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dc.contributor.authorMayker Chen, Ness-
dc.contributor.authorTucker, Michael A.-
dc.contributor.authorHoyer, Nils-
dc.contributor.authorJha, Saurabh W.-
dc.contributor.authorKwok, Lindsey-
dc.contributor.authorLeroy, Adam K.-
dc.contributor.authorRosolowsky, Erik-
dc.contributor.authorAshall, Chris-
dc.contributor.authorAnand, Gagandeep-
dc.contributor.authorBigiel, Frank-
dc.contributor.authorBoquien, Médéric-
dc.contributor.authorBurns, Chris-
dc.contributor.authorDale, Daniel-
dc.contributor.authorDerKacy, James M.-
dc.contributor.authorEgorov, Oleg V.-
dc.contributor.authorGalbany, Lluis-
dc.contributor.authorGrasha, Kathryn-
dc.contributor.authorHassani, Hamid-
dc.contributor.authorHoeflich, Peter-
dc.contributor.authorHsiao, Eric-
dc.contributor.authorKlessen, Ralf S.-
dc.contributor.authorLopez, Laura A.-
dc.contributor.authorLu, Jing-
dc.contributor.authorMorrell, Nidia-
dc.contributor.authorOrellana, Mariana Dominga-
dc.contributor.authorPinna, Francesca-
dc.contributor.authorSarbadhicary, Sumit K.-
dc.contributor.authorSchinnerer, Eva-
dc.contributor.authorShahbandeh, Melissa-
dc.contributor.authorStritzinger, Maximilian-
dc.contributor.authorThilker, David A.-
dc.contributor.authorWilliams, Thomas G.-
dc.date.accessioned2023-04-24T13:50:33Z-
dc.date.available2023-04-24T13:50:33Z-
dc.date.issued2023-02-
dc.identifier.citationNess Mayker Chen et al 2023 ApJL 944 L28es_ES
dc.identifier.issn2041-8205es_ES
dc.identifier.issn2041-8213es_ES
dc.identifier.otherhttps://ui.adsabs.harvard.edu/abs/2023arXiv230105718M-
dc.identifier.urihttp://rid.unrn.edu.ar/handle/20.500.12049/10059-
dc.description.abstractWe present new 0.3-21 micron photometry of SN 2021aefx in the spiral galaxy NGC 1566 at +357 days after B-band maximum, including the first detection of any SN Ia at >15 micron. These observations follow earlier JWST observations of SN 2021aefx at +255 days after the time of maximum brightness, allowing us to probe the temporal evolution of the emission properties. We measure the fraction of flux emerging at different wavelengths and its temporal evolution. Additionally, the integrated 0.3-14 micron decay rate of $\Delta m_{0.3-14} = 1.35 \pm 0.05$ mag/100 days is higher than the decline rate from the radioactive decay of $^{56}$Co of $\sim 1.2$mag/100 days. The most plausible explanation for this discrepancy is that flux is shifting to >14 micron, and future JWST observations of SNe Ia will be able to directly test this hypothesis. However, models predicting non-radiative energy loss cannot be excluded with the present data.es_ES
dc.format.extentp. L28.1-9es_ES
dc.language.isoenes_ES
dc.publisherIOP PUBLISHING LTDes_ES
dc.relation.urihttps://iopscience.iop.org/journal/2041-8205es_ES
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/4.0/-
dc.titleSerendipitous Nebular-phase JWST Imaging of SN Ia 2021aefx: Testing the Confinement of 56-Co Decay Energyes_ES
dc.title.alternativeSN 2021aefx with JWSTes_ES
dc.typeArticuloes_ES
dc.rights.licenseCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)-
dc.description.filiationNess Mayker Chen,Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USAes_ES
dc.description.filiationMichael A. Tucker, Center for Cosmology and Astroparticle Physics, 191 West Woodruff Avenue, Columbus, OH 43210, USAes_ES
dc.description.filiationNils Hoyer, Donostia International Physics Center, Paseo Manuel de Lardizabal 4, E-20118 Donostia-San Sebastián, Spaines_ES
dc.description.filiationSaurabh W. Jha, Department of Physics and Astronomy, Rutgers, the State University of New Jersey, USAes_ES
dc.description.filiationLindsey Kwok, Department of Physics and Astronomy, Rutgers, the State University of New Jersey, USAes_ES
dc.description.filiationAdam K. Leroy, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USAes_ES
dc.description.filiationErik Rosolowsky, Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canadaes_ES
dc.description.filiationChris Ashall, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USAes_ES
dc.description.filiationGagandeep Anand, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAes_ES
dc.description.filiationFrank Bigiel, Argelander-Institut fur Astronomie, Universitat Bonn, Auf dem Hugel 71, 53121 Bonn, Germanyes_ES
