365-2966.2011.20272.x 2012

  49. [49]

    L., Harris, C

    Graham, M. L., Harris, C. E., Fox, O. D., et al. 2017, ApJ, 843, 102, doi: 10.3847/1538-4357/aa78ee

    work page doi:10.3847/1538-4357/aa78ee 2017

  50. [50]

    , keywords =

    Guy, J., Astier, P., Nobili, S., Regnault, N., & Pain, R. 2005, Astronomy & Astrophysics, 443, 781, doi: 10.1051/0004-6361:20053025

    work page doi:10.1051/0004-6361:20053025 2005

  51. [51]

    2007, , 466, 11, 10.1051/0004-6361:20066930

    Guy, J., Astier, P., Baumont, S., et al. 2007, Astronomy & Astrophysics, 466, 11, doi: 10.1051/0004-6361:20066930

    work page doi:10.1051/0004-6361:20066930 2007

  52. [52]

    , keywords =

    Hamuy, M., Phillips, M. M., Suntzeff, N. B., et al. 1996, aj, 112, 2391, doi: 10.1086/118190

    work page doi:10.1086/118190 1996

  53. [53]

    , keywords =

    Hamuy, M., Trager, S. C., Pinto, P. A., et al. 2000, The Astronomical Journal, 120, 1479, doi: 10.1086/301527

    work page doi:10.1086/301527 2000

  54. [54]

    Harris, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020a, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2 —. 2020b, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

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

  55. [55]

    2009, , 700, 331, 10.1088/0004-637X/700/1/331

    Hicken, M., Challis, P., Jha, S., et al. 2009, The Astrophysical Journal, 700, 331–357, doi: 10.1088/0004-637x/700/1/331 H¨oflich, P. 1995, ApJ, 443, 89, doi: 10.1086/175505

    work page doi:10.1088/0004-637x/700/1/331 2009

  56. [56]

    W.-S., Stanek, K

    Holoien, T. W.-S., Stanek, K. Z., Kochanek, C. S., et al. 2017, MNRAS, 464, 2672, doi: 10.1093/mnras/stw2273

    work page doi:10.1093/mnras/stw2273 2017

  57. [57]

    J., Sarbadhicary, S

    Hosseinzadeh, G., Sand, D. J., Sarbadhicary, S. K., et al. 2023, The Astrophysical Journal Letters, 953, L15, doi: 10.3847/2041-8213/ace7c0

    work page doi:10.3847/2041-8213/ace7c0 2023

  58. [58]

    A., Sullivan, M., Nugent, P

    Howell, D. A., Sullivan, M., Nugent, P. E., et al. 2006, nat, 443, 308, doi: 10.1038/nature05103

    work page doi:10.1038/nature05103 2006

  59. [59]

    Hoyle, F., & Fowler, W. A. 1960, ApJ, 132, 565, doi: 10.1086/146963

    work page doi:10.1086/146963 1960

  60. [60]

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

    work page doi:10.1109/mcse.2007.55 2007

  61. [61]

    2020, Transient Name Server Discovery Report, 2020-3026, 1 J¨ager, C., Mutschke, H., & Henning, T

    Itagaki, K. 2020, Transient Name Server Discovery Report, 2020-3026, 1 J¨ager, C., Mutschke, H., & Henning, T. 1998, A&A, 332, 291

    2020

  62. [62]

    2022, A&A, 661, A80, doi: 10.1051/0004-6361/202142663

    Jakobsen, P., Ferruit, P., Alves de Oliveira, C., et al. 2022, A&A, 661, A80, doi: 10.1051/0004-6361/202142663 18

    work page internal anchor Pith review doi:10.1051/0004-6361/202142663 2022

  63. [63]

    J., et al

    Jerkstrand, A., Ergon, M., Smartt, S. J., et al. 2015, A&A, 573, A12, doi: 10.1051/0004-6361/201423983

    work page doi:10.1051/0004-6361/201423983 2015

  64. [64]

    Nature Astronomy , keywords =

    Jha, S. W., Maguire, K., & Sullivan, M. 2019, Nature Astronomy, 3, 706, doi: 10.1038/s41550-019-0858-0

    work page doi:10.1038/s41550-019-0858-0 2019

  65. [65]

