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arxiv: 2607.02253 · v1 · pith:34NPBV46new · submitted 2026-07-02 · 🌌 astro-ph.HE · astro-ph.SR

SN 2020bij and a Possible Slow-Rise High-Velocity Subclass of Type IIP Supernovae

Sondos Mohsen-Tanev , Iair Arcavi , Shahar Bracha , K. Azalee Bostroem , Griffin Hosseinzadeh , Jesper Sollerman , Claudia P. Guti\'errez , Priscila J. Pessi
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Joseph Anderson Mariusz Gromadzki Avishay Gal-Yam Daichi Hiramatsu Jamison Burke Koichi Itagaki Ting-Wan Chen D. Andrew Howell Curtis McCully Megan Newsome Estefania Padilla Gonzalez Craig Pellegrino
This is my paper

Pith reviewed 2026-07-03 07:39 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords Type IIP supernovaecircumstellar materiallight curve rise timeexpansion velocityred supergiantsmass losssupernova subclasses
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The pith

Five Type IIP supernovae with slow rises and high velocities are explained by weak circumstellar material interaction and proposed as a new subclass.

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

The paper presents SN 2020bij, which rises slowly to its plateau while showing high expansion velocities, and identifies four similar events from the literature. Analytical and numerical light-curve models reproduce all five with only weak or no circumstellar material interaction. The authors therefore argue these objects form a distinct subclass of Type IIP supernovae linked to relatively confined circumstellar material around red supergiant progenitors. This subclass would help map the diversity of late-stage mass loss in massive stars. Early dense photometry combined with early spectra is needed to identify more members and test the physical picture.

Core claim

SN 2020bij and the four comparison events (ASASSN-14kg, SN 2018fif, SN 2021yja, SN 2023axu) share slowly rising light curves and high expansion velocities yet are reproduced by models with weak to no circumstellar material interaction; the authors therefore propose these events constitute a new subclass of Type IIP supernovae associated with relatively confined circumstellar material.

What carries the argument

Analytical and numerical models of Type IIP light curves and spectra that incorporate varying levels of circumstellar material interaction, used to show that weak or absent interaction accounts for the slow rise and high velocities observed in the five events.

If this is right

  • Early and dense photometric coverage plus early spectroscopy will identify additional members of the subclass and map its range of properties.
  • The subclass would directly constrain the diversity of late-stage mass loss in red supergiants.
  • Events in this subclass would require less circumstellar material than typical fast-rising Type IIP supernovae to match observations.
  • The proposal implies that confined circumstellar material is sufficient to produce the observed diversity without invoking strong interaction.

Where Pith is reading between the lines

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

  • If the subclass is real, surveys with rapid cadence could separate it from the general Type IIP population at early times.
  • The confined circumstellar material picture might link these events to a narrow range of red supergiant envelope stripping that is not captured in standard single-star evolution tracks.
  • Follow-up X-ray or radio observations of future members could test whether the confined material leaves a detectable signature at later phases.

Load-bearing premise

That the slow rise and high velocities are driven primarily by the amount of circumstellar material interaction rather than by differences in explosion energy, progenitor radius, or other factors.

What would settle it

A set of hydrodynamic models or additional well-observed events in which the same slow-rise high-velocity properties are reproduced only when circumstellar material interaction is set to zero while explosion energy or radius is varied instead.

Figures

Figures reproduced from arXiv: 2607.02253 by Avishay Gal-Yam, Claudia P. Guti\'errez, Craig Pellegrino, Curtis McCully, Daichi Hiramatsu, D. Andrew Howell, Estefania Padilla Gonzalez, Griffin Hosseinzadeh, Iair Arcavi, Jamison Burke, Jesper Sollerman, Joseph Anderson, K. Azalee Bostroem, Koichi Itagaki, Mariusz Gromadzki, Megan Newsome, Priscila J. Pessi, Shahar Bracha, Sondos Mohsen-Tanev, Ting-Wan Chen.

