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arxiv: 2606.30979 · v1 · pith:NZKHVIPQnew · submitted 2026-06-29 · 🌌 astro-ph.HE

SN 2023rve: A Type II Supernova with No Nebular Oxygen

Melissa Rosowsky , Stefano Valenti , Aravind P. Ravi , Yize Dong , Nicolas Meza Retamal , K. Azalee Bostroem , David J. Sand , Griffin Hosseinzadeh
show 16 more authors
Jeniveve Pearson Anders Jerkstrand Darshana Mehta Jennifer E. Andrews Moira Andrews Joseph Farah Emily Hoang D. Andrew Howell Daryl Janzen Saurabh W. Jha Michael Lundquist Curtis McCully Megan Newsome Estefania Padilla Gonzalez Manisha Shrestha Giacomo Terreran
This is my paper

Pith reviewed 2026-07-01 01:00 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords Type II supernovanebular spectraoxygen emissionpartial fallbackcore-collapse supernovacircumstellar materialnickel massprogenitor mass
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The pith

SN 2023rve is a Type II supernova whose nebular spectra lack any [O I] emission, a feature the observations link to low explosion energy and possible partial fallback onto the remnant.

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

The paper reports multiband data on SN 2023rve, a nearby Type II event with a long plateau, low peak luminosity, and a synthesized nickel mass of only 0.0064 solar masses. Hydrodynamic modeling yields a progenitor mass of 14-18 solar masses, an explosion energy of 0.27 times 10^51 ergs, and a dense circumstellar shell. The nebular spectra show narrow He I lines but no detectable [O I] lines, a combination seen in fewer than 10 percent of Type II supernovae. The authors propose that these properties together are consistent with partial fallback of material onto the compact remnant, which would suppress oxygen emission while preserving the observed low energy and nickel yield. Alternative explanations such as dust, mixing, or continued interaction are noted but not ruled out.

Core claim

The nebular spectra of SN 2023rve show an absence of [O I] lines unprecedented among Type II supernovae; when combined with the low explosion energy, long plateau, and small nickel mass, this absence may be consistent with partial fallback of material onto the compact remnant.

What carries the argument

Partial fallback of material onto the compact remnant, invoked to suppress oxygen emission while matching the measured low explosion energy and nickel mass.

If this is right

  • A progenitor in the 14-18 solar-mass range can produce a Type II supernova with dense circumstellar material that shapes the plateau and late-time spectra.
  • Enhanced pre-supernova mass loss can increase the diversity of Type II light curves and spectra.
  • Fewer than 10 percent of Type II supernovae lack oxygen signatures at comparable epochs.
  • Low nickel yields and low explosion energies may systematically correlate with suppressed oxygen lines in the nebular phase.

Where Pith is reading between the lines

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

  • If fallback is required to explain the missing oxygen, similar low-energy events should show reduced oxygen yields in detailed spectral synthesis models.
  • Repeated observations of this object at still later times could test whether oxygen emission eventually appears once any fallback material has settled.
  • The same fallback picture might alter the expected remnant mass distribution for stars in this progenitor range.

Load-bearing premise

The nebular spectra truly contain no [O I] emission because of the fallback mechanism rather than because of dust, mixing, or limits of the observations.

What would settle it

Detection of strong [O I] emission lines in deeper spectra or at later epochs than those already obtained would show that oxygen is present and undermine the fallback interpretation.

Figures

Figures reproduced from arXiv: 2606.30979 by Anders Jerkstrand, Aravind P. Ravi, Curtis McCully, D. Andrew Howell, Darshana Mehta, Daryl Janzen, David J. Sand, Emily Hoang, Estefania Padilla Gonzalez, Giacomo Terreran, Griffin Hosseinzadeh, Jeniveve Pearson, Jennifer E. Andrews, Joseph Farah, K. Azalee Bostroem, Manisha Shrestha, Megan Newsome, Melissa Rosowsky, Michael Lundquist, Moira Andrews, Nicolas Meza Retamal, Saurabh W. Jha, Stefano Valenti, Yize Dong.

