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Campo DC | Valor | Lengua/Idioma |
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dc.contributor.author | Mayker Chen, Ness | - |
dc.contributor.author | Tucker, Michael A. | - |
dc.contributor.author | Hoyer, Nils | - |
dc.contributor.author | Jha, Saurabh W. | - |
dc.contributor.author | Kwok, Lindsey | - |
dc.contributor.author | Leroy, Adam K. | - |
dc.contributor.author | Rosolowsky, Erik | - |
dc.contributor.author | Ashall, Chris | - |
dc.contributor.author | Anand, Gagandeep | - |
dc.contributor.author | Bigiel, Frank | - |
dc.contributor.author | Boquien, Médéric | - |
dc.contributor.author | Burns, Chris | - |
dc.contributor.author | Dale, Daniel | - |
dc.contributor.author | DerKacy, James M. | - |
dc.contributor.author | Egorov, Oleg V. | - |
dc.contributor.author | Galbany, Lluis | - |
dc.contributor.author | Grasha, Kathryn | - |
dc.contributor.author | Hassani, Hamid | - |
dc.contributor.author | Hoeflich, Peter | - |
dc.contributor.author | Hsiao, Eric | - |
dc.contributor.author | Klessen, Ralf S. | - |
dc.contributor.author | Lopez, Laura A. | - |
dc.contributor.author | Lu, Jing | - |
dc.contributor.author | Morrell, Nidia | - |
dc.contributor.author | Orellana, Mariana Dominga | - |
dc.contributor.author | Pinna, Francesca | - |
dc.contributor.author | Sarbadhicary, Sumit K. | - |
dc.contributor.author | Schinnerer, Eva | - |
dc.contributor.author | Shahbandeh, Melissa | - |
dc.contributor.author | Stritzinger, Maximilian | - |
dc.contributor.author | Thilker, David A. | - |
dc.contributor.author | Williams, Thomas G. | - |
dc.date.accessioned | 2023-04-24T13:50:33Z | - |
dc.date.available | 2023-04-24T13:50:33Z | - |
dc.date.issued | 2023-02 | - |
dc.identifier.citation | Ness Mayker Chen et al 2023 ApJL 944 L28 | es_ES |
dc.identifier.issn | 2041-8205 | es_ES |
dc.identifier.issn | 2041-8213 | es_ES |
dc.identifier.other | https://ui.adsabs.harvard.edu/abs/2023arXiv230105718M | - |
dc.identifier.uri | http://rid.unrn.edu.ar/handle/20.500.12049/10059 | - |
dc.description.abstract | We 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.extent | p. L28.1-9 | es_ES |
dc.language.iso | en | es_ES |
dc.publisher | IOP PUBLISHING LTD | es_ES |
dc.relation.uri | https://iopscience.iop.org/journal/2041-8205 | es_ES |
dc.rights.uri | http://creativecommons.org/licenses/by-nc-sa/4.0/ | - |
dc.title | Serendipitous Nebular-phase JWST Imaging of SN Ia 2021aefx: Testing the Confinement of 56-Co Decay Energy | es_ES |
dc.title.alternative | SN 2021aefx with JWST | es_ES |
dc.type | Articulo | es_ES |
dc.rights.license | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | - |
dc.description.filiation | Ness Mayker Chen,Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA | es_ES |
dc.description.filiation | Michael A. Tucker, Center for Cosmology and Astroparticle Physics, 191 West Woodruff Avenue, Columbus, OH 43210, USA | es_ES |
dc.description.filiation | Nils Hoyer, Donostia International Physics Center, Paseo Manuel de Lardizabal 4, E-20118 Donostia-San Sebastián, Spain | es_ES |
dc.description.filiation | Saurabh W. Jha, Department of Physics and Astronomy, Rutgers, the State University of New Jersey, USA | es_ES |
dc.description.filiation | Lindsey Kwok, Department of Physics and Astronomy, Rutgers, the State University of New Jersey, USA | es_ES |
dc.description.filiation | Adam K. Leroy, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA | es_ES |
dc.description.filiation | Erik Rosolowsky, Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada | es_ES |
dc.description.filiation | Chris Ashall, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA | es_ES |
dc.description.filiation | Gagandeep Anand, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA | es_ES |
dc.description.filiation | Frank Bigiel, Argelander-Institut fur Astronomie, Universitat Bonn, Auf dem Hugel 71, 53121 Bonn, Germany | es_ES |
dc.description.filiation | Médéric Boquien, Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, Chile | es_ES |
dc.description.filiation | Chris Burns, Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA | es_ES |
dc.description.filiation | Daniel Dale, Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA | es_ES |
dc.description.filiation | James M. DerKacy, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA | es_ES |
dc.description.filiation | Oleg V. Egorov, Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitat Heidelberg, Heidelberg, Germany | es_ES |
dc.description.filiation | L. Galbany, Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain | es_ES |
dc.description.filiation | Kathryn Grasha, Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia | es_ES |
dc.description.filiation | Hamid Hassani, Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada | es_ES |
dc.description.filiation | Peter Hoeflich, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA | es_ES |
dc.description.filiation | Eric Hsiao, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA | es_ES |
dc.description.filiation | Ralf S. Klessen, Universitat Heidelberg, Zentrum fur Astronomie, Institut fur Theoretische Astrophysik, Albert-Ueberle-Str 2, D-69120 Heidelberg, Germany | es_ES |
dc.description.filiation | Laura A. Lopez, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA | es_ES |
dc.description.filiation | Jing Lu, Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA | es_ES |
dc.description.filiation | Nidia Morrell, Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile | es_ES |
dc.description.filiation | Mariana Orellana, Universidad Nacional de Río Negro. Sede Andina, Mitre 630 (8400), Bariloche, Argentina | es_ES |
dc.description.filiation | Mariana Orellana, Consejo Nacional de Investigaciones Científicas y Tećnicas (CONICET), Argentina | es_ES |
dc.description.filiation | Francesca Pinna, Max Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germany | es_ES |
dc.description.filiation | Sumit K. Sarbadhicary, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA | es_ES |
dc.description.filiation | Eva Schinnerer, Max Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germany | es_ES |
dc.description.filiation | Melissa Shahbandeh, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA | es_ES |
dc.description.filiation | Maximilian Stritzinger, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark | es_ES |
dc.description.filiation | David A. Thilker, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA | es_ES |
dc.description.filiation | Thomas G. Williams, Sub-department of Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK | es_ES |
dc.subject.keyword | interstellar medium: star-formation | es_ES |
dc.subject.keyword | supernova: locations | es_ES |
dc.subject.keyword | supernova: individual SN2021aefx | es_ES |
dc.type.version | info:eu-repo/semantics/acceptedVersion | es_ES |
dc.subject.materia | Astronomía | es_ES |
dc.origin.lugarDesarrollo | Colaboración internacional | es_ES |
dc.relation.journalissue | 944 | es_ES |
dc.description.review | true | es_ES |
dc.description.resumen | Presentamos 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.doi | https://doi.org/10.3847/2041-8213/acb6d8 | - |
dc.relation.journalTitle | The Astrophysical Journal Letters | es_ES |
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