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SN 2023vjh is a 1991bg-like Type Ia supernova that is systematically fainter than its class and explosion models, with reddening that may come from circumstellar dust rather than the host galaxy.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-07-13 06:26 UTC pith:Z5PHPOGW

load-bearing objection Solid multi-wavelength data set on an extreme 91bg-like SN whose faintness and color excess are real; the CSM reading is plausible but not forced, and the paper already flags residual model tension. the 2 major comments →

arxiv 2607.08821 v1 pith:Z5PHPOGW submitted 2026-07-09 astro-ph.HE

The type Ia supernova 2023vjh: a peculiar 1991bg-like SN with unusually faint light curves

M. Kopsacheili , L. Galbany , G. Folatelli , M. M. Phillips , C. R. Burns , M. D. Stritzinger , H.-Y. Miao , M. Gonz\'alez-Ba\~nuelos
show 27 more authors
R. Garc\'ia-Benito T. E. M\"uller-Bravo E. Y. Hsiao K. Auchettl J. P. Anderson C. Ashall T.-W. Chen D. D. Desai M. E. Huber T. de Jaeger J. M. DerKacy M. Gromadzki J. T. Hinkle W. Hoogendam C. Jimenez-Palau K. Matilaine P. A. Mazzali K. Medler T. Pessi C. Pfeffer K. Phan G. Pignata R. Sanfeliu B. J. Shappee M. A. Tucker H. Xiao D. R. Young
This is my paper
classification astro-ph.HE
keywords Type Ia supernovae1991bg-likesubluminous SNecircumstellar materiallight curvesextinctionSN 2023vjhfast decliners
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper presents multi-band photometry and optical-to-NIR spectra of SN 2023vjh, a fast-declining, subluminous Type Ia supernova in an elliptical galaxy. Its light-curve parameters and cool-photosphere spectral features place it firmly among 1991bg-like events, including the extreme-cool subclass. Yet the object is fainter than both typical members of that class and the explosion models compared to it. Light-curve fits and color relations imply substantial host reddening, which is rare for these events, while the absence of Na I D absorption and a large projected offset from the galaxy center argue that ordinary interstellar dust is minimal. The authors therefore suggest that circumstellar material may be dimming the light; applying a low-R_V CSM extinction law improves the match in the blue bands, though residual tension remains in the i band. The work matters because it flags an outlier that can test how complete current 91bg-like templates and models are, and because the same object still yields Hubble-constant estimates consistent with other fast decliners when standardized by color or the Tripp relation.

Core claim

SN 2023vjh is a spectroscopically and photometrically confirmed 1991bg-like (extreme-cool) Type Ia supernova whose light curves are systematically fainter than other well-studied members of the class and than Chandrasekhar-mass and sub-Chandrasekhar explosion models. The inferred host reddening is unusually high for the class, yet the lack of Na I D and large distance from a passive host imply that ordinary interstellar extinction is small, pointing instead to possible circumstellar dust.

What carries the argument

Joint light-curve fitting (SNooPy 91bg templates, Lira-law color, and Goobar-style CSM extinction) compared with Blondin DDC25 and SCH2p0 explosion models, together with the spectroscopic absence of Na I D and the measured 6.8 kpc projected offset from the host center.

Load-bearing premise

That missing Na I D absorption and a large projected distance from a passive elliptical galaxy together prove that any substantial reddening must be circumstellar rather than interstellar dust along the line of sight.

What would settle it

A high-resolution spectrum that either detects host Na I D (or equivalent dust tracers) at a strength matching E(B-V) ~ 0.2–0.35, or a multi-wavelength SED that rules out low-R_V CSM extinction while still matching the observed blue-band faintness.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • 91bg-like samples used for cosmology or template building must allow for objects that are systematically under-luminous relative to current models.
  • CSM extinction becomes a plausible extra parameter for at least some fast-declining SNe Ia even in elliptical hosts.
  • Residual i-band discrepancies after CSM correction indicate that model spectral energy distributions still need improvement in the red/NIR for cool events.
  • Color-based and Tripp-style standardization of fast decliners can still return H0 values consistent with larger samples even for this outlier.

