SN 2023ixf in Messier 101: The Twilight Years of the Progenitor as Seen by Pan-STARRS

Conor L. Ransome*, V. Ashley Villar, Anna Tartaglia, Sebastian Javier Gonzalez, Wynn V. Jacobson-Galán, Charles D. Kilpatrick, Raffaella Margutti, Ryan J. Foley, Matthew Grayling, Yuan Qi Ni, Ricardo Yarza, Christine Ye, Katie Auchettl, Thomas de Boer, Kenneth C. Chambers, David A. Coulter, Maria R. Drout, Diego Farias, Christa Gall, Hua GaoMark E. Huber, Adaeze L. Ibik, David O. Jones, Nandita Khetan, Chien Cheng Lin, Collin A. Politsch, Sandra I. Raimundo, Armin Rest, Richard J. Wainscoat, S. Karthik Yadavalli, Yossef Zenati

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

9 Scopus citations

Abstract

The nearby type II supernova, SN 2023ixf in M101 exhibits signatures of early time interaction with circumstellar material in the first week postexplosion. This material may be the consequence of prior mass loss suffered by the progenitor, which possibly manifested in the form of a detectable presupernova outburst. We present an analysis of long-baseline preexplosion photometric data in the g, w, r, i, z, and y filters from Pan-STARRS as part of the Young Supernova Experiment, spanning ∼5000 days. We find no significant detections in the Pan-STARRS preexplosion light curves. We train a multilayer perceptron neural network to classify presupernova outbursts. We find no evidence of eruptive presupernova activity to a limiting absolute magnitude of −7 mag. The limiting magnitudes from the full set of gwrizy (average absolute magnitude ≈ −8 mag) data are consistent with previous preexplosion studies. We use deep photometry from the literature to constrain the progenitor of SN 2023ixf, finding that these data are consistent with a dusty red supergiant progenitor with luminosity log L / L ⊙ ≈ 5.12

Original languageEnglish (US)
Article number93
JournalAstrophysical Journal
Volume965
Issue number1
DOIs
StatePublished - Apr 1 2024

Funding

Pan-STARRS is a project of the Institute for Astronomy of the University of Hawaii, and is supported by the NASA SSO Near Earth Observation Program under grants 80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, and 80NSSC21K1572 and by the State of Hawaii. The Pan-STARRS 1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen\u2019s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, STScI, NASA under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, NSF grant AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. V.A.V. and C.L.R. acknowledge support from the Charles E. Kaufman Foundation through the New Investigator grant KA2022-129525. W.J.-G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842165. C.D.K. acknowledges partial support from a CIERA postdoctoral fellowship. M.G. acknowledges support from the European Union's Horizon 2020 research and innovation program under ERC grant Agreement No. 101002652 and Marie Sk\u0142odowska-Curie grant Agreement No. 873089. M.R.D. acknowledges support from the NSERC through grant RGPIN-2019-06186, the Canada Research Chairs Program, and the Dunlap Institute at the University of Toronto. C.G. is supported by a VILLUM FONDEN Young Investigator grant (project number 25501). R.Y. is grateful for support from a Doctoral Fellowship from the University of California Institute for Mexico and the United States (UCMEXUS) and a NASA FINESST award (21-ASTRO21-0068). The UCSC team is supported in part by NASA grant NNG17PX03C, NSF grant AST-1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by a fellowship from the David and Lucile Packard Foundation to R.J.F. 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 and AST-1815935, PI: R. Foley; AST-1909796 and 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.

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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