Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve

Qinan Wang*, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P. Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. DavisMichael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O’Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

3 Scopus citations

Abstract

We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS captured the prominent early shock-cooling peak of SN 2021zby within the first ∼10 days after explosion with a 30 minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock-cooling phase. Using a multiband model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of ∼0.30-0.65 M and an envelope radius of ∼120-300 R . These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked feature, such as SNe 1993J, 2011dh, 2016gkg, and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock-cooling light curve, while the multiband observations, particularly UV, are also necessary to fully constrain the progenitor properties.

Original languageEnglish (US)
Article numberL15
JournalAstrophysical Journal Letters
Volume943
Issue number2
DOIs
StatePublished - Feb 1 2023

Funding

S.J.S., S.S., D.R.Y., and K.W.S. acknowledge funding from STFC grants ST/T000198/1 and ST/S006109/1. N.I. was partially supported by Polish NCN DAINA grant No. 2017/27/L/ST9/03221. This Letter includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA’s Science Mission Directorate. The TESS data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). The specific observations analyzed can be accessed via doi: 10.17909/0cp4-2j79 . STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support to MAST for these data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. L.G. and T.E.M.B. acknowledge financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the I-LINK 2021 LINKA20409, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. L.G. additionally acknowledges the European Social Fund (ESF) “Investing in your future” under the 2019 Ramón y Cajal program RYC2019-027683-I. J.D.L. and D.O.N. acknowledge support from a UK Research and Innovation Fellowship (MR/T020784/1). The UCSC team is supported in part by NASA grant 80NSSC20K0953, 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. This work makes use of data from Las Cumbres Observatory. The LCO group is supported by NSF grants AST-1911225 and AST-1911151. M.N. is supported by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 948381) and by a Fellowship from the Alan Turing Institute. I.A. is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement number 852097), from the Israel Science Foundation (grant number 2752/19), from the United States—Israel Binational Science Foundation (BSF), and from the Israeli Council for Higher Education Alon Fellowship. The author acknowledges Luc Dessart, Eli Waxman, Nir Sapir, Ryosuke Hirai., and Sasha Kozyreva for the valuable discussion. M.G. is supported by the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004719. This work was funded by ANID, Millennium Science Initiative, ICN12_009. Q.W. is supported in part by NASA grants 80NSSC22K0494, 80NSSC21K0242, and 80NSSC19K0112.

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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