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The Progenitor of the Type II-Plateau SN 2025pht in NGC 1637: The Dustiest, Most Luminous Red Supergiant So Far?

T0 review · 3 major / 4 minor · reviewed 2026-08-03 · deepseek-v4-flash

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Pith's one-line read A dust-enshrouded red supergiant may be the most luminous SN II-P progenitor yet found.

desk verdict A credible dusty-RSG identification with JWST data that overreaches on the 'most luminous' claim; the distance anchor is internally inconsistent and the extreme values should be read as model-dependent. read the letter →

arxiv 2601.09087 v2 pith:KZJKCDLB submitted 2026-01-14 astro-ph.SR astro-ph.HE

Schuyler D. Van Dyk , Tamas Szalai , Gagandeep S. Anand , Thomas G. Brink , Noah Zimmer , Dan Milisavljevic , Ori D. Fox , Jacob E. Jencson
show 9 more authors
WeiKang Zheng Alexei V. Filippenko Lukasz Wyrzykowski Przemyslaw J. Mikolajczyk Krzysztof Kotysz F.-J. Hambsch Agata Wozniak Michal Zejmo Andrea Reguitti
This is my paper · ORCID
classification astro-ph.SRastro-ph.HE
keywords TypeII-PsupernovaeredsupergiantprogenitorscircumstellardustSN2025phtNGC1637JWSTDUSTYradiativetransferlong-periodvariables
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that the star that exploded as SN 2025pht was a red supergiant (RSG) hidden behind a thick, silicate-rich circumstellar dust shell. Using JWST observations from February and October 2024 — the latter only about eight months before the presumed explosion — the authors reconstruct the star's spectral energy distribution and infer a bolometric luminosity of log(L/Lsun)=5.08±0.16 and a photospheric temperature around 2100–2500 K. If correct, this makes the candidate among the most luminous, and perhaps the dustiest, RSG progenitors ever identified for a Type II-plateau supernova, sitting near the empirical upper luminosity boundary for such progenitors. The result matters because it tests the 'RSG problem' — the apparent shortage of very luminous RSG progenitors — and shows that JWST is needed to find the most heavily obscured progenitors at all.

What carries the argument

The argument rests on a 'quasi-snapshot' of the candidate: JWST observations taken 510 and 264 days before discovery, spanning roughly 1.5–7.7 microns, which define the spectral energy distribution. The central object is a spherical, silicate-rich circumstellar dust shell, modeled with the DUSTY radiative-transfer code; the free parameters (photospheric temperature T_phot, inner-shell temperature T(R_in), and dust optical depth tau_V) are fit to the observed SED. The model converts the reddened infrared fluxes into a bolometric luminosity and yields a mass-loss rate of roughly 4.8e-5 solar masses per year. A simple sinusoid fit to the 2001 HST F814W variability, together with the JWST photom

What would settle it

A deep JWST image of the site taken a few years after explosion showing a point source with brightness comparable to the 2024 pre-explosion values would falsify the progenitor identification. Alternatively, a Cepheid or TRGB distance to NGC 1637 near 9 Mpc would lower the inferred luminosity to log L ≈ 4.9, making the 'most luminous' claim untenable.

Watch

Extended reading notes

Core claim

The central claim is that the pre-explosion source at the position of SN 2025pht was a luminous, heavily dust-enshrouded red supergiant. The star was detected in HST F814W images from 2001 and, 23 years later, in more than a dozen JWST NIRCam and MIRI bands; it was not detected in any optical band in 2024. After correcting for foreground and host-galaxy extinction (A_V(host)~1.7 mag) and using DUSTY radiative-transfer models of a silicate dust shell, the authors find a bolometric luminosity log(L_bol/L_sun)=5.08±0.16, an effective temperature of 2100–2500 K, and approximately 7.6 mag of circumstellar visual extinction. They conclude that the star is highly likely to have been a luminous RSG

Load-bearing premise

The adopted distance to NGC 1637 (10.73±1.76 Mpc) is a weighted mean of widely discordant estimates spanning 7.5–13.9 Mpc; because every luminosity, radius, and mass-loss value scales as distance squared, a true distance near the low end would erase the record-setting luminosity claim.