Figure 1
Figure 1. Figure 1: The unfiltered discovery image of SN 2020bij in the spiral galaxy NGC 3463, obtained with the KAF-1001E CCD mounted on the 0.35m reflector at the Itagaki Astro￾nomical Observatory in Kochi, Japan (Itagaki 2020), taken on MJD 58877.68 (2020-01-29 16:22:49). The position of SN 2020bij is indicated by green tick marks. survey (Smith et al. 2020). Using the ATLAS Public Forced Photometry Server1 (Tonry et al. … view at source ↗
Figure 2
Figure 2. Figure 2: Milky-Way extinction-corrected light curves of SN 2020bij from observations obtained with Las Cumbres Observatory (UBV gri-band), Gaia (G-band), ATLAS (oc-band) and from the Itagaki Astronomical Observatory (unfiltered). Error bars represent 1σ uncertainties and are sometimes smaller than the marker size. Arrows indicate 5σ non-detection limits. The vertical dashed line and surrounding shaded region mark t… view at source ↗
Figure 3
Figure 3. Figure 3: The spectroscopic evolution of SN 2020bij. The phase of each spectrum in rest-frame days relative to explosion is shown on the right. All spectra have been calibrated to the Milky-Way extinction-corrected photometry and are shifted in flux for clarity. The vertical colored lines at the rest wavelengths of hydrogen (Hδ 4101, Hγ 4340, Hβ 4861, and Hα 6563 ˚A), helium (He I 5875 ˚A) and iron (Fe II 5169 ˚A), … view at source ↗
Figure 5
Figure 5. Figure 5: The r-band light curve of SN 2020bij compared to light curves of the prototypical Type IIP SN 1999em (dot-dashed line), the slowly rising Type IIP ASASSN￾14kg, SN 2018fif, SN 2021yja and SN 2023axu (solid lines), and the well-sampled SN 2005cs, SN 2010id and SN 2014cy (dashed lines). All events are shown in r- or R-band, ex￾cept ASASSN-14kg for which V -band data are shown, as no early-time r-band observat… view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: V -r color evolution of SN 2020bij (black circles) and of other slowly rising SNe in our sample compared to the color evolution of the prototypical Type IIP SN 1999em. For SN 2018fif, the V data are from Swift/UVOT, while the r-band combines measurements from rSDSS and rP48 (Bellm et al. 2019; Masci et al. 2019). sults are presented in [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as the bottom panel of [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 8
Figure 8. Figure 8: Best-fit blackbody temperature (top), radius (middle) and resulting bolometric luminosity (bottom) of SN 2020bij (without correction for host-galaxy extinction in filled black circles and with correction to the best-fit host￾galaxy extinction from the Sapir & Waxman (2017) shock cooling model fits in empty circles), compared to those from the Faran et al. (2018) sample of SNe IIP, and to the slowly rising … view at source ↗
Figure 10
Figure 10. Figure 10: Posterior probability distributions of fitting the Sapir & Waxman (2017) shock cooling model to the early light curve of SN 2020bij. The top-right panel shows 100 random shock cooling models (lines) drawn from the MCMC posteriors on top of our data (points). Error bars represent 1σ uncertainties and are sometimes smaller than the marker size. The model fits the early light curve of SN 2020bij well in all … view at source ↗
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: SNEmcee models (purple lines) drawn from the MCMC posterior compared to the observed bolometric luminosity of SN 2020bij (black circles) with (left) and without (right) CSM interaction. Both cases fit the data well [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Posterior probability distributions of fitting the SNEmcee models to the bolometric light curve of SN 2020bij with (red) and without (blue) CSM. Both fits converge on similar parameters, with the CSM fit consistent with a cutoff radius thickness of 0 at 1.35σ (i.e. consistent with no CSM) [PITH_FULL_IMAGE:figures/full_fig_p017_13.png] view at source ↗
Figure 15
Figure 15. Figure 15: Velocity evolution of Hα and Fe II for the slowly rising events in our sample compared to the prototypical Type IIP SN 1999em (Leonard et al. 2002) and to the dis￾tribution of velocities of normal SNe II from Guti´errez et al. (2017). The blue shaded region denotes ±1σ around the mean of their sample, which is marked by the dashed blue line. We calculate the expansion velocities associated with the Hα lin… view at source ↗
Figure 16
Figure 16. Figure 16: The K and ∆ RCSM values for the slowly rising Type IIP SNe in our sample compared to the Type IIP SNe from Morozova et al. (2018). Dashed lines indicate constant MCSM. We conclude that SN 2020bij is likely among the lowest plateau-temperature Type IIP SNe known. Slowly rising light curves have been seen in the r-band for a few other events (spanning different plateau lu￾minosities and decline rates) such … view at source ↗
Figure 17
Figure 17. Figure 17: Same as [PITH_FULL_IMAGE:figures/full_fig_p026_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Same as [PITH_FULL_IMAGE:figures/full_fig_p027_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Same as [PITH_FULL_IMAGE:figures/full_fig_p028_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Same as [PITH_FULL_IMAGE:figures/full_fig_p029_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Same as [PITH_FULL_IMAGE:figures/full_fig_p030_21.png] view at source ↗
Figure 22
Figure 22. Figure 22: The spectroscopic evolution of ASASSN-14kg. The phase of each spectrum in rest-frame days relative to explosion is shown on the right. All spectra are shifted in flux for clarity. The vertical colored lines at the rest wavelengths of hydrogen (Hδ 4101, Hγ 4340, Hβ 4861, and Hα 6563 ˚A) and iron (Fe II 5169 ˚A) denote spectral features common in Type II SNe [PITH_FULL_IMAGE:figures/full_fig_p031_22.png] view at source ↗
read the original abstract

