SN 2023rve: A Type II Supernova with No Nebular Oxygen
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 ± 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 ± 0.02 mag/50 days during the plateau. The bolometric light curve implies a 56Ni mass of 0.0064 M⊙. Using hydrodynamic light-curve modeling, we infer an intermediate-mass progenitor (∼14−18 M⊙), a low explosion energy of 0.27×1051 ergs, and a dense CSM component with radial extent of 2900 R⊙ and density parameter of 1018 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.
Versions
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BibTeX
@misc{rosowsky20262023rve,
title = {{SN 2023rve: A Type II Supernova with No Nebular Oxygen}},
author = {Melissa Rosowsky and Stefano Valenti and Aravind P. Ravi and Yize Dong and Nicolas Meza Retamal and K. Azalee Bostroem and David J. Sand and Griffin Hosseinzadeh and Jeniveve Pearson and Anders Jerkstrand and Darshana Mehta and Jennifer E. Andrews and Moira Andrews and Joseph Farah and Emily Hoang and D. Andrew Howell and Daryl Janzen and Saurabh W. Jha and Michael Lundquist and Curtis McCully and Megan Newsome and Estefania Padilla Gonzalez and Manisha Shrestha and Giacomo Terreran},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2606.30979},
eprint = {2606.30979},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.30979},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - SN 2023rve: A Type II Supernova with No Nebular Oxygen
AU - Melissa Rosowsky
AU - Stefano Valenti
AU - Aravind P. Ravi
AU - Yize Dong
AU - Nicolas Meza Retamal
AU - K. Azalee Bostroem
AU - David J. Sand
AU - Griffin Hosseinzadeh
AU - Jeniveve Pearson
AU - Anders Jerkstrand
AU - Darshana Mehta
AU - Jennifer E. Andrews
AU - Moira Andrews
AU - Joseph Farah
AU - Emily Hoang
AU - D. Andrew Howell
AU - Daryl Janzen
AU - Saurabh W. Jha
AU - Michael Lundquist
AU - Curtis McCully
AU - Megan Newsome
AU - Estefania Padilla Gonzalez
AU - Manisha Shrestha
AU - Giacomo Terreran
PY - 2026
DA - 2026/09/29
PB - arXiv
DO - 10.48550/arxiv.2606.30979
UR - https://arxiv.org/abs/2606.30979
AB - 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 ± 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 ± 0.02 mag/50 days during the plateau. The bolometric light curve implies a ^56Ni mass of 0.0064 M_⊙. Using hydrodynamic light-curve modeling, we infer an intermediate-mass progenitor (∼14−18 M_⊙), a low explosion energy of 0.27×10^51 ergs, and a dense CSM component with radial extent of 2900 R_⊙ and density parameter 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.
ER -