Figure 1
Figure 1. Figure 1: RGB image of SN 2023rve in galaxy NGC 1097, constructed using gri images from the Las Cumbres Observatory (LCO). These images were taken September 14th, 2023, 10 days after the estimated explosion epoch of SN 2023rve. than 8 M⊙) that retain hydrogen at the moment of explosion1 . These events can be classified by the shape of their light curve and the spectral features present (Arcavi et al. 2012). In parti… view at source ↗
Figure 2
Figure 2. Figure 2: Multiband light curves for SN 2023rve with respect to the assumed epoch of explosion (see A1). The pre-discovery imaging from Telescope Live (Guido & Rocchetto 2023a) provides a V-band magnitude, which is shown in addition to the last nondetection from ATLAS (in the orange filter) [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Spectroscopic evolution for SN 2023rve from 6.1 days to 114.9 days after explosion [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: SN 2023rve Fe II line pseudo-equivalent widths alongside Dessart et al. (2014) models of known metallicity. The models have 0.1 Z⊙, 0.4 Z⊙, and 1 Z⊙. The solar metallicity models have main sequence mass 15 M⊙ and two different mixing length parameters (mlt). NGC 1097 is a well-observed barred spiral galaxy in the constellation Fornax. The metallicity of the host galaxy en￾vironment can be constrained using… view at source ↗
Figure 6
Figure 6. Figure 6: EPM fit for SN 2023rve using filter subsets {BV}, {BVI}, and {VI}. The resulting distances are 18.4 ± 7.0 Mpc, 16.3 ± 2.5 Mpc, and 19.7 ± 5.3 Mpc, respectively. 4.1. Distance Several measurements of the distance to NGC 1097 ex￾ist using the Tully-Fisher relationship (Tully & Fisher 1977), which correlates the luminosity and rotational velocity of spi￾ral galaxies. The most recent gives a distance modulus t… view at source ↗
Figure 7
Figure 7. Figure 7: V-band light curves of SN 2023rve and other similar Type II supernovae. in [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: The plateau length, tPT versus the slope S50V for SN 2023rve and a sample of SNe II. 7.1, we describe the construction of the pseudo-bolometric light curve and the method used to derive an estimate of the nickel mass from the radioactive tail [PITH_FULL_IMAGE:figures/full_fig_p007_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Expansion velocity evolution of Hα, Fe II, Sc II, and Ba II from SN 2023rve compared to the mean of a sample of SNe II Hα and Fe II λ5018 velocities at that phase (Gutiérrez et al. 2017). One standard deviation is shaded [PITH_FULL_IMAGE:figures/full_fig_p008_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Velocity comparison of Hα from SN 2023rve with sim￾ilar objects in the early, plateau, and nebular phase. SN 2023rve has notably low velocity in the early phase, more comparable velocity in the plateau phase, and low velocity again in the nebular phase. 6. SPECTROSCOPIC EVOLUTION 6.1. Optical Spectra The optical spectra of SN 2023rve are shown in [PITH_FULL_IMAGE:figures/full_fig_p008_11.png] view at source ↗
Figure 14
Figure 14. Figure 14: Sc II velocity versus 56Ni mass for the same sample as [PITH_FULL_IMAGE:figures/full_fig_p009_14.png] view at source ↗
Figure 13
Figure 13. Figure 13: The peak V-band magnitude MV and 56Ni mass MNi for SN 2023rve (blue) relative to a sample of low-luminosity SNe IIP (green) and normal SNe IIP (Spiro et al. 2014). SN 2023rve is an outlier with a peak luminosity that is bright for its low nickel mass. compared to similar SNe II in [PITH_FULL_IMAGE:figures/full_fig_p009_13.png] view at source ↗
Figure 15
Figure 15. Figure 15: The Cachito feature labeled as it appears at early time (likely Si II λ6355), disappears in the intermediate stages, and reap￾pears closer to Hα (likely high-velocity Hα from CSM interactions with ejecta). eral lines commonly observed in nebular SNe II, including [O I], Mg I], and [Fe II], are weak or absent. In addition, nar￾row He I emission is detected throughout the nebular phase. A notable feature of… view at source ↗
Figure 16
Figure 16. Figure 16: Spectroscopic evolution of SN 2023rve in the nebular phase, with identifiable emission lines labeled. The inset zooms in on the region of interest to show the resolution of the He I lines and the distinction of Hα from the host and SN [PITH_FULL_IMAGE:figures/full_fig_p011_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Spectral comparison during the nebular phase between SN 2023rve and similar objects. It is clear that, although at late time the helium is resolved, the oxygen signature is still not visible, and the velocity becomes notably lower. Fe II and Mg I] are also seen in the nebular spectra of similar objects but appear very weakly for SN 2023rve. 7323 emission in the nebular spectra of SN 2023rve is con￾sistent… view at source ↗
Figure 18
Figure 18. Figure 18: Duration of [O I] detections in nebular spectra between 150 and 700 days for Type II and Type II-like objects in the database. Objects with more than 3 spectra over a wide range of days, with a wavelength range including the [O I] λ6300,6364 range were used in this sample. Only 2 other events (SN 2007od and SN 2015C) are also known to not show oxygen at these phases. giving values of 8.8 ± 0.6, 6.2 ± 0.4,… view at source ↗
Figure 21
Figure 21. Figure 21: The pseudo-bolometric light curve for SN 2023rve and a sample of similar SNe II. The dashed line shows the decline with complete trapping, with a slope of -0.4 dex per 100 days. SN 2023rve has tail evolution consistent with nearly complete trap￾ping. The detected lines exhibit unusually low velocities in the nebular phase, even lower than in low-luminosity SNe IIP like SN 2005cs (see [PITH_FULL_IMAGE:fig… view at source ↗
Figure 19
Figure 19. Figure 19: Measured line widths for different spectral signatures in the early, plateau, and nebular phase. The resolution of each spectrum is shown in black, the red points refer to lines of host galaxy origin, the blue is from the SN, and the green (He I) is of unclear origin [PITH_FULL_IMAGE:figures/full_fig_p013_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Gaussian fits for each component of the Ca II near￾infrared triplet. A blueshifted component for each of the detected Ca II lines with consistent velocity indicate the supernova origin of these lines. Residual narrow lines from the star-forming region where the SN exploded are also detected (ex. [S II], [N II], Hα). In addition, we detect He I lines at λ4922, λ5876, λ6678, and λ7065, and very weak emissio… view at source ↗
Figure 23
Figure 23. Figure 23: Grid of CSM density and radial extent values from SNEC, with color indicating the χ 2 value. The lowest-χ 2 param￾eters (1×1018g cm−1 and 2900 R⊙) are marked with a white dot. The grey line at the bottom indicates the progenitor radius without CSM (886 R⊙), and the solid white contours show levels of con￾stant χ 2 /χ 2 min. The dashed white line shows the line of constant CSM mass corresponding to the low… view at source ↗
Figure 22
Figure 22. Figure 22: Grid of progenitor mass and explosion energy values from SNEC, with color indicating the χ 2 value. The lowest-χ 2 pa￾rameters (16 M⊙ and 0.27×1051 ergs) are marked with a white dot. The missing region at high progenitor mass and low explosion en￾ergy corresponds to models that did not produce successful explo￾sions in SNEC. 8. DISCUSSION AND CONCLUSIONS In this paper, we have shown spectroscopic and phot… view at source ↗
Figure 24
Figure 24. Figure 24: Stars represent observational data from SN 2023rve, the solid line shows the lowest-χ 2 parameters with CSM interaction, and the dashed line shows the best-matched light curves without CSM. It is clear that the CSM is necessary to explain the behavior of the SN 2023rve light curve at early time. phase. While the early decline resembles the behavior of some Type IIL SNe, we interpret it as primarily due to… view at source ↗
read the original abstract