Editorial extensions

If this is right

  • If the candidate is confirmed, SN II-P progenitors can be as luminous as log L ~ 5.1–5.2, pushing against the upper bound set by the 'RSG problem'.
  • Obscured progenitors like this one would be systematically missed by optical-only pre-explosion searches, so the bright, dusty end of the RSG progenitor luminosity distribution may be incomplete.
  • The high circumstellar extinction (~7.6 mag) implies substantial recent mass loss, consistent with the short-plateau nature of SN 2025pht and with possible late-time CSM interaction.
  • The inferred period-luminosity agreement favors a ~660-day pulsation period, which, if real, links the progenitor to the long-period-variable RSG population.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the true distance to NGC 1637 is near the low end of the published range (~7.5 Mpc), the luminosity would drop by ~0.3 dex and the candidate would be unexceptional; a definitive TRGB distance would settle this.
  • The same SED-fitting approach, applied to archival JWST data of other nearby galaxies, could reveal a population of optically invisible RSG progenitors and revise the empirical upper luminosity limit.
  • The paper's abstract and body quote different distances (11.67 vs 10.73 Mpc) and different best-fit luminosities (5.16 vs 5.08), so reconciling the adopted distance is a simple internal consistency check.
  • Future JWST observations could test whether the star is genuinely gone, but if late-time CSM interaction produces infrared excess, the disappearance may be masked; a color- or position-based test would be more discriminating.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper characterizes the likely progenitor candidate of Type II-plateau SN 2025pht in NGC 1637 using HST WFPC2 images from 2001 and JWST NIRCam/MIRI imaging from 2024. The candidate is detected only in the near/mid-infrared and is undetected in optical HST bands. The authors construct a reddening- and distance-corrected SED, fit it with DUSTY radiative-transfer models of a dusty circumstellar shell, and infer T_eff = 2100–2500 K, log(L_bol/L_sun) = 5.08 ± 0.16, A_V(CSM) ≈ 7.6 mag, a mass-loss rate ≈ 4.8×10^-5 M_sun/yr, and a possible long-period variability of ~660 days. They conclude that the star was a highly luminous, dusty RSG, possibly the most luminous SN II-P progenitor candidate known to date.

Significance. If the quantitative extremes hold, this object is a crucial addition to the small sample of directly imaged SN II-P progenitors, probing the upper luminosity boundary of the 'RSG problem' and demonstrating that JWST can uncover heavily dust-obscured progenitors that are invisible in optical pre-explosion data. The 'quasi-snapshot' of the SED across 1.5–7.7 μm is genuinely unprecedented for a pre-explosion image, and the paper makes full use of archival public data with a transparent modeling approach, including a comparison to contemporaneous independent work by Kilpatrick et al. The qualitative conclusions — that the star was an RSG with significant circumstellar dust — are well supported. However, the headline 'most luminous' and 'dustiest' claims rest on a small number of fragile assumptions: the adopted distance, the host-galaxy reddening, and the DUSTY input parameters.

