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A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx

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dc.contributor.authorKwok, Lindsey A.en
dc.contributor.authorJha, Saurabh W.en
dc.contributor.authorTemim, Teaen
dc.contributor.authorFox, Ori D.en
dc.contributor.authorLarison, Conoren
dc.contributor.authorCamacho-Neves, Yssavoen
dc.contributor.authorBrenner Newman, Max J.en
dc.contributor.authorPierel, Justin D. R.en
dc.contributor.authorFoley, Ryan J.en
dc.contributor.authorAndrews, Jennifer E.en
dc.contributor.authorBadenes, Carlesen
dc.contributor.authorBarna, Barnabasen
dc.contributor.authorBostroem, K. Azaleeen
dc.contributor.authorDeckers, Maximeen
dc.contributor.authorFloers, Andreasen
dc.contributor.authorGarnavich, Peteren
dc.contributor.authorGraham, Melissa L.en
dc.contributor.authorGraur, Oren
dc.contributor.authorHosseinzadeh, Griffinen
dc.contributor.authorHowell, D. Andrewen
dc.contributor.authorHughes, John P.en
dc.contributor.authorJohansson, Joelen
dc.contributor.authorKendrew, Sarahen
dc.contributor.authorKerzendorf, Wolfgang E.en
dc.contributor.authorMaeda, Keiichien
dc.contributor.authorMaguire, Kateen
dc.contributor.authorMcCully, Curtisen
dc.contributor.authorO'Brien, John T.en
dc.contributor.authorRest, Arminen
dc.contributor.authorSand, David J.en
dc.contributor.authorShahbandeh, Melissaen
dc.contributor.authorStrolger, Louis-Gregoryen
dc.contributor.authorSzalai, Tamasen
dc.contributor.authorAshall, Chrisen
dc.contributor.authorBaron, E.en
dc.contributor.authorBurns, Chris R.en
dc.contributor.authorDerKacy, James M.en
dc.contributor.authorEvans, Tyco Meraen
dc.contributor.authorFisher, Alecen
dc.contributor.authorGalbany, Lluisen
dc.contributor.authorHoeflich, Peteren
dc.contributor.authorHsiao, Ericen
dc.contributor.authorde Jaeger, Thomasen
dc.contributor.authorKaramehmetoglu, Emiren
dc.contributor.authorKrisciunas, Kevinen
dc.contributor.authorKumar, Sahanaen
dc.contributor.authorLu, Jingen
dc.contributor.authorMaund, Justynen
dc.contributor.authorMazzali, Paolo A.en
dc.contributor.authorMedler, Kyleen
dc.contributor.authorMorrell, Nidiaen
dc.contributor.authorPhillips, Mark. M.en
dc.contributor.authorShappee, Benjamin J.en
dc.contributor.authorStritzinger, Maximilianen
dc.contributor.authorSuntzeff, Nicholasen
dc.contributor.authorTelesco, Charlesen
dc.contributor.authorTucker, Michaelen
dc.contributor.authorWang, Lifanen
dc.date.accessioned2023-10-20T14:38:41Zen
dc.date.available2023-10-20T14:38:41Zen
dc.date.issued2023-02en
dc.description.abstractWe present JWST near-infrared (NIR) and mid-infrared (MIR) spectroscopic observations of the nearby normal Type Ia supernova (SN) SN 2021aefx in the nebular phase at +255 days past maximum light. Our Near Infrared Spectrograph (NIRSpec) and Mid Infrared Instrument observations, combined with ground-based optical data from the South African Large Telescope, constitute the first complete optical+NIR+MIR nebular SN Ia spectrum covering 0.3-14 mu m. This spectrum unveils the previously unobserved 2.5-5 mu m region, revealing strong nebular iron and stable nickel emission, indicative of high-density burning that can constrain the progenitor mass. The data show a significant improvement in sensitivity and resolution compared to previous Spitzer MIR data. We identify numerous NIR and MIR nebular emission lines from iron-group elements as well as lines from the intermediate-mass element argon. The argon lines extend to higher velocities than the iron-group elements, suggesting stratified ejecta that are a hallmark of delayed-detonation or double-detonation SN Ia models. We present fits to simple geometric line profiles to features beyond 1.2 mu m and find that most lines are consistent with Gaussian or spherical emission distributions, while the [Ar iii] 8.99 mu m line has a distinctively flat-topped profile indicating a thick spherical shell of emission. Using our line profile fits, we investigate the emissivity structure of SN 2021aefx and measure kinematic properties. Continued observations of SN 2021aefx and other SNe Ia with JWST will be transformative to the study of SN Ia composition, ionization structure, density, and temperature, and will provide important constraints on SN Ia progenitor and explosion models.en
