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arxiv: 2605.16916 · v1 · pith:2QG3F4CWnew · submitted 2026-05-16 · 🌌 astro-ph.HE

SN 2023dbc in M108: Optical and Near-Infrared Observations of a Highly-Obscured, Moderately Energetic Stripped-Envelope Supernova

Masayuki Yamanaka , Takahiro Nagayama , Akari Kumano , Devendra Kumar Sahu , Avinash Singh , Hrishav Das , G. C. Anupama This is my paper

Pith reviewed 2026-05-19 20:00 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords supernovaType Ibaspherical explosioncore fallbackbinary progenitornear-infrared observationsstripped-envelope supernovaSN 2023dbc
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The pith

SN 2023dbc originated from an aspherical explosion with partial core fallback from a 15 solar mass binary progenitor that retained its helium envelope.

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

The paper presents optical and near-infrared observations of the highly reddened Type Ib supernova SN 2023dbc spanning 2 to 136 days after explosion. Color comparisons yield an extinction of about 4.1 magnitudes in V, and corrected peak magnitudes around -16.8 to -17.0 in the near-infrared. The rise time, velocities reaching 16000 km/s, and light-curve timescale lead to estimates of kinetic energy 4.1 times 10^51 erg, ejecta mass 2.3 solar masses, and nickel mass 0.038 solar masses. A two-component model applied to the data reveals a steep outer density profile against a dense inner core, which the authors take as direct evidence of ejecta asphericity and partial core fallback.

Core claim

SN 2023dbc is a moderately energetic stripped-envelope supernova whose light-curve timescale, expansion velocities, and low nickel yield are best explained by an aspherical explosion with partial core fallback arising from a progenitor of initial mass about 15 solar masses that retained its helium envelope within a binary system.

What carries the argument

Two-component model fitted to the light-curve timescale and velocity data that separates a steep outer density profile from a dense inner core and thereby implies ejecta asphericity.

If this is right

  • The progenitor must have lost its hydrogen but kept helium through binary interaction rather than single-star winds.
  • Partial core fallback naturally accounts for the modest nickel mass without requiring unusual nucleosynthesis.
  • The event sits spectroscopically between ordinary Type Ib and broad-lined Type Ic supernovae, suggesting a continuous sequence of explosion energies and asymmetries.
  • Similar two-component density structures may appear in other moderately energetic stripped-envelope events observed at late times.

Where Pith is reading between the lines

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

  • If asphericity is common in this mass range, polarization surveys of future Type Ib events could reveal a larger fraction of non-spherical explosions than currently assumed.
  • Binary population synthesis models may need to increase the fraction of 15-solar-mass systems that retain helium envelopes at core collapse.
  • The same density-profile diagnostic could be applied to archival light curves of other reddened supernovae to test how often partial fallback occurs.

Load-bearing premise

The two-component model applied to the light-curve timescale and velocity data accurately captures a steep outer density profile versus dense inner core and that this structure directly implies ejecta asphericity rather than viewing-angle effects or incomplete line identification.

What would settle it

Spectropolarimetry showing no significant polarization or a full 3D hydrodynamic simulation reproducing the light curve and spectra with a spherical geometry would falsify the asphericity claim.

Figures

Figures reproduced from arXiv: 2605.16916 by Akari Kumano, Avinash Singh, Devendra Kumar Sahu, G. C. Anupama, Hrishav Das, Masayuki Yamanaka, Takahiro Nagayama.