dc.description.filiationMédéric Boquien, Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, Chilees_ES
dc.description.filiationChris Burns, Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USAes_ES
dc.description.filiationDaniel Dale, Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USAes_ES
dc.description.filiationJames M. DerKacy, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USAes_ES
dc.description.filiationOleg V. Egorov, Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitat Heidelberg, Heidelberg, Germanyes_ES
dc.description.filiationL. Galbany, Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spaines_ES
dc.description.filiationKathryn Grasha, Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australiaes_ES
dc.description.filiationHamid Hassani, Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canadaes_ES
dc.description.filiationPeter Hoeflich, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USAes_ES
dc.description.filiationEric Hsiao, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USAes_ES
dc.description.filiationRalf S. Klessen, Universitat Heidelberg, Zentrum fur Astronomie, Institut fur Theoretische Astrophysik, Albert-Ueberle-Str 2, D-69120 Heidelberg, Germanyes_ES
dc.description.filiationLaura A. Lopez, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USAes_ES
dc.description.filiationJing Lu, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USAes_ES
dc.description.filiationNidia Morrell, Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chilees_ES
dc.description.filiationMariana Orellana, Universidad Nacional de Río Negro. Sede Andina, Mitre 630 (8400), Bariloche, Argentinaes_ES
dc.description.filiationMariana Orellana, Consejo Nacional de Investigaciones Científicas y Tećnicas (CONICET), Argentinaes_ES
dc.description.filiationFrancesca Pinna, Max Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germanyes_ES
dc.description.filiationSumit K. Sarbadhicary, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USAes_ES
dc.description.filiationEva Schinnerer, Max Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germanyes_ES
dc.description.filiationMelissa Shahbandeh, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USAes_ES
dc.description.filiationMaximilian Stritzinger, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmarkes_ES
dc.description.filiationDavid A. Thilker, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USAes_ES
dc.description.filiationThomas G. Williams, Sub-department of Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UKes_ES
dc.subject.keywordinterstellar medium: star-formationes_ES
dc.subject.keywordsupernova: locationses_ES
dc.subject.keywordsupernova: individual SN2021aefxes_ES
dc.type.versioninfo:eu-repo/semantics/acceptedVersiones_ES
dc.subject.materiaAstronomíaes_ES
dc.origin.lugarDesarrolloColaboración internacionales_ES
dc.relation.journalissue944es_ES
dc.description.reviewtruees_ES
dc.description.resumenPresentamos una nueva fotometría en longitudes de 0,3-21 micras de SN 2021aefx en la galaxia espiral NGC 1566 a +357 días después del máximo de la banda B, incluida la primera detección de cualquier SN Ia a >15 micras. Estas observaciones siguen a observaciones anteriores del JWST de SN 2021aefx a +255 días después del momento de máximo brillo, lo que nos permite probar la evolución temporal de las propiedades de emisión. Medimos la fracción de flujo que emerge a diferentes longitudes de onda y su evolución temporal. Además, la tasa de desintegración integrada de 0,3-14 micras de m__(0,3-14) = 1,35 +/- 0,05 mag/100 días es mayor que la tasa de desintegración de la desintegración radiactiva de 56Co de +/- 1.2 mag/100 días. La explicación más plausible para esta discrepancia es que el flujo se está desplazando a >14 micras, y las futuras observaciones de SNe Ia del JWST podrán probar directamente esta hipótesis. Sin embargo, los modelos que predicen la pérdida de energía no radiativa no pueden excluirse con los datos actuales.es_ES
dc.identifier.doihttps://doi.org/10.3847/2041-8213/acb6d8-
dc.relation.journalTitleThe Astrophysical Journal Letterses_ES
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