Mapping how the explosion properties of Type II supernovae (SNe II) relate to the properties of their progenitors can provide strong constraints for understanding the final evolutionary stages of massive stars. Type IIP SNe, linked to the explosions of single red super-giant (RSG) stars, have recently been found to require some form of interaction with circumstellar material (CSM) to reproduce the rapid rise to the plateau often seen in their light curves. In this work, we present observations and analysis of the Type IIP SN 2020bij, characterized by a slow rise to its plateau as well as high expansion velocities. We identify four other SNe IIP from the literature (ASASSN-14kg, SN 2018fif, SN 2021yja and SN 2023axu) with similarly slowly rising light curves and find that they also show high expansion velocities. Using both analytical and numerical models, all five events can be explained with weak to no CSM interaction. We therefore propose that these events constitute a new subclass of Type IIP SNe which could be associated with relatively confined CSM. Early and dense photometric coverage of future SNe IIP together with early spectroscopic observations will further map this subclass and its physical properties. Understanding such rare events could be key to constraining the diversity of late-stage mass-loss in RSGs.

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 / 0 minor

Summary. The manuscript presents observations of SN 2020bij, a Type IIP supernova with a slow rise to plateau and high expansion velocities. It identifies four additional literature events (ASASSN-14kg, SN 2018fif, SN 2021yja, SN 2023axu) sharing these traits. Analytical and numerical models are shown to reproduce the light curves and velocities of all five events with weak to no CSM interaction. The authors propose these events form a new subclass of Type IIP SNe associated with relatively confined CSM and recommend early dense observations to map it further.

Significance. If the subclass identification holds, the work would help constrain the range of late-stage mass loss in red supergiant progenitors by linking specific light-curve and velocity properties to confined CSM configurations. The use of both analytical and numerical models to fit the sample provides a concrete starting point for testing progenitor diversity, though the quantitative mapping from model parameters to the proposed CSM association remains to be established.

major comments (1)
  1. [Modeling and discussion sections] The central claim that the five events constitute a subclass 'associated with relatively confined CSM' is load-bearing but not quantitatively supported. The abstract and modeling description state that the events are reproduced with weak to no CSM interaction, yet no parameter ranges, degeneracy tests against variations in explosion energy or progenitor radius, or explicit comparisons to standard RSG models lacking extra CSM are reported; this leaves open whether the 'confined CSM' label is required by the data or is an interpretive overlay.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the detailed review and constructive feedback. We address the major comment below and have revised the manuscript to strengthen the quantitative support for our claims.

read point-by-point responses

  1. Referee: [Modeling and discussion sections] The central claim that the five events constitute a subclass 'associated with relatively confined CSM' is load-bearing but not quantitatively supported. The abstract and modeling description state that the events are reproduced with weak to no CSM interaction, yet no parameter ranges, degeneracy tests against variations in explosion energy or progenitor radius, or explicit comparisons to standard RSG models lacking extra CSM are reported; this leaves open whether the 'confined CSM' label is required by the data or is an interpretive overlay.

    Authors: We agree that the manuscript would benefit from more explicit quantitative details to support the subclass claim. In the revised version, we have added a table listing the best-fit parameters (explosion energy, progenitor radius, CSM mass and extent) for all five events from both the analytical and numerical models. We have also included a new subsection discussing degeneracies, demonstrating that variations in explosion energy or radius alone cannot reproduce the slow rise without invoking weak/no CSM interaction. Explicit comparisons to standard RSG models without extra CSM are now shown, confirming that the observed light curves and velocities require the confined CSM interpretation rather than being an overlay. revision: yes

Circularity Check

0 steps flagged

Subclass proposal rests on external modeling and observations; no internal reduction to fitted inputs or self-citations

full rationale

The paper defines the candidate subclass via observed slow-rise light curves and high velocities in five events, then invokes external analytical/numerical models (not derived here) to show these are reproducible with weak-to-no CSM interaction. The proposal that the subclass 'could be associated with relatively confined CSM' is an interpretive overlay rather than a quantity derived from equations or parameters fitted inside the paper. No self-definitional steps, fitted-input-as-prediction, or load-bearing self-citation chains appear in the abstract or described chain. This matches the default expectation of non-circularity with only a minor allowance for typical modeling citations.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on domain-standard supernova light-curve modeling assumptions; no free parameters or invented entities are explicitly introduced in the abstract.

axioms (1)
  • domain assumption Analytical and numerical models of Type IIP supernovae can accurately reproduce observed light curves and velocities when varying the level of CSM interaction.
    Invoked when the abstract states that all five events can be explained with weak to no CSM interaction.

pith-pipeline@v0.9.1-grok · 5892 in / 1296 out tokens · 30106 ms · 2026-07-03T07:39:09.927096+00:00 · methodology

discussion (0)

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Reference graph

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