major comments (3)
  1. [§3.5, Abstract (and §5)] The distance is internally inconsistent: the abstract states 11.67 ± 0.27 Mpc, while §3.5 adopts d = 10.73 ± 1.76 Mpc. The adopted value is an inverse-variance weighted mean of distances spanning 7.5–13.9 Mpc (Fig. 5), including low EPM values the authors themselves call 'likely to be the less certain.' Since L_bol ∝ d^2, a true distance of 7.5 Mpc would reduce log L to ≈4.77, erasing the 'most luminous' claim; even the 1σ lower bound (9.0 Mpc) gives log L ≈ 4.93. The JAGB- and Cepheid-based distances (11.38 ± 0.58 and 11.7 ± 1.0 Mpc) are more reliable and agree with each other. The paper should either adopt these stellar-based distances as primary or present all luminosity-dependent results as a function of distance, showing how the conclusions degrade at the low end.
  2. [§4, DUSTY fitting] The reported T_eff = 2100–2500 K and L_bol are not independent inferences: T_phot is an input parameter of the DUSTY model, and L_bol is the integral of the best-fit model SED. The 'inference' is therefore to a large extent a restatement of the assumed input grid. The paper should explicitly state that these are model output values conditioned on the assumed input photosphere, and should present the sensitivity of L_bol and the derived stellar radius to the assumed T_phot (e.g., giving the 3500 K case as an alternative in Table/form). The DUSTY point-source warning (T_eff > 2508 K) is mentioned, but the paper still quotes R_eff ≈ 2180 R_sun as 'truly enormous' without a caveat that this radius is formally outside the model's validity.
  3. [§3.4 and §4] The adopted host reddening E(B−V)_host = 0.54 (A_V(host) = 1.69) comes from spectral and color template matching, while the Na I D EW suggests A_V ≈ 0.7. The authors dismiss the Na I D measurement, but the discrepancy is large and the template-based method assumes the comparison SNe have zero or well-known intrinsic colors, which the paper itself discusses is uncertain. The derived CSM optical depth τ_V = 11–14 and A_V(CSM) ≈ 7.6 are obtained after correcting for A_V(host); if A_V(host) were lower, the required CSM dust column would drop accordingly. The 'dustiest' claim is therefore degenerate with the assumed host reddening. The authors should propagate the full range of E(B−V)_host through the DUSTY fitting, or fit host reddening and CSM dust simultaneously, and show how L_bol, τ_V, and A_V(CSM) vary with this assumption.
minor comments (4)
  1. [§3.3] The variability analysis is acknowledged to be 'somewhat contrived and a bit fanciful.' The 470 and 660 day sinusoids are fit to only a handful of F814W points, and the consistency with NIRCam data is qualitative. Since this is not central to the main claims, it could be moved to a separate 'speculative' subsection or toned down to avoid giving the impression of a secure period.
  2. [§5, Period–luminosity relation] The comparison with the Yang & Jiang, Soraisam et al., and Ren et al. period–luminosity relations uses M_Ks estimated from F212N/F277W photometry without a clear filter transformation to K_s. The authors should state what color correction (if any) was applied, or present this as a rough consistency check only.
  3. [Table 1 and §3.2] The F770W photometry differs from Kilpatrick et al. by 0.3–0.7 mag depending on method, and the star sits on a PAH-emission ridge. This systematic uncertainty is large compared to the formal errors and should be propagated into the SED fit or at least discussed with quantitative impact.
  4. [§4] The DUSTY grid is coarse (χ²_red < 1) and the models 'do not precisely follow' the F164N and F187N data, yet the quoted allowed ranges (T_phot = 2100–2500 K, τ_V = 11–14) are presented as firm. A residual plot or a statement of which data points drive the constraints would help the reader judge the fit quality.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: SED-model parameters are fitted to independent JWST photometry; distance and reddening enter as external inputs.