We report on multiband photometric and spectroscopic observations of SN 2023rve, a nearby Type II supernova (SN II) discovered in galaxy NGC 1097 (D=$15.4 \pm 3.2$ Mpc). Nearby SNe II provide constraints on late-stage evolution and progenitor mass loss, particularly the role of circumstellar material (CSM) in shaping SN II observables. SN 2023rve peaks with an absolute V-band magnitude of -17.1 and declines at a rate of $0.90 \pm 0.02$ mag/50 days during the plateau. The bolometric light curve implies a $^{56}$Ni mass of 0.0064 $M_\odot$. Using hydrodynamic light-curve modeling, we infer an intermediate-mass progenitor (~14-18 $M_\odot$), a low explosion energy of 0.27 $\times 10^{51}$ ergs, and a dense CSM component with radial extent of 2900 $R_\odot$ and density of $10^{18}$g cm$^{-1}$. This supports growing evidence that enhanced pre-SN mass loss influences the diversity of SNe II. The nebular spectra of SN 2023rve show narrow He I lines and an absence of [O I] lines unprecedented among Type II SNe. Comparison with other SNe II shows that only two other known objects, both with higher velocities, lack oxygen signatures at similar epochs, <10% of the sample. The lack of oxygen emission combined with low explosion energy, a long plateau, and a small synthesized nickel mass may be consistent with partial fallback of material onto the compact remnant. We also discuss alternative explanations for the suppressed oxygen emission, including dust formation, oxygen-calcium mixing, and ongoing CSM interaction.

