The Astrophysical Journal (Jan 2024)

SN 2022oqm: A Bright and Multipeaked Calcium-rich Transient

  • S. Karthik Yadavalli,
  • V. Ashley Villar,
  • Luca Izzo,
  • Yossef Zenati,
  • Ryan J. Foley,
  • J. Craig Wheeler,
  • Charlotte R. Angus,
  • Dominik Bánhidi,
  • Katie Auchettl,
  • Barna Imre Bíró,
  • Attila Bódi,
  • Zsófia Bodola,
  • Thomas de Boer,
  • Kenneth C. Chambers,
  • Ryan Chornock,
  • David A. Coulter,
  • István Csányi,
  • Borbála Cseh,
  • Srujan Dandu,
  • Kyle W. Davis,
  • Connor Braden Dickinson,
  • Diego Farias,
  • Joseph Farah,
  • Christa Gall,
  • Hua Gao,
  • D. Andrew Howell,
  • Wynn V. Jacobson-Galan,
  • Nandita Khetan,
  • Charles D. Kilpatrick,
  • Réka Könyves-Tóth,
  • Levente Kriskovics,
  • Natalie LeBaron,
  • Kayla Loertscher,
  • X. K. Le Saux,
  • Raffaella Margutti,
  • Eugene A. Magnier,
  • Curtis McCully,
  • Peter McGill,
  • Hao-Yu Miao,
  • Megan Newsome,
  • Estefania Padilla Gonzalez,
  • András Pál,
  • Boróka H. Pál,
  • Yen-Chen Pan,
  • Collin A. Politsch,
  • Conor L. Ransome,
  • Enrico Ramirez-Ruiz,
  • Armin Rest,
  • Sofia Rest,
  • Olivia Robinson,
  • Huei Sears,
  • Jackson Scheer,
  • Ádám Sódor,
  • Jonathan Swift,
  • Péter Székely,
  • Róbert Szakáts,
  • Tamás Szalai,
  • Kirsty Taggart,
  • Giacomo Terreran,
  • Padma Venkatraman,
  • József Vinkó,
  • Grace Yang,
  • Henry Zhou

DOI
https://doi.org/10.3847/1538-4357/ad5a7c
Journal volume & issue
Vol. 972, no. 2
p. 194

Abstract

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We present the photometric and spectroscopic evolution of SN 2022oqm, a nearby multipeaked hydrogen- and helium-weak calcium-rich transient (CaRT). SN 2022oqm was detected 13.1 kpc from its host galaxy, the face-on spiral galaxy NGC 5875. Extensive spectroscopic coverage reveals an early hot ( T ≥ 40,000 K) continuum and carbon features observed ∼1 day after discovery, SN Ic-like photospheric-phase spectra, and strong forbidden calcium emission starting 38 days after discovery. SN 2022oqm has a relatively high peak luminosity ( M _B = −17 mag) for CaRTs, making it an outlier in the population. We determine that three power sources are necessary to explain the light curve (LC), with each corresponding to a distinct peak. The first peak is powered by an expanding blackbody with a power-law luminosity, suggesting shock cooling by circumstellar material (CSM). Subsequent LC evolution is powered by a double radioactive decay model, consistent with two sources of photons diffusing through optically thick ejecta. From the LC, we derive an ejecta mass and ^56 Ni mass of ∼0.6 M _⊙ and ∼0.09 M _⊙ . Spectroscopic modeling ∼0.6 M _⊙ of ejecta, and with well-mixed Fe-peak elements throughout. We discuss several physical origins for SN 2022oqm and find either a surprisingly massive white dwarf progenitor or a peculiar stripped envelope model could explain SN 2022oqm. A stripped envelope explosion inside a dense, hydrogen- and helium-poor CSM, akin to SNe Icn, but with a large 56Ni mass and small CSM mass could explain SN 2022oqm. Alternatively, helium detonation on an unexpectedly massive white dwarf could also explain SN 2022oqm.

Keywords