Abstract
We present optical, ultraviolet, and infrared data of the type II supernova (SN II) 2020jfo at 14.5 Mpc. This wealth of multiwavelength data allows us to compare different metrics commonly used to estimate progenitor masses of SN II for the same object. Using its early light curve, we infer SN 2020jfo had a progenitor radius of ≈700 R ⊙, consistent with red supergiants of initial mass M ZAMS = 11-13 M ⊙. The decline in its late-time light curve is best fit by a 56 Ni mass of 0.018 ±0.007 M ⊙consistent with that ejected from SN II-P with ≈13 M ⊙initial mass stars. Early spectra and photometry do not exhibit signs of interaction with circumstellar matter, implying that SN 2020jfo experienced weak mass-loss within the final years prior to explosion. Our spectra at > 250 d are best fit by models from 12 M ⊙initial mass stars. We analysed integral field unit spectroscopy of the stellar population near SN 2020jfo, finding its massive star population had a zero age main sequence mass of 9.7 + 2 . 5-1 . 3 M ⊙. We identify a single counterpart in pre-explosion imaging and find it has an initial mass of at most 7 . 2 + 1 . 2-0 . 6 M ⊙. We conclude that the inconsistency between this mass and indirect mass indicators from SN 2020jfo itself is most likely caused by extinction with A V = 2-3 mag due to matter around the progenitor star, which lowered its observed optical luminosity. As SN 2020jfo did not e xhibit e xtinction at this lev el or evidence for interaction with circumstellar matter between 1.6 and 450 d from explosion, we conclude that this material was likely confined within ≈3000 R ⊙from the progenitor star.
Original language | English (US) |
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Pages (from-to) | 2161-2185 |
Number of pages | 25 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 524 |
Issue number | 2 |
DOIs | |
State | Published - Sep 1 2023 |
Funding
IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. We thank K. Clever, C. Smith, and E. Strasburger for help with obtaining our Nickel observations. CDK acknowledges support from HST program AR-16136 and from a CIERA postdoctoral fellowship. CG acknowledges support from a VILLUM FONDEN Young Investor Grant (project number 25501). DOJ acknowledges support provided by NASA Hubble Fellowship grant HST-HF2-51462.001, which is awarded by the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. AJGO acknowledges support from the Lachlan Gilchrist Fellowship Fund. MRD acknowledges support from the NSERC through grant RGPIN-2019-06186, the Canada Research Chairs Program, the Canadian Institute for Advanced Research (CIFAR), and the Dunlap Institute at the University of Toronto. 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, 80NSSC21K1572 and by the State of Hawaii. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work makes use of observations from the LCOGT network through programs NOAO2020A-008, NOAO2020B-009 (PI Kilpatrick), NOAO2020A-012, and NOAO2020B-011 (PI Foley). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5–26555. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 108-2112-M-008-001.
Keywords
- stars: e volution -stars: massive -transients: supernovae
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science