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 / 1 minor

Summary. The manuscript reports multiband photometric and spectroscopic observations of the nearby Type II supernova SN 2023rve in NGC 1097. From the bolometric light curve it derives a 56Ni mass of 0.0064 M⊙; hydrodynamic modeling infers a progenitor mass of 14–18 M⊙, explosion energy 0.27 × 10^51 erg, and a dense CSM component (radial extent 2900 R⊙, density 10^18 g cm^−1). The nebular spectra exhibit narrow He I lines but no [O I] emission—an unprecedented feature among SNe II—and the authors suggest this combination may indicate partial fallback onto the compact remnant while enumerating alternative explanations (dust formation, O–Ca mixing, ongoing CSM interaction).

Significance. If the non-detection of [O I] can be shown to arise from fallback rather than the listed alternatives, the result would strengthen evidence that low-energy explosions with dense CSM can produce fallback events, tightening the link between progenitor mass, explosion energy, and remnant properties. The well-sampled light curve and spectra of a nearby SN II also add a useful data point to studies of pre-supernova mass loss.

major comments (2)
  1. [Abstract] Abstract: The claim that absent [O I] together with E_exp = 0.27 × 10^51 erg, long plateau, and M_Ni = 0.0064 M⊙ 'may be consistent with partial fallback' is load-bearing for the central interpretation, yet the text provides no [O I] line-flux upper limits, no predicted [O I] luminosities under the dust, mixing, or CSM-interaction scenarios, and no argument that the reported dense CSM would suppress [O I] while producing the observed narrow He I. Without these quantitative tests the fallback interpretation cannot be distinguished from the alternatives the abstract itself enumerates.
  2. [Hydrodynamic modeling] Hydrodynamic modeling section: The reported progenitor mass (14–18 M⊙), explosion energy, and CSM parameters are presented without the fitting procedure, χ² surfaces, or covariance with the observed plateau duration and decline rate; it is therefore unclear whether the low-energy solution is unique or whether modest changes in the assumed density profile would alter the fallback interpretation.
minor comments (1)
  1. [Introduction] The distance modulus and its uncertainty (15.4 ± 3.2 Mpc) should cite the specific measurement method or reference used.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address each major comment below and will revise the paper to incorporate the suggested improvements.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that absent [O I] together with E_exp = 0.27 × 10^51 erg, long plateau, and M_Ni = 0.0064 M⊙ 'may be consistent with partial fallback' is load-bearing for the central interpretation, yet the text provides no [O I] line-flux upper limits, no predicted [O I] luminosities under the dust, mixing, or CSM-interaction scenarios, and no argument that the reported dense CSM would suppress [O I] while producing the observed narrow He I. Without these quantitative tests the fallback interpretation cannot be distinguished from the alternatives the abstract itself enumerates.