Where Pith is reading between the lines

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

  • If CSM is confirmed around other 91bg-like events, it would tighten the link between subluminous explosions and residual binary-interaction material.
  • The lack of a clear H-band break in the late NIR spectra may be another signature of the same cool, low-56Ni ejecta that produces the extreme-cool classification.
  • Future surveys that catch similar objects early enough for dense multi-band coverage could separate CSM from intrinsic under-luminosity by tracking color evolution before maximum.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The manuscript presents multi-band photometry (POISE/Swope, ZTF, ATLAS) and optical/NIR spectroscopy of SN 2023vjh, a fast-declining Type Ia supernova in the elliptical galaxy MCG+04-10-013. Light-curve parameters from SNooPy (Δm15(B) = 1.89 ± 0.01 mag, sBV = 0.45 ± 0.03) and spectral features (strong Si II, Ca II, Ti II; cool/extreme-cool placement on Branch/Wang and pEW diagrams) firmly place it among 91bg-like events. The central claim is that SN 2023vjh is systematically fainter than both typical 91bg-like SNe and the Blondin et al. (2018) DDC25/SCH2p0 models, while color-based and SNooPy fits imply unusually large host reddening (E(B-V)host ~ 0.2–0.35 mag). The non-detection of host Na I D (3σ EW upper limit < 0.53 Å) and the 6.8 kpc projected offset from the center of a passive elliptical are used to argue that ordinary interstellar extinction is minimal, so circumstellar (Goobar 2008) dust may be required; residual i-band discrepancies are attributed to model SED limitations. An H0 estimate using the Phillips et al. (2026) Tripp and Color methods for fast decliners is also presented.

Significance. If the faintness and the need for non-standard (CSM-like) extinction hold, SN 2023vjh expands the known diversity of 91bg-like events and supplies a concrete case where color-inferred reddening and spectroscopic/host indicators of dust disagree. The data set is of high quality: dense early multi-band coverage, consistent SNooPy parameters across max/EBV2/color models, Monte-Carlo continuum-varied velocities and pEWs, three late NIR spectra, and host IFS age/metallicity. The H0 exercise with the Phillips et al. (2026) calibrations is a useful consistency check for the emerging standardization of fast decliners. These strengths make the paper a solid observational contribution even if the CSM interpretation remains provisional.

major comments (2)
  1. §4.2 and Abstract: The inference that E(B-V)host ~ 0.2–0.35 mag must be circumstellar rests on the non-detection of Na I D (3σ EW < 0.53 Å from the smoothed spectra in Fig. A.3) plus the 6.8 kpc projected offset. Na I D is an imperfect tracer (large scatter in EW–E(B-V) relations; dust can exist without detectable Na, especially if ionization or composition is atypical). Projected galactocentric distance does not exclude a line-of-sight cloud or halo material. The paper should either (i) quantify how much of the color excess could still be ordinary host ISM given the EW limit and known scatter, or (ii) present the CSM scenario more explicitly as one possible interpretation among others (intrinsic coolness/template mismatch, atypical R_V, undetected ISM). Without that, the claim that the object is 'systematically fainter than models/other 91bg-likes' under MW-only correction (Fig. 6 fille
  2. §4.2 and Fig. 4: Even after applying MW-type CSM extinction with E(B-V)host = 0.2, residual discrepancies remain, especially in the i-band (and a milder one in B). The text attributes these to model SED limitations (Ca II NIR triplet, line blanketing). Because the same residual is used both to justify CSM and to excuse model mismatch, the paper should test whether an intrinsic luminosity offset (lower 56Ni or different ejecta mass) plus ordinary extinction can reproduce the multi-band light curves equally well, or show that the i-band residual is quantitatively expected from the model spectra. Otherwise the conclusion that 'including CSM-like extinction improves agreement' is only partially demonstrated.
minor comments (5)
  1. Table 1: The host MB is listed as 20.13 ± 0.53; absolute magnitudes of galaxies are conventionally negative. Clarify whether this is an absolute magnitude or an apparent magnitude, and correct the sign if needed.
  2. §4.1 / Fig. A.2: The r-band light curve is broader and the i-band narrower than the 91bg template. A short quantitative statement of the residual (e.g., peak-to-template magnitude difference or reduced χ^{2} per band) would help the reader assess the quality of the SNooPy fits used for Δm15 and sBV.
  3. Fig. 14 / §5.2: The absence of an H-band break is noted but left ambiguous (S/N vs. physical). A simple upper limit on the break contrast or a direct comparison of continuum S/N with SN 2015bo/2022xkq at the same wavelengths would strengthen the statement.
  4. Throughout: Occasional missing spaces after punctuation and a few duplicated words in the abstract/introduction (e.g., 'We presentobservations') should be cleaned in production.
  5. §4.5: The H0 values are consistent with Phillips et al. (2026), but the i-band systematically pulls H0 low. A one-sentence note that this is expected from the already-noted faint i-band light curve would avoid the impression of tension.

