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 Banhidi, Katie Auchettl, Barna Imre Biro, Attila Bodi, Zsofia Bodola, Thomas de Boer, Kenneth C. Chambers, Ryan Chornock, David A. Coulter, Istvan Csanyi, Borbala Cseh, Srujan Dandu, Kyle W. DavisConnor Braden Dickinson, Diego Farias, Joseph Farah, Christa Gall, Hua Gao, D. Andrew Howell, Wynn V. Jacobson-Galan, Nandita Khetan, Charles D. Kilpatrick, Reka Konyves-Toth, 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, Andras Pal, Boroka H. Pal, Yen Chen Pan, Collin A. Politsch, Conor L. Ransome, Enrico Ramirez-Ruiz, Armin Rest, Sofia Rest, Olivia Robinson, Huei Sears, Jackson Scheer, Ádam Sodor, Jonathan Swift, Peter Szekely, Robert Szakats, Tamas Szalai, Kirsty Taggart, Giacomo Terreran, Padma Venkatraman, Jozsef Vinko, Grace Yang, Henry Zhou

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Abstract

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 56Ni 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.

Original languageEnglish (US)
Article number194
JournalAstrophysical Journal
Volume972
Issue number2
DOIs
StatePublished - Sep 1 2024

Funding

This project has been supported by the GINOP-2-3-2-15-2016-00033 project and the NKFIH/OTKA grants FK-134432 and K-142534 of the National Research, Development and Innovation (NRDI) Office of Hungary, partly funded by the European Union. T.S. is supported by the J\u00E1nos Bolyai Research Scholarship of the Hungarian Academy of Sciences, and by the New National Excellence Program (UNKP-22-5) of the Ministry for Culture and Innovation from the source of the NRDI Fund, Hungary. This project was supported by the KKP-137523 \u201CSeismoLab\u201D \u00C9lvonal grant of the Hungarian Research, Development and Innovation Office (NKFIH) and by the Lend\u00FClet Program of the Hungarian Academy of Sciences under project No. LP2018-7. We thank Ido Irani and Avishay Gal-Yam for insightful feedback on modeling this object and interpreting the progenitor system. We thank Greg Zeimann for help with HET data reduction and Dan Weisz for Kast observations. S. K. Yadavalli and V. A. Villar acknowledge support by the NSF through grant AST-2108676. Much of the photometry and spectroscopy presented here were acquired as part of the ongoing Young Supernova Experiment (Jones et al. 2021; Aleo et al. 2023) The Young Supernova Experiment (YSE) and its research infrastructure is supported by the European Research Council under the European Union\u2019s Horizon 2020 research and innovation program (ERC grant Agreement 101002652, PI K. Mandel), the Heising-Simons Foundation (2018-0913, PI R. Foley; 2018-0911, PI R. Margutti), NASA (NNG17PX03C, PI R. Foley), NSF (AST-1720756, AST-1815935, PI R. Foley; AST-1909796, AST-1944985, PI R. Margutti), the David & Lucille Packard Foundation (PI R. Foley), VILLUM FONDEN (project 16599, PI J. Hjorth), and the Center for AstroPhysical Surveys (CAPS) at the National Center for Supercomputing Applications (NCSA) and the University of Illinois Urbana-Champaign. J.C.W. and J.V. acknowledge the support from the NSF grant AST-1813825. W.J.-G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842165. W.J.-G. acknowledges support through NASA grants in support of Hubble Space Telescope program GO-16075 and 16500. C.D.K. is partly supported by a CIERA postdoctoral fellowship. D.A.C. acknowledges support from the National Science Foundation Graduate Research Fellowship under grant DGE1339067. C.R.A. was supported by a grant from VILLUM FONDEN (project No. 16599). D.F. is supported by a VILLUM FONDEN Young Investigator Grant (project No. 25501). This publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 108-2112-M-008-001. We additionally acknowledge the use of public data from the Swift data archive. This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near-earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen\u2019s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile. Y.Z. was partially supported by NASA TCAN and grant Nos. NNH17ZDA001N and TCAN-80NSSC18K1488. We acknowledge observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku, and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. This work makes use of observations from the Las Cumbres Observatory global telescope network. The LCO group is supported by NSF grants AST-1911225 and AST0-1911151, and NASA Swift grant 80NSSC19K1639. This research has made use of the Spanish Virtual Observatory ( https://svo.cab.inta-csic.es ) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. The work of the Spanish Virtual Observatory\u2019s Filter Profile Service has proven to be the backbone of using the proper filter bandpasses in proper photometric modeling. We cite them here (Rodrigo et al. ; Rodrigo & Solano ). We thank Ido Irani and Avishay Gal-Yam for insightful feedback on modeling this object and interpreting the progenitor system. We thank Greg Zeimann for help with HET data reduction and Dan Weisz for Kast observations. S. K. Yadavalli and V. A. Villar acknowledge support by the NSF through grant AST-2108676. Much of the photometry and spectroscopy presented here were acquired as part of the ongoing Young Supernova Experiment (Jones et al. ; Aleo et al. ) The Young Supernova Experiment (YSE) and its research infrastructure is supported by the European Research Council under the European Union\u2019s Horizon 2020 research and innovation program (ERC grant Agreement 101002652, PI K. Mandel), the Heising-Simons Foundation (2018-0913, PI R. Foley; 2018-0911, PI R. Margutti), NASA (NNG17PX03C, PI R. Foley), NSF (AST-1720756, AST-1815935, PI R. Foley; AST-1909796, AST-1944985, PI R. Margutti), the David & Lucille Packard Foundation (PI R. Foley), VILLUM FONDEN (project 16599, PI J. Hjorth), and the Center for AstroPhysical Surveys (CAPS) at the National Center for Supercomputing Applications (NCSA) and the University of Illinois Urbana-Champaign. J.C.W. and J.V. acknowledge the support from the NSF grant AST-1813825. W.J.-G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842165. W.J.-G. acknowledges support through NASA grants in support of Hubble Space Telescope program GO-16075 and 16500. C.D.K. is partly supported by a CIERA postdoctoral fellowship. D.A.C. acknowledges support from the National Science Foundation Graduate Research Fellowship under grant DGE1339067. C.R.A. was supported by a grant from VILLUM FONDEN (project No. 16599). D.F. is supported by a VILLUM FONDEN Young Investigator Grant (project No. 25501).

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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