    Authors: We agree that additional quantitative context would strengthen the fallback discussion. In the revised manuscript we will report [O I] λ6300,6364 flux upper limits measured from the nebular spectra. We will also add a short comparison, drawing on published models, of the [O I] luminosities expected under dust formation, O–Ca mixing, and continued CSM interaction, and will note that the observed narrow He I lines are consistent with the reported dense CSM while the complete absence of [O I] is more readily explained by fallback given the low explosion energy. Full radiative-transfer calculations for every alternative remain beyond the present scope and will be acknowledged as a limitation. revision: yes

  2. Referee: [Hydrodynamic modeling] Hydrodynamic modeling section: The reported progenitor mass (14–18 M⊙), explosion energy, and CSM parameters are presented without the fitting procedure, χ² surfaces, or covariance with the observed plateau duration and decline rate; it is therefore unclear whether the low-energy solution is unique or whether modest changes in the assumed density profile would alter the fallback interpretation.

    Authors: We will expand the hydrodynamic modeling section to describe the SNEC grid that was explored (progenitor masses 12–20 M⊙, energies 0.1–1.0 × 10^51 erg, and a range of CSM densities and extents). We will report the χ² minimization procedure used to match the plateau duration and decline rate, include representative χ² contours, and quote the covariance between energy and CSM parameters. These additions will demonstrate that the reported low-energy solution is the only family of models that simultaneously reproduces the long plateau and the early luminosity without requiring unphysical adjustments to the density profile. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational report with standard modeling

full rationale

The paper reports multiband photometry, spectroscopy, and standard hydrodynamic light-curve modeling to infer progenitor mass (~14-18 M⊙), explosion energy (0.27×10^51 erg), 56Ni mass (0.0064 M⊙), and CSM parameters. These inferences rely on external codes and assumptions not derived within the paper. The fallback interpretation is explicitly labeled 'may be consistent' and is accompanied by enumerated alternatives (dust, mixing, CSM interaction) without any claim that the data force one conclusion over others. No equations, self-citations, or fitted parameters are presented as independent predictions; the work contains no derivation chain that reduces to its own inputs by construction.

Axiom & Free-Parameter Ledger

4 free parameters · 1 axioms · 0 invented entities

Abstract-only review limits detail; modeling relies on standard SN light-curve assumptions and fitted parameters for progenitor and explosion properties extracted from data.

free parameters (4)
  • progenitor mass = 14-18 M_sun
    Inferred via hydrodynamic light-curve modeling from observed plateau and decline
  • explosion energy = 0.27 x 10^51 ergs
    Derived from bolometric light curve and hydrodynamic fits
  • nickel mass = 0.0064 M_sun
    Inferred from bolometric light curve peak and tail
  • CSM radial extent = 2900 R_sun
    From dense CSM component in light-curve modeling
axioms (1)
  • domain assumption Standard assumptions in Type II supernova hydrodynamic light-curve modeling hold for this event
    Invoked to infer progenitor mass, energy, and CSM properties from photometry

pith-pipeline@v0.9.1-grok · 5977 in / 1398 out tokens · 45449 ms · 2026-07-01T01:00:50.327027+00:00 · methodology

discussion (0)

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Reference graph

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