full rationale

The central claims (dusty RSG, T_eff = 2100–2500 K, log L_bol/L_sun = 5.08 ± 0.16) come from fitting a DUSTY radiative-transfer grid to independent HST/JWST photometry. T_eff is the fitted input photospheric temperature of the model, but this is ordinary parameter estimation rather than a self-fulfilling prediction: the data select a restricted range (T_phot = 2100–2500 K, T(R_in) = 1000–1200 K, tau_V = 11–14) that the paper exhibits as fits to observed fluxes in many bands. L_bol is the integral of the best-fit model, but that model is constrained to reproduce the observed near- to mid-infrared SED; the integral is not algebraically identical to a single input parameter. The dusty-CSM conclusion is driven by the observed red SED, which a bare 2300 K PHOENIX photosphere cannot match, and the silicate-rich composition is additionally checked by fitting (no more than ~4% carbon allowed). The adopted distance, while internally inconsistent between abstract (11.67 ± 0.27 Mpc) and body (10.73 ± 1.76 Mpc), enters externally as a d^2 scaling; a different distance would rescale L_bol but does not make the inference equivalent to the input. Self-citations to prior Van Dyk work for DUSTY modeling assumptions are supportive, not load-bearing, because the present data independently select the allowed model ranges. The admittedly 'contrived' variability model is not load-bearing for the luminosity or dust claims. No step reduces to its own input or to a self-citation chain.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The paper's central claims rest on a standard set of modeling tools (DUSTY, PHOENIX) plus several unverified assumptions: the host extinction measured toward the SN is assumed identical to that toward the candidate, the dust is assumed to be O-rich silicates, and the adopted distance is a weighted mean of heterogeneous estimates. No new physical entities are introduced. The largest leverage on the headline luminosity comes from the free distance parameter, whose value differs between the abstract and the text.

free parameters (6)
  • Host-galaxy distance modulus μ = 30.15 ± 0.36 mag (d = 10.73 ± 1.76 Mpc)
    Weighted mean of discordant literature and new distances (7.5–13.9 Mpc); all luminosity inferences scale with d². The abstract quotes a different value (11.67 ± 0.27 Mpc).
  • Host-galaxy reddening E(B−V)_host = 0.54 ± 0.08 mag
    Adopted from spectral and B−V color template matching to comparison SNe; used to deredden all candidate photometry and hence shapes the SED and luminosity.
  • DUSTY model parameters T_phot, T(R_in), τ_V = T_phot = 2100–2500 K, T(R_in) = 1000–1200 K, τ_V = 11–14 (best: 2300 K, 1100 K, 12)
    Fit to the observed SED with χ²_red < 1 over a coarse grid; T_phot is then reported as the inferred effective temperature.
  • Variability periods = ~470 and ~660 days
    Sinusoidal fits to 8 F814W epochs in 2001 plus JWST/NIRCam constraints; authors describe the model as 'contrived'.
  • R_V = 3.1 and extinction laws = R_V = 3.1; Cardelli et al. (1989) for optical–NIR, Xue et al. (2016) for F2100W
    Standard assumption for interstellar dust; affects all dereddened photometry.
  • Gas-to-dust ratio and bulk dust density for M_dot = 200 and 3 g/cm³
    Assumed Galactic values used to convert DUSTY optical depth into mass-loss rate; does not affect the central luminosity claim.
assumptions (6)
  • domain assumption DUSTY code correctly computes radiative transfer through a spherical dusty shell with r^-2 density profile.
    DUSTY is a standard code, but the spherical-shell/r^-2 geometry is an assumption; §4 of the paper.
  • domain assumption The dust composition is predominantly O-rich silicates (≤4% amorphous carbon).
    Justified by expecting RSG chemistry, not directly observed; §4: 'The predominantly Si-rich nature of the CSM dust appears to be quite firm.'
  • domain assumption The central photosphere is described by PHOENIX model atmospheres at solar metallicity, log g = −0.5.
    Used as DUSTY input; §4. A different metallicity/gravity would change the model SED.
  • domain assumption All host-galaxy extinction derived toward the SN applies equally to the progenitor candidate.
    Stated in §3.4: 'We hereafter assume that this total extinction to the SN is applicable to the progenitor candidate as well.'
  • domain assumption Comparison SNe (SN 2007od, 2008M, 2013ej) have negligible or known host reddening and are valid templates for the SN 2025pht reddening estimate.
    Used in Appendix A.2–A.4; e.g., SN 2007od and 2008M assumed to have A_V(host) = 0.
  • domain assumption The JAGB distance method calibration anchored to M106 applies to NGC 1637 and has no significant metallicity dependence.
    Appendix B.3; authors caution 'JAGB technique is relatively new' and cite ongoing metallicity studies (Goldman et al. 2025).