dc.description.notesWe thank Shelly Meyett for her consistently excellent work scheduling these JWST observations, Greg Sloan for assistance with the MIRI LRS wavelength solution correction, and Glenn Wahlgren for help with the NIRSpec observations.; This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST program No. 02072. Support for this program at Rutgers University was provided by NASA through grant JWST-GO-02072.001.; The SALT data presented here were obtained with Rutgers University program 2022-1-MLT-004 (PI: Jha). We are grateful to SALT Astronomer Rosalind Skelton for taking these observations.; L.A.K. acknowledges support by NASA FINESST fellowship 80NSSC22K1599.; T.S. is supported by the NKFIH/OTKA FK-134432 grant of the National Research, Development and Innovation (NRDI) Office of Hungary, the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences, and the New National Excellence Program (UNKP-22-5) of the Ministry for Innovation and Technology of Hungary from the source of NRDI Fund.; Time-domain research by the University of Arizona team and D.J.S. is supported by NSF grants AST-1821987, 1813466, 1908972, and 2108032, and by the Heising-Simons Foundation under grant No. 2020-1864.; K.M. acknowledges support from the Japan Society for the Promotion of Science (JSPS) KAKENHI grants JP18H05223 and JP20H00174.; L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN), the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033, and the European Social Fund (ESF) "Investing in your future" under the 2019 Ramon y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M.; K.M. and M.D. are funded by the EU H2020 ERC grant No. 758638.; J.P.H. acknowledges support from the George A. and Margaret M. Downsbrough bequest.; The Aarhus supernova group is funded in part by an Experiment grant (No. 28021) from the Villum FONDEN, and by a project (1) grant (No. 8021-00170B) from the Independent Research Fund Denmark (IRFD).; C.L. acknowledges support from the National Science Foundation Graduate Research Fellowship under grant No. DGE-2233066.; A.F. acknowledges support by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (ERC advanced grant KILO-NOVA No. 885281).en
dc.description.sponsorshipNASA [NAS 5-03127, JWST-GO-02072.001]; JWST program [02072]; Rutgers University [2022-1-MLT-004]; NASA FINESST fellowship [80NSSC22K1599]; NKFIH/OTKA grant of the National Research, Development and Innovation (NRDI) Office of Hungary [FK-134432]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; New National Excellence Program of the Ministry for Innovation and Technology of Hungary from the source of NRDI Fund [UNKP-22-5]; NSF [AST-1821987, 1813466, 1908972, 2108032]; Heising-Simons Foundation [2020-1864]; Japan Society for the Promotion of Science (JSPS) KAKENHI grants [JP18H05223, JP20H00174]; Spanish Ministerio de Ciencia e Innovacion (MCIN), the Agencia Estatal de Investigacion (AEI); European Social Fund (ESF) "Investing in your future" under the 2019 Ramon y Cajal program [RYC2019-027683-I, PID2020-115253GA-I00]; Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project [20215AT016]; program Unidad de Excelencia Maria de Maeztu [CEX2020-001058-M]; EU H2020 ERC grant [758638]; George A. and Margaret M. Downsbrough bequest; Villum FONDEN [28021]; Independent Research Fund Denmark (IRFD) [8021-00170B]; National Science Foundation Graduate Research Fellowship [DGE-2233066]; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (ERC) [885281]; Direct For Mathematical & Physical Scien; Division Of Astronomical Sciences [2108032] Funding Source: National Science Foundationen
dc.description.versionPublished versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.3847/2041-8213/acb4ecen
dc.identifier.eissn2041-8213en
dc.identifier.issn2041-8205en
dc.identifier.issue1en
dc.identifier.otherL3en
dc.identifier.urihttp://hdl.handle.net/10919/116518en
dc.identifier.volume944en
dc.language.isoenen
dc.publisherIOP Publishingen
dc.rightsCreative Commons Attribution 4.0 Internationalen
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/en
dc.subjectchandrasekhar mass modelsen
dc.subjectsn 2014jen
dc.subjectdelayed-detonationen
dc.subjectexplosive nucleosynthesisen
dc.subjectspace-telescopeen
dc.subjectextinctionen
dc.subjectspectropolarimetryen
dc.subjectspectroscopyen
dc.subjectinstrumenten
dc.subjectasymmetryen
dc.titleA JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefxen
dc.title.serialAstrophysical Journal Lettersen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten

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