The progenitor of the type IIb SN 2008ax revisited
- Autores
- Folatelli, Gaston; Bersten, Melina Cecilia; Kuncarayakti, Hanindyo; Benvenuto, Omar Gustavo; Maeda, Keiichi; Nomoto, Ken’ichi
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Hubble Space Telescope observations of the site of the supernova (SN) SN 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf?Rayet (W-R) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modeling shows that the pre-explosion mass was 4?5 M⊙ and the radius was 30?50 R⊙, which is incompatible with a W-R progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9?B0 main-sequence star may have remained after the explosion.
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón
Fil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón
Fil: Kuncarayakti, Hanindyo . Millennium Institute of Astrophysics; Chile
Fil: Benvenuto, Omar Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Maeda, Keiichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón
Fil: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón - Materia
-
Supernovae
Sn2008ax (Supernova) - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/12612
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The progenitor of the type IIb SN 2008ax revisitedFolatelli, GastonBersten, Melina CeciliaKuncarayakti, Hanindyo Benvenuto, Omar GustavoMaeda, Keiichi Nomoto, Ken’ichi SupernovaeSn2008ax (Supernova)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Hubble Space Telescope observations of the site of the supernova (SN) SN 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf?Rayet (W-R) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modeling shows that the pre-explosion mass was 4?5 M⊙ and the radius was 30?50 R⊙, which is incompatible with a W-R progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9?B0 main-sequence star may have remained after the explosion.Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; JapónFil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; JapónFil: Kuncarayakti, Hanindyo . Millennium Institute of Astrophysics; ChileFil: Benvenuto, Omar Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Maeda, Keiichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; JapónFil: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; JapónIop Publishing2015-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/12612Folatelli, Gaston; Bersten, Melina Cecilia; Kuncarayakti, Hanindyo ; Benvenuto, Omar Gustavo; Maeda, Keiichi ; et al.; The progenitor of the type IIb SN 2008ax revisited; Iop Publishing; Astrophysical Journal; 811; 2; 10-2015; 147-1590004-637Xenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/811/2/147/metainfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/811/2/147info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:10:36Zoai:ri.conicet.gov.ar:11336/12612instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-03 10:10:37.176CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The progenitor of the type IIb SN 2008ax revisited |
title |
The progenitor of the type IIb SN 2008ax revisited |
spellingShingle |
The progenitor of the type IIb SN 2008ax revisited Folatelli, Gaston Supernovae Sn2008ax (Supernova) |
title_short |
The progenitor of the type IIb SN 2008ax revisited |
title_full |
The progenitor of the type IIb SN 2008ax revisited |
title_fullStr |
The progenitor of the type IIb SN 2008ax revisited |
title_full_unstemmed |
The progenitor of the type IIb SN 2008ax revisited |
title_sort |
The progenitor of the type IIb SN 2008ax revisited |
dc.creator.none.fl_str_mv |
Folatelli, Gaston Bersten, Melina Cecilia Kuncarayakti, Hanindyo Benvenuto, Omar Gustavo Maeda, Keiichi Nomoto, Ken’ichi |
author |
Folatelli, Gaston |
author_facet |
Folatelli, Gaston Bersten, Melina Cecilia Kuncarayakti, Hanindyo Benvenuto, Omar Gustavo Maeda, Keiichi Nomoto, Ken’ichi |
author_role |
author |
author2 |
Bersten, Melina Cecilia Kuncarayakti, Hanindyo Benvenuto, Omar Gustavo Maeda, Keiichi Nomoto, Ken’ichi |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
Supernovae Sn2008ax (Supernova) |
topic |
Supernovae Sn2008ax (Supernova) |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Hubble Space Telescope observations of the site of the supernova (SN) SN 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf?Rayet (W-R) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modeling shows that the pre-explosion mass was 4?5 M⊙ and the radius was 30?50 R⊙, which is incompatible with a W-R progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9?B0 main-sequence star may have remained after the explosion. Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón Fil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón Fil: Kuncarayakti, Hanindyo . Millennium Institute of Astrophysics; Chile Fil: Benvenuto, Omar Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Maeda, Keiichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón Fil: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón |
description |
Hubble Space Telescope observations of the site of the supernova (SN) SN 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf?Rayet (W-R) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modeling shows that the pre-explosion mass was 4?5 M⊙ and the radius was 30?50 R⊙, which is incompatible with a W-R progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9?B0 main-sequence star may have remained after the explosion. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015-10 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/12612 Folatelli, Gaston; Bersten, Melina Cecilia; Kuncarayakti, Hanindyo ; Benvenuto, Omar Gustavo; Maeda, Keiichi ; et al.; The progenitor of the type IIb SN 2008ax revisited; Iop Publishing; Astrophysical Journal; 811; 2; 10-2015; 147-159 0004-637X |
url |
http://hdl.handle.net/11336/12612 |
identifier_str_mv |
Folatelli, Gaston; Bersten, Melina Cecilia; Kuncarayakti, Hanindyo ; Benvenuto, Omar Gustavo; Maeda, Keiichi ; et al.; The progenitor of the type IIb SN 2008ax revisited; Iop Publishing; Astrophysical Journal; 811; 2; 10-2015; 147-159 0004-637X |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/811/2/147/meta info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/811/2/147 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Iop Publishing |
publisher.none.fl_str_mv |
Iop Publishing |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1842270127166324736 |
score |
13.13397 |