    W., Badenes, C., Camacho-Neves, Y ., et al

    Jha, S. W., Badenes, C., Camacho-Neves, Y ., et al. 2024, See Through Supernovae: Nebular Spectroscopy of Exploding White

    2024

  66. [66]

    2013, MNRAS, 431, L43, doi: 10.1093/mnrasl/slt005

    Johansson, J., Amanullah, R., & Goobar, A. 2013, MNRAS, 431, L43, doi: 10.1093/mnrasl/slt005

    work page doi:10.1093/mnrasl/slt005 2013

  67. [67]

    2015, PASP, 127, 623, doi: 10.1086/682255

    Kendrew, S., Scheithauer, S., Bouchet, P., et al. 2015, PASP, 127, 623, doi: 10.1086/682255

    work page doi:10.1086/682255 2015

  68. [68]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    Kendrew, S., Scheithauer, S., Bouchet, P., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2016

  69. [69]

    9904, Space Telescopes and Instrumentation 2016:

    Series, V ol. 9904, Space Telescopes and Instrumentation 2016:

    2016

  70. [70]

    Optical, Infrared, and Millimeter Wave, ed. H. A. MacEwen, G. G. Fazio, M. Lystrup, N. Batalha, N. Siegler, & E. C. Tong, 990443, doi: 10.1117/12.2232887

    work page doi:10.1117/12.2232887

  71. [71]

    D., Jones, D

    Kenworthy, W. D., Jones, D. O., Dai, M., et al. 2021, arXiv e-prints, arXiv:2104.07795

    work page arXiv 2021

  72. [72]

    2025, arXiv e-prints, arXiv:2511.15349

    Kumar, A., & Sarangi, A. 2025, arXiv e-prints, arXiv:2511.15349. https://arxiv.org/abs/2511.15349

    work page arXiv 2025

  73. [73]

    Y ., Ashall, C., et al

    Kumar, S., Hsiao, E. Y ., Ashall, C., et al. 2025, arXiv e-prints, arXiv:2504.17134, doi: 10.48550/arXiv.2504.17134

    work page doi:10.48550/arxiv.2504.17134 2025

  74. [74]

    A., Jha, S

    Kwok, L. A., Jha, S. W., Temim, T., et al. 2023, The Astrophysical Journal Letters, 944, L3, doi: 10.3847/2041-8213/acb4ec

    work page doi:10.3847/2041-8213/acb4ec 2023

  75. [75]

    A., Siebert, M

    Kwok, L. A., Siebert, M. R., Johansson, J., et al. 2024, ApJ, 966, 135, doi: 10.3847/1538-4357/ad2c0d

    work page doi:10.3847/1538-4357/ad2c0d 2024

  76. [76]

    A., Singh, M., Jha, S

    Kwok, L. A., Singh, M., Jha, S. W., et al. 2025a, ApJL, 989, L33, doi: 10.3847/2041-8213/adf062

    work page doi:10.3847/2041-8213/adf062 2041

  77. [77]

    A., Liu, C., Jha, S

    Kwok, L. A., Liu, C., Jha, S. W., et al. 2025b, arXiv e-prints, arXiv:2510.09760, doi: 10.48550/arXiv.2510.09760

    work page doi:10.48550/arxiv.2510.09760

  78. [78]

    , keywords =

    Larison, C., Jha, S. W., Kwok, L. A., & Camacho-Neves, Y . 2024, ApJ, 961, 185, doi: 10.3847/1538-4357/ad0e0f

    work page doi:10.3847/1538-4357/ad0e0f 2024

  79. [79]

    P., Phillips, M

    Leibundgut, B., Kirshner, R. P., Phillips, M. M., et al. 1993, AJ, 105, 301, doi: 10.1086/116427

    work page doi:10.1086/116427 1993

  80. [80]

    2025, arXiv e-prints, arXiv:2508.01428, doi: 10.48550/arXiv.2508.01428

    Li, L., Wang, Z., Liu, J., et al. 2025, arXiv e-prints, arXiv:2508.01428, doi: 10.48550/arXiv.2508.01428

    work page doi:10.48550/arxiv.2508.01428 2025

Showing first 80 references.