Figure 1
Figure 1. Figure 1: Optical and NIR g ′ , r ′ , o, i, z, J, H, and Ks-band light curves of SN 2023dbc. Note that these light curves have not been corrected for Galactic or host-galaxy extinction. For clarity, the data are plotted with arbitrary vertical offsets. The g ′ , r ′ , o, i, and z-band magnitudes are presented in the AB system, whereas the J, H, and Ks magnitudes are in the Vega system. The r-band maximum date is ado… view at source ↗
Figure 2
Figure 2. Figure 2: Extinction-corrected r − Ks, r − H, and r − J color evo￾lutions of SN 2023dbc. These are compared with those of SNe 2002ap (Yoshii et al. 2003; Tomita et al. 2006), 2007Y (Stritzinger et al. 2009), 2007gr (Hunter et al. 2009), 2008D (Modjaz et al. 2009; Bianco et al. 2014), 2008ax (Pastorello et al. 2008; Bianco et al. 2014), 2009jf (Sahu et al. 2011; Valenti et al. 2011; Bianco et al. 2014), and 2011dh (S… view at source ↗
Figure 3
Figure 3. Figure 3: NIR J, H, and Ks-band absolute magnitude light curves of SN 2023dbc, compared with those of other SNe Ib/c and IIb. The light curves were corrected for extinction using AJ = 1.0, AH = 0.7, and AKs = 0.4 mag, assuming a distance modulus of µ = 29.8 mag. For SN 2023dbc, the reference epoch (t= 0) is the date of the r-band maximum, whereas for the comparison objects, the reference epochs are as defined in the… view at source ↗
Figure 4
Figure 4. Figure 4: Quasi-bolometric light curve of SN 2023dbc, derived by inte￾grating the g,r,i,z,J,H, and Ks-band photometric data. For compari￾son, the bolometric light curves of other SNe are also shown, including SNe 2002ap (Foley et al. 2003; Yoshii et al. 2003; Tomita et al. 2006), 2007Y (Stritzinger et al. 2009), 2007gr (Valenti et al. 2008b; Hunter et al. 2009), 2008D (Modjaz et al. 2009), 2009jf (Valenti et al. 201… view at source ↗
Figure 5
Figure 5. Figure 5: shows the spectral evolution of SN 2023dbc. Although the observed spectra are significantly reddened owing to the high extinction, several absorption features can be clearly identified. Specifically, the He i λ5876, λ6678, and λ7065 lines are present. The Si iiλ6355 absorp￾tion feature is also visible around t = 4 d. For the subse￾quent analysis, these spectra were corrected for extinction using AV = 4.1 m… view at source ↗
Figure 6
Figure 6. Figure 6: Extinction-corrected spectrum of SN 2023dbc (AV = 4.1 mag and RV = 3.1). The spectrum was smoothed using a 5-pixel boxcar window to enhance the signal-to-noise ratio. For comparison, spectra of the Type Ic-BL SNe 2002ap, 2003jd (Valenti et al. 2008a), and the Type Ib SN 2012au (Takaki et al. 2013) are also shown. The t = 0 d spectrum of SN 2002ap was retrieved from the Weizmann Interactive Supernova data R… view at source ↗
Figure 7
Figure 7. Figure 7: (Upper panel) Ejecta mass (Mej) versus kinetic en￾ergy (Ekin) for SN 2023dbc compared with the large sample from Cano (2013). The explosion properties of SN 2023dbc are consistent with those of typical SNe Ib/c. (Lower panel) Similar to the upper panel, but showing the correlation be￾tween Mej and the radioactive 56Ni mass (MNi ). In both panels, SN 2023dbc is located within the distribution of standard st… view at source ↗
Figure 8
Figure 8. Figure 8: Quasi-bolometric light curve of SN 2023dbc. In addition to the flux integrated over the grizJHKs bands, the curve derived from the inte￾gration of rJHKs data is also shown for comparison. The data are fitted with two-component model curves (Maeda et al. 2003) char￾acterized by γ-ray optical depths of τout/1000 = 0.5 and τin/1000 = 6. The model assumes an outer-layer 56Ni mass of M( 56Ni)out = 0.02 M⊙ and a… view at source ↗
read the original abstract

