The Astrophysical Journal (Jan 2024)

Evidence of Weak Circumstellar Medium Interaction in the Type II SN 2023axu

  • Manisha Shrestha,
  • Jeniveve Pearson,
  • Samuel Wyatt,
  • David J. Sand,
  • Griffin Hosseinzadeh,
  • K. Azalee Bostroem,
  • Jennifer E. Andrews,
  • Yize Dong,
  • Emily Hoang,
  • Daryl Janzen,
  • Jacob E. Jencson,
  • Michael Lundquist,
  • Darshana Mehta,
  • Nicolás Meza Retamal,
  • Stefano Valenti,
  • Jillian C. Rastinejad,
  • Phil Daly,
  • Dallan Porter,
  • Joannah Hinz,
  • Skyler Self,
  • Benjamin Weiner,
  • G. Grant Williams,
  • Daichi Hiramatsu,
  • D. Andrew Howell,
  • Curtis McCully,
  • Estefania Padilla Gonzalez,
  • Craig Pellegrino,
  • Giacomo Terreran,
  • Megan Newsome,
  • Joseph Farah,
  • Koichi Itagaki,
  • Saurabh W. Jha,
  • Lindsey Kwok,
  • Nathan Smith,
  • Michaela Schwab,
  • Jeonghee Rho,
  • Yi Yang

DOI
https://doi.org/10.3847/1538-4357/ad11e1
Journal volume & issue
Vol. 961, no. 2
p. 247

Abstract

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We present high-cadence photometric and spectroscopic observations of SN 2023axu, a classical Type II supernova with an absolute V -band peak magnitude of –17.2 ± 0.1 mag. SN 2023axu was discovered by the Distance Less Than 40 Mpc (DLT40) survey within 1 day of the last nondetection in the nearby galaxy NGC 2283 at 13.7 Mpc. We modeled the early light curve using a recently updated shock cooling model that includes the effects of line blanketing and found the explosion epoch to be MJD 59971.48 ± 0.03 and the probable progenitor to be a red supergiant. The shock cooling model underpredicts the overall UV data, which point to a possible interaction with circumstellar material. This interpretation is further supported by spectral behavior. We see a ledge feature around 4600 Å in the very early spectra (+1.1 and +1.5 days after the explosion), which can be a sign of circumstellar interaction. The signs of circumstellar material are further bolstered by the presence of absorption features blueward of H α and H β at day >40, which is also generally attributed to circumstellar interaction. Our analysis shows the need for high-cadence early photometric and spectroscopic data to decipher the mass-loss history of the progenitor.

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