Circularity Check

0 steps flagged

No significant circularity: observational measurements and empirical comparisons; secondary H0 uses co-authored calibration but is not load-bearing for the faintness/CSM claim.

full rationale

The paper is a standard observational characterization of SN 2023vjh. Light-curve shape parameters (Δm15(B), sBV), absolute magnitudes, expansion velocities, and pEWs are measured directly from photometry and spectra (Sects. 4.1, 5.1; Tables B.2). Classification as 91bg-like / cool / extreme-cool follows by placing those measured quantities on established diagrams (Branch, Wang, Folatelli, Alburai) against external comparison samples; this is comparison, not a self-definitional loop. Host reddening is inferred from SNooPy EBV/color models and the Lira relation, then tested against the independent spectroscopic non-detection of Na I D and the projected offset; the paper does not redefine the non-detection as the extinction value. Model comparisons (Blondin DDC25/SCH2p0 + Goobar CSM law) are external templates applied after the fact; residual i-band tension is acknowledged rather than forced away. The only self-citation of note is the secondary H0 estimate (Sect. 4.5) that adopts coefficients from Phillips et al. (2026), whose author list overlaps; that result is not required for the central faintness/CSM interpretation and does not reduce the main claim by construction. No equation equates a claimed prediction to a fitted input, no uniqueness theorem is imported to forbid alternatives, and no ansatz is smuggled as a derivation. Score 1 reflects only the minor, non-load-bearing co-authored calibration use.

Axiom & Free-Parameter Ledger

4 free parameters · 5 axioms · 0 invented entities

The central claim rests on standard SN Ia light-curve fitting machinery, published explosion models, and an empirical CSM extinction prescription, plus the observational premise that non-detection of Na I D plus host morphology rule out ordinary interstellar dust. No new physical entities are introduced; free parameters are the usual fitted extinction and light-curve shape quantities.

free parameters (4)
  • E(B-V)_host = 0.20–0.35 mag
    Fitted by SNooPy EBV_model2 and color_model (~0.35 mag) and by the updated Lira law (~0.20 mag); adopted trial value 0.2 for CSM tests. Directly controls the absolute-magnitude comparison that drives the 'unusually faint' claim.
  • R_V (host) = 2.1±0.5
    Derived from SNooPy color_model as 2.1±0.5; also implicit in the Goobar (2008) CSM law parameters (p, α) chosen for MW/LMC dust.
  • s_BV / Δm15(B) = s_BV=0.45, Δm15=1.89
    Light-curve shape parameters fitted by SNooPy (s_BV=0.45±0.03, Δm15(B)=1.89±0.01) that place the object in the 91bg-like locus and enter the H0 Tripp/Color estimators.
  • power-law rise indices n_r, n_g = n_r=1.31±0.11, n_g=1.51±0.17
    Fitted jointly to early g/r light curves to obtain explosion epoch t0; used only for rise-time reporting, not the faintness claim.
axioms (5)
  • domain assumption Cardelli et al. (1989) extinction law with R_V=3.1 for Milky Way dust (E(B-V)_MW=0.236 from Schlafly & Finkbeiner 2011).
    Applied uniformly to all photometry and spectra before host/CSM tests (§2.1).
  • domain assumption Blondin et al. (2018) DDC25 and SCH2p0 models correctly represent the expected luminosity and colors of 91bg-like explosions in the absence of extra dust.
    Used as the baseline against which residual faintness is judged (§4.2, Fig. 4).
  • domain assumption Goobar (2008) CSM extinction law (A_λ = A_V (1-α + α(λ/λ_V)^p) with p=-1.5/-2.5, α=0.9/0.8) is an adequate description of possible circumstellar dust.
    Applied as the alternative extinction prescription that improves blue-band agreement (§4.2).
  • ad hoc to paper Non-detection of Na I D (EW upper limit <0.53 Å) plus large projected galactocentric distance implies negligible host interstellar extinction.
    Key premise that forces the interpretation toward CSM or intrinsic faintness (§4.2).
  • domain assumption SNooPy 91bg templates and the updated Lira relation of Burns et al. (2014) correctly recover shape and color parameters for fast decliners.
    Used for all light-curve fits and the independent E(B-V) estimate (§4.1–4.2).

pith-pipeline@v1.1.0-grok45 · 38740 in / 3439 out tokens · 30548 ms · 2026-07-13T06:26:53.195437+00:00 · methodology

