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PreprintCC BY 4.0arXiv

SN 2019cqc: A Hydrogen-rich Superluminous Supernova Showing Electron-Scattering Signatures

  • Dinesh Hebbar
  • Rupak Roy
  • Matt Nicholl
  • Jesper Sollerman
  • Joseph P Anderson
  • Mariusz Gromadzki
  • D. Andrew Howell
  • Tuomas Kangas
  • Seppo Mattila
  • Daichi Hiramatsu
  • Avishay Gal-Yam
  • Edo Berger
6 more authors
  • K. Azalee Bostroem
  • Ting-Wan Chen
  • Joseph Farah
  • Sebastian Gomez
  • Curtis McCully
  • Jeonghee Rho
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Abstract

Hydrogen-rich superluminous supernovae without narrow emission lines (SLSNe-II) are rare transients whose powering mechanisms remain debated, particularly the role of circumstellar medium (CSM) interaction. We present photometric and spectroscopic observations of SN 2019cqc to investigate its power source and progenitor mass loss. We model the lightcurve using MOSFiT with the csm and csmni models to constrain the explosion and CSM parameters. SN 2019cqc peaked at Mg = −20.21 ± 0.07 and emitted ∼ 1.7 × 1050 erg of energy in the form of radiation. Photometric and spectroscopic modeling indicates that CSM interaction dominates in both scenarios, with best-fit CSM and ejecta masses of ∼ 4.5 M⊙ and ∼ 32 M⊙, respectively. The inferred CSM properties imply an extreme eruptive mass loss at a rate of ∼ 0.2−−0.3 M⊙ yr−1 in the years preceding the core collapse, consistent with a variable progenitor of luminous blue variable progenitor. We observe a persistent blueshifted asymmetry in the Hα emission line. At early times (≲ +110~d), this is attributed to electron scattering with bulk Velocity of ejecta, while the profile at late epochs (≳ +402~d onward) suggests the subsequent formation of dust in the ejecta. Additionally, we identify a distinct, short-lived feature at ∼ 4600 Å , likely a blend of ionized C III/N III lines powered by the interaction of the SN-shock with the extended atmosphere.

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Cite

BibTeXRIS
BibTeX
@misc{hebbar20262019cqc,
  title = {{SN 2019cqc: A Hydrogen-rich Superluminous Supernova Showing Electron-Scattering Signatures}},
  author = {Dinesh Hebbar and Rupak Roy and Matt Nicholl and Jesper Sollerman and Joseph P Anderson and Mariusz Gromadzki and D. Andrew Howell and Tuomas Kangas and Seppo Mattila and Daichi Hiramatsu and Avishay Gal-Yam and Edo Berger and K. Azalee Bostroem and Ting-Wan Chen and Joseph Farah and Sebastian Gomez and Curtis McCully and Jeonghee Rho},
  howpublished = {arXiv},
  year = {2026},
  month = aug,
  doi = {10.48550/arxiv.2608.30309},
  eprint = {2608.30309},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2608.30309},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - SN 2019cqc: A Hydrogen-rich Superluminous Supernova Showing Electron-Scattering Signatures
AU  - Dinesh Hebbar
AU  - Rupak Roy
AU  - Matt Nicholl
AU  - Jesper Sollerman
AU  - Joseph P Anderson
AU  - Mariusz Gromadzki
AU  - D. Andrew Howell
AU  - Tuomas Kangas
AU  - Seppo Mattila
AU  - Daichi Hiramatsu
AU  - Avishay Gal-Yam
AU  - Edo Berger
AU  - K. Azalee Bostroem
AU  - Ting-Wan Chen
AU  - Joseph Farah
AU  - Sebastian Gomez
AU  - Curtis McCully
AU  - Jeonghee Rho
PY  - 2026
DA  - 2026/08/31
PB  - arXiv
DO  - 10.48550/arxiv.2608.30309
UR  - https://arxiv.org/abs/2608.30309
AB  - Hydrogen-rich superluminous supernovae without narrow emission lines (SLSNe-II) are rare transients whose powering mechanisms remain debated, particularly the role of circumstellar medium (CSM) interaction. We present photometric and spectroscopic observations of SN 2019cqc to investigate its power source and progenitor mass loss. We model the lightcurve using MOSFiT with the csm and csmni models to constrain the explosion and CSM parameters. SN 2019cqc peaked at M_g = −20.21 ± 0.07 and emitted ∼ 1.7 × 10^50 erg of energy in the form of radiation. Photometric and spectroscopic modeling indicates that CSM interaction dominates in both scenarios, with best-fit CSM and ejecta masses of ∼ 4.5 M_⊙ and ∼ 32 M_⊙, respectively. The inferred CSM properties imply an extreme eruptive mass loss at a rate of ∼ 0.2−−0.3 M_⊙ yr^−1 in the years preceding the core collapse, consistent with a variable progenitor of luminous blue variable progenitor. We observe a persistent blueshifted asymmetry in the Hα emission line. At early times (≲ +110~d), this is attributed to electron scattering with bulk Velocity of ejecta, while the profile at late epochs (≳ +402~d onward) suggests the subsequent formation of dust in the ejecta. Additionally, we identify a distinct, short-lived feature at ∼ 4600 Å , likely a blend of ionized C III/N III lines powered by the interaction of the SN-shock with the extended atmosphere.
ER  -