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Cite this review

Pith. "Pith review of The Progenitor of the Type II-Plateau SN 2025pht in NGC 1637: The Dustiest, Most Luminous Red Supergiant So Far?." pith.science (2026). https://pith.science/paper/KZJKCDLB

@misc{pith2026260109087,
  author       = {Pith},
  title        = {Pith review of: The Progenitor of the Type II-Plateau SN 2025pht in NGC 1637: The Dustiest, Most Luminous Red Supergiant So Far?},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KZJKCDLB}},
  note         = {Machine review of arXiv:2601.09087}
}
read the original abstract

We provide a characterization of the red supergiant (RSG) progenitor candidate for the nearby Type II-plateau supernova (SN) 2025pht in NGC 1637. The star was first detectable in 2001 by the Hubble Space Telescope (HST) and then again in a dozen bands by the James Webb Space Telescope (JWST) in 2024. This "quasi-snapshot" of the star's nature almost immediately prior to explosion is unprecedented. The RSG varied in brightness, and we posit that it could have been a pulsating variable, possibly with a long period of ~660 days. The largest uncertainty is the host-galaxy distance, which we establish to be 11.67+/-0.27 Mpc. The star was also heavily extinguished by interstellar dust internal to the host, with visual extinction A_V(host)~1.7 mag (total A_V(tot)~1.8 mag). Dust radiative-transfer modeling reveals the star's circumstellar medium to be quite dusty and silicate-rich, yielding a bolometric luminosity as high as log(L_bol/L_Sun)=5.16+/-0.03 and a cool effective temperature T_eff=2100--2500 K. The available HST optical data had no bearing on the shape of the candidate's observed spectral energy distribution -- for the first time, without the archival JWST observations we would not have been able to detect and characterize the candidate at all. The SN 2025pht progenitor candidate, although quite similar to that of SN 2023ixf, may be the most luminous star identified to date.

Figures

Figures reproduced from arXiv: 2601.09087 by the authors.