We present near-infrared (NIR) and optical observations of the highly reddened and moderately energetic Type Ib supernova (SN) 2023dbc, {\bf covering a period from} 2 to 136 days after the explosion. By comparing its color {\bf evolution}, specifically in $r-JHK_{\mathrm{s}}$ and $i-JHK_{\mathrm{s}}$, with those of broad-lined Type Ic (Ic-BL) and Type IIb SNe, we estimate a significant extinction of $A_{V}=4.1\pm0.1$\,mag toward the SN. The extinction-corrected peak absolute magnitudes are $M_{J} = -16.8\pm0.2$\,mag, $M_{H} = -16.8\pm0.2$\,mag, and $M_{K_{\mathrm{s}}} = -17.0\pm0.2$\,mag. The SN {\bf exhibited} an $r$-band rise time of 14.9 days. The spectra {\bf display} broad features {\bf indicative of} high expansion velocities; the He~{\sc i} line velocity was measured at $16,000\,\mathrm{km\,s^{-1}}$ at $t=-4$\,d. Its spectral profile is broader than {\bf those} of typical moderately energetic Type Ib SNe, {\bf yet narrower than those of Type Ic-BL SNe, placing it in an intermediate category}. Based on the light-curve timescale and velocity, we estimate {\bf a} kinetic energy of $E_k = (4.1\pm0.7) \times 10^{51}$\,erg, {\bf an} ejecta mass of $M_{\mathrm{ej}} = 2.3\pm0.7\,M_{\odot}$, and a radioactive $^{56}\mathrm{Ni}$ mass of $(3.8\pm0.1) \times 10^{-2}\,M_{\odot}$. {\bf An} analysis using a two-component model suggests a steep density profile in the outer layer {\bf contrasted with} a dense inner core, {\bf which implies} ejecta asphericity. The low $^{56}\mathrm{Ni}$ mass is consistent with a partial fallback scenario. We conclude that SN 2023dbc originated from an aspherical explosion with partial core fallback, {\bf arising} from a progenitor ($M_{\mathrm{ini}} \simeq 15\,M_{\odot}$) that had retained {\bf its} helium envelope {\bf within} a binary system.

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 reports optical and NIR observations of the highly reddened Type Ib supernova SN 2023dbc spanning 2 to 136 days post-explosion. Extinction is estimated at A_V = 4.1 ± 0.1 mag via color comparisons to Ic-BL and IIb SNe, yielding extinction-corrected peak magnitudes M_J ≈ -16.8, M_H ≈ -16.8, M_Ks ≈ -17.0 mag. An r-band rise time of 14.9 days and He I velocity of 16,000 km s^{-1} at t = -4 d are measured. Scaling from light-curve timescale and velocity gives E_k = (4.1 ± 0.7) × 10^{51} erg, M_ej = 2.3 ± 0.7 M_⊙, and ^{56}Ni mass = (3.8 ± 0.1) × 10^{-2} M_⊙. A two-component model is applied to infer a steep outer density profile versus dense inner core, interpreted as implying ejecta asphericity; the low Ni mass supports partial core fallback. The authors conclude the event arose from an aspherical explosion with partial fallback from a ~15 M_⊙ binary progenitor that retained its helium envelope.

Significance. If the two-component modeling and its geometric interpretation hold, the work adds a well-observed, moderately energetic example to the sample of obscured stripped-envelope SNe and provides constraints on asphericity and fallback scenarios. The direct observational anchors (extinction, magnitudes, velocities) are solid; the derived parameters and progenitor inference could inform binary evolution and explosion asymmetry models if the density-profile-to-asphericity step is strengthened.

major comments (2)
  1. [two-component model analysis] In the two-component model analysis (abstract and the section deriving physical parameters from light-curve timescale and velocity): the statement that the model 'suggests a steep density profile in the outer layer contrasted with a dense inner core, which implies ejecta asphericity' is load-bearing for the central claim but rests on an untested mapping. No comparison to 1D spherical radiative-transfer models with broken power-law density profiles, no polarization data, and no hydrodynamic simulations are referenced to exclude alternatives such as viewing-angle effects or incomplete line identification, as highlighted by the stress-test concern.
  2. [conclusions and progenitor discussion] In the concluding synthesis of progenitor properties: the assignment of M_ini ≃ 15 M_⊙ and a binary system retaining the helium envelope chains the low ^{56}Ni mass and asphericity inference through multiple scaling relations whose applicability to this specific object (with its derived parameters) is stated but not independently validated against the observed rise time and line velocities.
minor comments (2)
  1. [physical parameter estimation] The scaling relations used for E_k, M_ej, and Ni mass (based on light-curve timescale and velocity) should include explicit citations to the source papers at the point of application rather than relying on general references.
  2. [abstract and observations] Minor grammatical phrasing in the abstract (e.g., 'The SN exhibited an r-band rise time of 14.9 days') could be tightened for clarity, and the exact epochs used for the r-JHK_s and i-JHK_s color comparisons should be tabulated or stated.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report on our manuscript. We have addressed each major comment point by point below, providing clarifications and revisions where warranted to strengthen the presentation of our results on SN 2023dbc.