0 comments
read the original abstract

We present observations of the 1991bg-like type Ia supernova (SN) 2023vjh, associated with the elliptical galaxy MCG+04-10-013. Its light-curve shape parameters ($\Delta m_{15}(B)=1.89 \pm 0.01$ mag and $s_{BV} = 0.45 \pm 0.03$), together with its spectroscopic evolution, place it firmly within the class of fast-declining, subluminous SNe Ia. The near-peak spectra show prominent features of Si II, Ca II, and Ti II, consistent with a cool photosphere, and place SN 2023vjh within the "cool" and extreme cool regions on the classification diagrams. In addition, the three late-phase near-infrared (NIR) spectra display the Ca II NIR triplet, Fe II, and Co II absorptions, but no obvious $H$-band break. Although SN 2023vjh falls in the same regions of the classification diagrams as other well-studied 91bg-like events, it shows some deviation within this class. In particular, it is systematically fainter than predicted by explosion models and fainter than other well-studied 91bg-like SNe. Light-curve fitting and color-based analyses indicate a relatively large reddening ($E(B-V)_{host}\sim$ 0.2 - 0.35 mag), which is unusual for 91bg-like SNe. Yet, the lack of detectable Na I D absorption in its spectra, along with its large projected distance from the center of its passive host galaxy (6.8 kpc), suggests that interstellar extinction along the line of sight is minimal. SN 2023vjh appears to be fainter than typical 91bg-like SNe, and it could be affected by circumstellar material (CSM). Comparisons with explosion models and alternative extinction prescriptions show that including CSM-like extinction improves agreement in the blue bands, but residual discrepancies in the $i$-band may reflect limitations in the model.

Figures

Figures reproduced from arXiv: 2607.08821 by B. J. Shappee, C. Ashall, C. Jimenez-Palau, C. Pfeffer, C. R. Burns, D. D. Desai, D. R. Young, E. Y. Hsiao, G. Folatelli, G. Pignata, H. Xiao, H.-Y. Miao, J. M. DerKacy, J. P. Anderson, J. T. Hinkle, K. Auchettl, K. Matilaine, K. Medler, K. Phan, L. Galbany, M. A. Tucker, M. D. Stritzinger, M. E. Huber, M. Gonz\'alez-Ba\~nuelos, M. Gromadzki, M. Kopsacheili, M. M. Phillips, P. A. Mazzali, R. Garc\'ia-Benito, R. Sanfeliu, T. de Jaeger, T. E. M\"uller-Bravo, T. Pessi, T.-W. Chen, W. Hoogendam.

Figure 1
Figure 1. Figure 1: The field of the SN 2023vjh and its host galaxy MCG+04- [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Left: Collapsed 2D image of the galaxy, obtained by summing the flux over all wavelengths (from a PMAS cube at CAHA). The red circle marks the radius containing 90% of the galaxy light, and the white ’X’ indicates the masked position of SN 2023vjh. Right: Spectrum of the galaxy extracted within the same radius (black line) with the best-fit model from pPXF overplotted (red line). The residuals of the fit a… view at source ↗
Figure 3
Figure 3. Figure 3: The optical light curves of SN 2023vjh. The gray, dotted [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: The light-curve of SN 2023vjh (red line) in comparison [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Luminosity width relation as a function of [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The MW extinction corrected color curves of SN 2023vjh [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Color-stretch parameter 𝑠𝐵𝑉 as a function of 𝑡 𝑖 𝑚𝑎𝑥 − 𝑡 𝐵 𝑚𝑎𝑥 for different sub-types of SN Ia (Ashall et al. 2020). The 𝑡 𝑖 max and 𝑡 𝐵 max refer to the epochs of maximum light in the 𝑖 and 𝐵 bands, respectively. B V g r i Filter 65 70 75 80 H0 [km/s/Mpc] mean H0 - Color mean H0 - Tripp Phillips+26: Tripp 75.5 ± 3.1 Phillips+26: Color 76.7 ± 3.0 Tripp = 71.56 ± 3.09 Color = 74.60 ± 2.22 [PITH_FULL_IMAGE… view at source ↗
Figure 9
Figure 9. Figure 9: We derive the Hubble constant from SN 2023vjh us [PITH_FULL_IMAGE:figures/full_fig_p009_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: The optical spectrum of SN 2023vjh obtained around [PITH_FULL_IMAGE:figures/full_fig_p009_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Evolution of the expansion velocities. −10 0 10 20 30 40 50 Days after B-band maximum 0 100 200 300 400 500 pEW [Å] O I λ7775 Si II λ6355 Si II λ5972 Ca II IR [PITH_FULL_IMAGE:figures/full_fig_p010_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Evolution of the pseudo-equivalent widths. [PITH_FULL_IMAGE:figures/full_fig_p010_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Near-infrared spectra of SN 2023vjh, corrected for Milky [PITH_FULL_IMAGE:figures/full_fig_p011_14.png] view at source ↗

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