Figure 1
Figure 1. Portions of images in which the SN 2025pht site was serendipitously captured, all shown to the same orientation and scale. The site location corresponds to that of the progenitor candidate identified by I. P´erez-Fournon et al. (2025) and indicated by solid tickmarks in each panel. Panel (a) is a coaddition of all the HST WFPC2 F555W images obtained of the host galaxy from 2001 September 2 to October 31; panel (b) i… view at source ↗
Figure 2
Figure 2. Optical spectra of SN 2025pht from 2025 July 3 (J. Strader 2025), and from July 31, August 21, and August 30 (this study). Various spectral features, including telluric absorption, are indicated. Also shown for comparison are spectra at various ages of the SNe II-P SN 2007od and SN 2008M (C. P. Guti´errez et al. 2017), SN 2013ej (G. Dhungana et al. 2016), and SN 2023ixf (W. Zheng et al. 2025). All spectra have been … view at source ↗
Figure 3
Figure 3. Optical BV I (Vega) light curves of SN 2025pht from P. J. Mikolajczyk et al. (2025). For comparison we show light curves in these bands for SN 2007od (C. Inserra et al. 2011; J. P. Anderson et al. 2024), SN 2008M (J. P. Anderson et al. 2024), SN 2009bw (C. Inserra et al. 2012), and SN 2013ej (S. Valenti et al. 2014; S. Bose et al. 2015; F. Huang et al. 2015; G. Dhungana et al. 2016; F. Yuan et al. 2016); these curve… view at source ↗
Figures from the paper (13 more)
Figure 4
Figure 4. Figure 4: (a): Photometry from HST WFPC2 data from 2001 in F814W (see [PITH_FULL_IMAGE:figures/full_fig_p013_4.png]
Figure 5
Figure 5. Figure 5: A compendium of all of the known distance estimates to the host galaxy NGC 1637. The estimates we have culled from the literature are shown as filled circles. Also included here are estimates we have made in this study, based on SCM measurements to SN 1999em (filled sq…
Figure 6
Figure 6. Figure 6: The reddening- and distance-corrected observed SED of the SN 2025pht progenitor candidate. Measurements from HST and JWST data from 2024 are shown with solid circles; the HST data from 2001 are open circles. Only the faintest HST F814W detection from 2001 (see [PITH_F…
Figure 7
Figure 7. Figure 7: Hertzsprung-Russell diagram show￾ing the inferred locus in Teff and Lbol of the SN 2025pht progenitor candidate (black square). Also shown are theoretical BPASS single-star evolution￾ary tracks (E. R. Stanway & J. J. Eldridge 2018) at two different metallicities, Z = 0…
Figure 8
Figure 8. Figure 8: Comparison of the observed, reddening- and distance-corrected, SEDs of four of the dustiest known SN progenitor candidates: SN 2025pht (this study), SN 2012aw (S. D. Van Dyk et al. 2012), SN 2017eaw (S. D. Van Dyk et al. 2019), and SN 2023ixf (S. D. Van Dyk et al. 2024…
Figure 9
Figure 9. Figure 9: The region around the Na i D feature in flux-normalized optical spectra (solid curves) of SN 2025pht from 2025 July 3 (J. Strader 2025) and from July 31, August 21, and August 30 (all in this study). The spectra have been corrected for the redshift of the host galaxy. …
Figure 10
Figure 10. Figure 10: Optical spectra of SN 2025pht. We show the SN 2025pht classification spectrum from 2025 July 3 (J. Strader 2025) in panel (a), and spectra from 2025 July 31, August 21, and August 30 (all from this study) in panels (b), (c), and (d), respectively. Displayed for compar…
Figure 11
Figure 11. Figure 11: Optical B − V color evolution of SN 2025pht, based on photometry from (P. J. Mikolajczyk et al. 2025). Also shown for comparison are B − V color curves for SN 2007od (C. Inserra et al. 2011; J. P. Anderson et al. 2024), SN 2008M (J. P. Anderson et al. 2024), SN 2009bw…
Figure 12
Figure 12. Figure 12: B −V color curves for SN 2007od (C. Inserra et al. 2011; J. P. Anderson et al. 2024), SN 2008M (J. P. Anderson et al. 2024), SN 2009bw (C. Inserra et al. 2012), and SN 2013ej (S. Valenti et al. 2014; S. Bose et al. 2015; F. Huang et al. 2015; G. Dhungana et al. 2016; …
Figure 13
Figure 13. Figure 13: Expansion velocities for SN 2025pht, based on the Fe ii absorption lines. Shown for comparison are the mean velocities, and their uncertainties, for the SN II-P sample from C. P. Guti´errez et al. (2017). B.3. A JAGB Distance For the Host Galaxy Following S. Li et al.…
Figure 14
Figure 14. Figure 14: The JAGB F150W brightness, corrected for Galactic foreground extinction (E. F. Schlafly & D. P. Finkbeiner 2011), as a function of radial distance from the NGC 1637 nucleus (solid red curve; following A. J. Lee et al. 2025). Each data point is the mode measured from t…
Figure 15
Figure 15. Figure 15: Left: CMD in F150W and F277W for the stars in NGC 1637 beyond a radial distance of 2.19 kpc from the galactic nucleus; see [PITH_FULL_IMAGE:figures/full_fig_p033_15.png]
Figure 16
Figure 16. Figure 16: CMD based on the WFPC2 and WFC3 UVIS data for the host galaxy NGC 1637. The Dolphot photometry has been post-processed via quality filtering (see text) and corrected from Galactic foreground reddening. Also shown would be the brightness of the TRGB if the host distanc…

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Pith tools

Reviewed August 3, 2026 · model on record in the stance chip above.