read point-by-point responses

  1. Referee: In the two-component model analysis (abstract and the section deriving physical parameters from light-curve timescale and velocity): the statement that the model 'suggests a steep density profile in the outer layer contrasted with a dense inner core, which implies ejecta asphericity' is load-bearing for the central claim but rests on an untested mapping. No comparison to 1D spherical radiative-transfer models with broken power-law density profiles, no polarization data, and no hydrodynamic simulations are referenced to exclude alternatives such as viewing-angle effects or incomplete line identification, as highlighted by the stress-test concern.

    Authors: We agree that the two-component decomposition offers an indirect constraint on the density structure rather than a definitive proof of asphericity. The approach follows standard techniques applied to other stripped-envelope events in the literature, where a steep outer profile paired with a dense core is commonly interpreted as evidence for asymmetry. We have revised the relevant section and abstract to include explicit caveats, added references to prior studies employing analogous modeling, and briefly discuss possible alternatives including viewing-angle effects and line-identification uncertainties. Full hydrodynamic simulations or new polarization data lie outside the scope of this observational study, but the revised text now frames the asphericity inference more cautiously as suggestive rather than conclusive. revision: partial

  2. Referee: In the concluding synthesis of progenitor properties: the assignment of M_ini ≃ 15 M_⊙ and a binary system retaining the helium envelope chains the low ^{56}Ni mass and asphericity inference through multiple scaling relations whose applicability to this specific object (with its derived parameters) is stated but not independently validated against the observed rise time and line velocities.

    Authors: The progenitor mass and binary configuration are inferred by placing the observationally derived ejecta mass (2.3 M_⊙), kinetic energy, and low nickel mass onto standard binary-evolution tracks for stars that retain a helium envelope. These tracks predict rise times and expansion velocities consistent with the measured 14.9-day r-band rise and 16,000 km s^{-1} He I velocity at t = -4 d. We have expanded the discussion section to include a direct side-by-side comparison of the observed rise time and line velocities with the model predictions for a ~15 M_⊙ binary progenitor, thereby providing the requested independent validation of the scaling relations for this specific event. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives kinetic energy, ejecta mass, and 56Ni mass from observed rise time and line velocities using established external scaling relations. The two-component model is then applied to infer a steep outer density profile versus dense inner core, which is interpreted as implying asphericity and partial fallback; this interpretive step does not reduce the final progenitor conclusion to the inputs by construction, self-definition, or a self-citation chain. No load-bearing uniqueness theorem, ansatz smuggling, or renaming of known results is present. The overall chain remains self-contained against the observational data and standard methods.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central conclusions rest on standard supernova scaling relations calibrated on other events, assumptions about the applicability of a two-component density model, and the interpretation of line velocities as representative of bulk ejecta motion. No new physical constants or entities are introduced.

free parameters (2)
  • A_V extinction
    Derived from color evolution comparison to other SNe; value 4.1 mag is fitted to match observed r-JHK and i-JHK colors.
  • scaling constants in kinetic energy and mass estimates
    E_k and M_ej are obtained from light-curve timescale and velocity using relations whose normalization constants come from prior samples.
axioms (2)
  • domain assumption The two-component model provides a valid description of the outer steep density profile and inner dense core for this event.
    Invoked to interpret the light-curve shape as evidence of asphericity.
  • domain assumption Line velocities measured from He I features represent the characteristic expansion velocity of the ejecta.
    Used to convert observed velocities into kinetic energy and mass estimates.

pith-pipeline@v0.9.0 · 6065 in / 1632 out tokens · 32484 ms · 2026-05-19T20:00:09.340924+00:00 · methodology

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