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

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dc.contributor.authorWang, Qinanen
dc.contributor.authorArmstrong, Patricken
dc.contributor.authorZenati, Yossefen
dc.contributor.authorRidden-Harper, Ryanen
dc.contributor.authorRest, Arminen
dc.contributor.authorArcavi, Iairen
dc.contributor.authorKilpatrick, Charles D.en
dc.contributor.authorFoley, Ryan J.en
dc.contributor.authorTucker, Brad E.en
dc.contributor.authorLidman, Chrisen
dc.contributor.authorKillestein, Thomas L.en
dc.contributor.authorShahbandeh, Melissaen
dc.contributor.authorAnderson, Joseph P.en
dc.contributor.authorAngulo, Rodrigoen
dc.contributor.authorAshall, Chrisen
dc.contributor.authorBurke, Jamisonen
dc.contributor.authorChen, Ting-Wanen
dc.contributor.authorvon Coelln, Sophieen
dc.contributor.authorDalrymple, Kyle A.en
dc.contributor.authorDavis, Kyle W.en
dc.contributor.authorFulton, Michael D.en
dc.contributor.authorGalbany, Lluisen
dc.contributor.authorGonzalez, Estefania Padillaen
dc.contributor.authorGao, Boreen
dc.contributor.authorGromadzki, Mariuszen
dc.contributor.authorHowell, D. Andrewen
dc.contributor.authorIhanec, Nadaen
dc.contributor.authorJencson, Jacob E.en
dc.contributor.authorJones, David O.en
dc.contributor.authorLyman, Joseph D.en
dc.contributor.authorMcCully, Curtisen
dc.contributor.authorMuller-Bravo, Tomas E.en
dc.contributor.authorNewsome, Meganen
dc.contributor.authorNicholl, Matten
dc.contributor.authorO'Neill, Daviden
dc.contributor.authorPellegrino, Craigen
dc.contributor.authorRest, Sofiaen
dc.contributor.authorSmartt, Stephen J.en
dc.contributor.authorSmith, Kenen
dc.contributor.authorSrivastav, Shubhamen
dc.contributor.authorTerreran, Giacomoen
dc.contributor.authorTinyanont, Samapornen
dc.contributor.authorYoung, David R.en
dc.contributor.authorZenteno, Alfredoen
dc.date.accessioned2023-03-27T17:05:52Zen
dc.date.available2023-03-27T17:05:52Zen
dc.date.issued2023-02-01en
dc.description.abstractWe 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 similar to 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 similar to 0.30-0.65 M-circle dot and an envelope radius of similar to 120-300 R-circle dot. 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.en
dc.description.notesThis 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.; This work makes use of data from Las Cumbres Observatory. The LCO group is supported by NSF grants AST-1911225 and AST-1911151.; This work was funded by ANID, Millennium Science Initiative, ICN12_009.; This work is partially based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey). ePESSTO+ observations were obtained under ESO program IDs 1103.D-0328, 106.216C, 108.220C (PI: Inserra).; Q.W. is supported in part by NASA grants 80NSSC22K0494, 80NSSC21K0242, and 80NSSC19K0112.; 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 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.; L.G. and T.E.M.B. acknowledge financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN), and the Agencia Estatal de Investigacion (AEI) 10.13039/ 501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project 20215AT016 and the I-LINK 2021 LINKA20409, and the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M. L.G. additionally acknowledges the European Social Fund (ESF) "Investing in your future" under the 2019 Ramon y Cajal program RYC2019-027683-I.; M.G. is supported by the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004719.; N.I. was partially supported by Polish NCN DAINA grant No. 2017/27/L/ST9/03221.; J.D.L. and D.O.N. acknowledge support from a UK Research and Innovation Fellowship (MR/T020784/1).; 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.; S.J.S., S.S., D.R.Y., and K.W.S. acknowledge funding from STFC grants ST/T000198/1 and ST/S006109/1.en
dc.description.sponsorshipNASA [NAS5-26555, 80NSSC22K0494, 80NSSC21K0242, 80NSSC19K0112, 80NSSC20K0953]; NASA Office of Space Science [NAG5-7584]; NSF [AST-1911225, AST-1911151, AST-1815935]; ANID, Millennium Science Initiative [ICN12_009]; ESO [1103.D-0328, 106.216C, 108.220C]; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program [852097, 948381]; Israel Science Foundation [2752/19]; United States-Israel Binational Science Foundation (BSF); Israeli Council for Higher Education Alon Fellowship; Gordon & Betty Moore Foundation; Heising-Simons Foundation; David and Lucile Packard Foundation; Spanish Ministerio de Ciencia e Innovacion (MCIN) [PID2020-115253GA-I00]; Agencia Estatal de Investigacion (AEI) [PID2020-115253GA-I00]; Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project [20215AT016]; Centro Superior de Investigaciones Cientificas (CSIC) under I-LINK 2021 [LINKA20409]; program Unidad de Excelencia Maria de Maeztu [CEX2020-001058-M]; European Social Fund (ESF) "Investing in your future" under the 2019 Ramon y Cajal program [RYC2019-027683-I]; European Union [101004719]; Polish NCN DAINA grant [2017/27/L/ST9/03221]; UK Research and Innovation Fellowship [MR/T020784/1]; Alan Turing Institute; STFC [ST/T000198/1, ST/S006109/1]en
dc.description.versionPublished versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.3847/2041-8213/acb0d0en
dc.identifier.eissn2041-8213en
dc.identifier.issue2en
dc.identifier.otherL15en
dc.identifier.urihttp://hdl.handle.net/10919/114190en
dc.identifier.volume943en
dc.language.isoenen
dc.publisherIOP Publishingen
dc.rightsCreative Commons Attribution 4.0 Internationalen
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/en
dc.subjectYellow supergiant progenitoren
dc.subjectwolf-rayet starsen
dc.subjectiib supernovaen
dc.subjectearly evolutionen
dc.subjectia supernovaen
dc.subjectmass-lossen
dc.subject2011dhen
dc.subjectemissionen
dc.subjectspectraen
dc.subjectspectrographen
dc.titleRevealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curveen
dc.title.serialAstrophysical Journal Lettersen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten

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