Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv
- Autores
- Gall, C.; Stritzinger, M. D.; Ashall, C.; Baron, E.; Burns, C. R.; Hoeflich, P.; Hsiao, E. Y.; Mazzali, P. A.; Phillips, M. M.; Filippenko, A. V.; Anderson, J. P.; Benetti, S.; Brown, P. J.; Campillay, A.; Challis, P.; Contreras, C.; Elias De La Rosa, N.; Folatelli, Gaston; Foley, R. J.; Fraser, M.; Holmbo, S.; Marion, G. H.; Morrell, N.; Pan, Y. C.; Pignata, G.; Suntzeff, N. B.; Taddia, F.; Torres Robledo, S.; Valenti, S.
- Año de publicación
- 2018
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by Δm15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B- and H-band magnitudes differ by ~ 0.60 mag and ~0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ~ 14% and ~ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B - V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B - V colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.
Fil: Gall, C.. University Aarhus; Dinamarca
Fil: Stritzinger, M. D.. University Aarhus; Dinamarca
Fil: Ashall, C.. Liverpool John Moores University; Reino Unido
Fil: Baron, E.. Oklahoma State University; Estados Unidos
Fil: Burns, C. R.. Carnegie Observatories; Chile
Fil: Hoeflich, P.. Florida State University; Estados Unidos
Fil: Hsiao, E. Y.. University Aarhus; Dinamarca. Florida State University; Estados Unidos
Fil: Mazzali, P. A.. Liverpool John Moores University; Reino Unido
Fil: Phillips, M. M.. Las Campanas Observatory; Chile
Fil: Filippenko, A. V.. University of California at Berkeley; Estados Unidos
Fil: Anderson, J. P.. European Southern Observatory Santiago; Chile
Fil: Benetti, S.. Osservatorio Astronomico Di Padova; Italia
Fil: Brown, P. J.. Texas A&M University; Estados Unidos
Fil: Campillay, A.. Las Campanas Observatory; Chile
Fil: Challis, P.. European Southern Observatory Santiago; Chile
Fil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; Chile
Fil: Elias De La Rosa, N.. Osservatorio Astronomico Di Padova; Italia
Fil: Folatelli, Gaston. Texas A&M University; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Foley, R. J.. University of California; Estados Unidos
Fil: Fraser, M.. University College Dublin; Irlanda
Fil: Holmbo, S.. University Aarhus; Dinamarca
Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos
Fil: Morrell, N.. Las Campanas Observatory; Chile
Fil: Pan, Y. C.. University of California; Estados Unidos
Fil: Pignata, G.. Millennium Institute Of Astrophysics; Chile. Universidad Andrés Bello; Chile
Fil: Suntzeff, N. B.. Texas A&M University; Estados Unidos
Fil: Taddia, F.. Stockholms Universitet; Suecia
Fil: Torres Robledo, S.. Las Campanas Observatory; