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arxiv: 2606.00208 · v1 · pith:P6PLEEXSnew · submitted 2026-05-29 · 🌌 astro-ph.HE · astro-ph.GA· astro-ph.SR

JWST Reveals Large Reservoirs of Dust and Ongoing Circumstellar Interaction in SN Ibn/Icn 2023xgo over a Year Post-Explosion

Kyle W. Davis , Kirsty Taggart , Samaporn Tinyanont , Ryan J. Foley , Jeonghee Rho , Katie Auchettl , Diego Farias , Ori D. Fox
show 18 more authors
Joel Johansson Charles D. Kilpatrick Kishore C. Patra Craig Pellegrino Enrico Ramirez-Ruiz David A. Coulter Yize Dong Alexander T. Gagliano T. R. Geballe Wynn V. Jacobson-Gal\'an Jenna Karcheski Ravjit Kaur Ryan M. Lau Thomas Moore Seong Hyun Park Armin Rest Tam\'as Szalai Qinan Wang
This is my paper

Pith reviewed 2026-06-28 21:16 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GAastro-ph.SR
keywords supernovadust formationJWSTcircumstellar mediumType Ibninfrared spectroscopySN 2023xgoshock interaction
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The pith

JWST observations of SN 2023xgo show at least 0.03 solar masses of cool silicate dust at the shock radius plus ongoing circumstellar interaction at 377 days post-explosion.

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

The paper reports JWST infrared photometry and spectroscopy of the nearby Type Ibn/Icn supernova 2023xgo out to 377 days after explosion. The late-time spectrum matches thermal emission from cool silicate dust at 300-600 K with mass at least 0.03 solar masses located at a radius matching the forward shock, plus a smaller amount of carbonaceous dust. Narrow blueshifted He I emission at 2.06 microns indicates the shock is still running into helium-rich circumstellar material shed by the progenitor. Earlier Gemini and WISE data at 70-100 days already show hot dust, and the lack of molecular lines together with changing optical line profiles point to rapid interior dust formation. These results indicate that the dense, hydrogen-poor environments of SNe Ibn/Icn enable substantial dust production both before and after core collapse.

Core claim

At +377 days, the JWST spectrum is consistent with emission from cool (~300-600 K) silicate dust with M ≳ 3 × 10^{-2} M⊙ at a radius similar to the shock radius (2.3 × 10^{16} cm), and we detect narrow (FWHM = 520+/-130 km s^{-1}) He I λ2.06 micron emission blueshifted by 340+/-40 km s^{-1}, indicating the SN shock continues to encounter circumstellar material. The large dust mass and rapid onset of dust formation observed in SN 2023xgo show that the unique physical environments of SNe Ibn/Icn facilitate substantial dust formation both before and after the SN.

What carries the argument

The +377-day JWST NIRSpec/MIRI spectrum modeled as thermal emission from silicate and carbonaceous dust grains combined with the narrow He I 2.06 micron line profile that tracks ongoing shock-CSM interaction.

If this is right

  • SNe Ibn/Icn can produce total dust masses exceeding 0.03 solar masses within the first year.
  • Dust formation begins rapidly, already detectable at 70 days, and continues at large radii matching the shock front.
  • Circumstellar interaction with He/C-rich material persists at least to 377 days, traced by narrow blueshifted He I emission.
  • The environments of hydrogen-poor interacting supernovae are efficient sites for both pre-explosion and post-explosion dust production.

Where Pith is reading between the lines

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

  • Similar late-time JWST observations of other rare Ibn/Icn events could reveal whether large dust reservoirs are common in this subclass.
  • If the dust mass scaling holds for higher-redshift analogs, these events may contribute measurably to cosmic dust budgets at early epochs.
  • The blueshifted He I line offers a direct kinematic probe of the unshocked CSM velocity that can be compared with progenitor wind models.

Load-bearing premise

The observed mid-infrared flux and spectrum at late times arise primarily from thermal radiation by dust grains at the quoted temperatures and masses rather than from free-free, synchrotron, or other continuum processes.

What would settle it

A +377-day spectrum or photometry that shows infrared flux levels and spectral shape matching only the expected supernova continuum without requiring an additional 300-600 K blackbody component of the reported mass and radius.

Figures

Figures reproduced from arXiv: 2606.00208 by Alexander T. Gagliano, Armin Rest, Charles D. Kilpatrick, Craig Pellegrino, David A. Coulter, Diego Farias, Enrico Ramirez-Ruiz, Jenna Karcheski, Jeonghee Rho, Joel Johansson, Katie Auchettl, Kirsty Taggart, Kishore C. Patra, Kyle W. Davis, Ori D. Fox, Qinan Wang, Ravjit Kaur, Ryan J. Foley, Ryan M. Lau, Samaporn Tinyanont, Seong Hyun Park, Tam\'as Szalai, Thomas Moore, T. R. Geballe, Wynn V. Jacobson-Gal\'an, Yize Dong.

Figure 1
Figure 1. Figure 1: Composite color cutout image of SN 2023xgo at +377 days post-explosion from MIRI images. F1280W, F1500W, F1800W, and F2100W filters are assigned to each color channel. We show a field-of-view of 40-by-40′′, with a 2- by-2′′ cutout of the SN inset in the upper-right. SN 2023xgo is clearly detected. The host galaxy is seen trailing to the lower-right of the SN, and we expect minimal emission from the host at… view at source ↗
Figure 2
Figure 2. Figure 2: Full SED of 2023xgo from JWST observations at +377 days post-explosion. The NIRSpec G235M and G395M spectra are shown in blue and orange respectively and additionally in the two lower panels. MIRI LRS data are shown in green. MIRI imaging data are shown in pink diamonds. The flux calibration is taken directly from the data reduction pipeline, and we show the data without any other normalizations. its host … view at source ↗
Figure 3
Figure 3. Figure 3: SED fits for six dust emission models used in our analysis. Results are presented in [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Best-fit optically thin dust models to Gemini and WISE observations of SN 2023xgo at +101 days post￾explosion. Carbonaceous dust model is shown in blue, while silicate dust model is shown in orange. We obtain the dust temperature by fitting the GNIRS spectrum independent of the WISE photometry. We then determine a dust mass by scaling the dust SED to the WISE observations (with the assumption that the dust… view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of He I line profiles in velocity space relative to the rest frame of the host galaxy. The gray ver￾tical dashed line shows 0 km s−1 . By +67 days, the emis￾sion is clearly blueshifted, most likely due to optically thick dust forming interior to the emitting region (e.g. Smith et al. 2008a). By this epoch, the emission lines in both the opti￾cal and NIR show an intermediate-width component extend… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of ∼+1 year NIR spectrum of SN 2023xgo with that of other CCSNe (SN 2006jc, SN 2023ixf, SN 2024ggi Mattila et al. 2008; Medler et al. 2025; Mera et al. 2026). The fluxes are normalized to a common distance, then offset for visual clarity (dashed lines show Fν = 0 for each spectrum). CO fundamental and first overtone emission bands are shown in the grayed-out regions. Unlike the spectra of SN 202… view at source ↗
Figure 8
Figure 8. Figure 8: Detection of narrow emission from He I λ2.06 µm at +377 days post-explosion. We measure a FWHM of 520±130 km s−1 when fitting the line with a Lorentzian after subtracting the local continuum. The measured FWHM is roughly half of that measured from early-time optical spec￾tra of SN 2023xgo (Gangopadhyay et al. 2025). The line is blueshifted by 340±40 km s−1 relative to the rest frame. This could arise from … view at source ↗
Figure 9
Figure 9. Figure 9: Carbonaceous dust temperature at different echo radii given a peak SN luminosity adapted from (Fox et al. 2011). Contours show different peak SN luminosities in units of L⊙, where the parameter space below each represents per￾mitted dust/echo parameters given the input energy. The peak luminosity of SN 2023xgo from Gangopadhyay et al. (2025) is marked in red. The input luminosity is treated as a single pul… view at source ↗
Figure 10
Figure 10. Figure 10: Left: Compilation of observed dust masses versus phase for SNe Ibn/Icn (Mattila et al. 2008; Gan et al. 2021, this paper) compared to several types of CCSNe (Meikle et al. 2007; Gall et al. 2011; Wesson et al. 2015; Gallagher et al. 2012a; Shahbandeh et al. 2023; Gallagher et al. 2012b; Zs´ıros et al. 2024; Shahbandeh et al. 2025; Tinyanont et al. 2025; Pearson et al. 2025; Singh et al. 2026, and referenc… view at source ↗
read the original abstract

We present infrared (IR) photometric and spectroscopic observations of SN 2023xgo, a recent and nearby Type Ibn/Icn supernova (SN Ibn/Icn) which shows shock interaction with a He/C-rich and H-poor circumstellar medium (CSM). Although interacting SNe are predicted to produce large amounts of dust, the rarity of SNe Ibn and Icn has resulted in few opportunities to observe these objects in the IR at late times. Here, we report observations of SN 2023xgo from JWST (NIRSpec and MIRI), WISE, and Gemini taken out to +377 days post-explosion. At +377 days, the JWST spectrum is consistent with both emission from cool (~300-600 K) silicate dust with $M \gtrsim 3 \times 10^{-2}$ M$_{\odot}$ at a radius similar to the shock radius ($2.3 \times 10^{16}$ cm), and optically thin carbonaceous dust with $M = 8 \times 10^{-3}$ M$_{\odot}$. We also detect narrow (FWHM = 520+/-130 km s$^{-1}$) He I $\lambda$2.06 micron emission at +377 days, indicating that the SN shock continues to encounter material shed from the star to this late epoch. The emission line is blueshifted from the rest frame by 340+/-40 km s$^{-1}$. The Gemini and WISE observations at ~70-100 days reveal emission from 6.8$\times$10$^{-5}$ M$_{\odot}$ of hot (~1300 K) dust, which we interpret as a lower limit of the total dust mass at that phase. Molecular gas emission is not detected in any data, though emission line profiles in the optical and NIR taken at ~70 days after explosion show progressively less redshifted emission, attributed to attenuation from dust and suggesting that some dust is rapidly forming interior to the unshocked CSM. The large dust mass and rapid onset of dust formation observed in SN 2023xgo show that the unique physical environments of SNe Ibn/Icn facilitate substantial dust formation both before and after the SN.

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 presents JWST (NIRSpec+MIRI) spectroscopic and photometric observations of the Type Ibn/Icn supernova SN 2023xgo at +377 days post-explosion, supplemented by Gemini and WISE data at ~70-100 days. It claims that the +377 d spectrum is consistent with cool (~300-600 K) silicate dust with mass M ≳ 3×10^{-2} M⊙ at a radius (2.3×10^{16} cm) matching the shock radius, reports an alternative optically thin carbonaceous dust mass of 8×10^{-3} M⊙, and detects narrow (FWHM=520±130 km s^{-1}) blueshifted He I λ2.06 μm emission indicating ongoing CSM interaction. Earlier epochs show hot (~1300 K) dust at lower mass, with no molecular gas detected; the work concludes that SNe Ibn/Icn enable rapid, substantial dust formation both before and after explosion.

Significance. If the dust-mass and interaction results hold, the paper supplies rare late-time IR constraints on dust production in the uncommon Ibn/Icn subclass, with potential relevance to dust budgets in core-collapse events and early-universe enrichment. The direct spectroscopic evidence for continued shock-CSM interaction at +377 d and the JWST-enabled detection of cool dust at radii comparable to the forward shock constitute concrete observational anchors for models of dust formation in dense, He/C-rich environments.

major comments (1)
  1. [Abstract] Abstract (and the +377 d JWST spectral modeling section): the headline dust mass M ≳ 3×10^{-2} M⊙ is obtained by fitting the observed continuum to a cool silicate thermal-emission model. No quantitative upper limits or joint fits are supplied to demonstrate that non-dust continuum sources (free-free from the interaction zone, residual synchrotron, or unmodeled line wings) remain negligible across the fitted wavelength range; this assumption directly controls the conversion from flux to mass and radius.
minor comments (1)
  1. [Abstract] The abstract states the spectrum is 'consistent with both' silicate and carbonaceous dust but does not clarify whether these are mutually exclusive models or whether a two-component fit was performed.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful and constructive review. We address the single major comment below and have revised the manuscript to incorporate additional quantitative checks on the continuum modeling.

read point-by-point responses

  1. Referee: [Abstract] Abstract (and the +377 d JWST spectral modeling section): the headline dust mass M ≳ 3×10^{-2} M⊙ is obtained by fitting the observed continuum to a cool silicate thermal-emission model. No quantitative upper limits or joint fits are supplied to demonstrate that non-dust continuum sources (free-free from the interaction zone, residual synchrotron, or unmodeled line wings) remain negligible across the fitted wavelength range; this assumption directly controls the conversion from flux to mass and radius.

    Authors: We agree that explicit quantification of possible non-dust contributions is necessary to robustly support the reported dust masses. In the revised manuscript we have added a dedicated paragraph to the +377 d spectral modeling section that (i) places an upper limit on free-free emission by scaling from the observed narrow He I λ2.06 μm luminosity and an assumed post-shock density consistent with the line width, finding <8% contribution longward of 5 μm; (ii) notes the lack of any radio detection that would indicate significant synchrotron; and (iii) demonstrates that the observed line profiles lack broad wings capable of affecting the continuum fit at the 5% level. These limits are now referenced in the abstract. The dust-mass and radius values themselves are unchanged, but the modeling assumptions are now stated with the requested quantitative support. revision: yes

Circularity Check

0 steps flagged

No circularity; results are direct model fits to new JWST data

full rationale

The paper reports new JWST NIRSpec+MIRI spectra and photometry of SN 2023xgo at +377 days, then fits these observed fluxes to standard cool silicate and carbonaceous dust emission models to obtain M_dust, T, and radius. These are conventional forward-model fits to external telescope data against calibrated flux standards; the output dust mass is not an input, nor is any quantity renamed or predicted from a prior fit within the same dataset. No equations, uniqueness theorems, or ansatzes are imported via self-citation in a load-bearing way. The derivation chain is therefore self-contained and non-circular.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The work is purely observational; no new theoretical free parameters, axioms, or invented entities are introduced beyond standard assumptions of thermal dust emission and line identification used in supernova infrared analysis.

pith-pipeline@v0.9.1-grok · 6088 in / 1375 out tokens · 25178 ms · 2026-06-28T21:16:12.851555+00:00 · methodology

discussion (0)

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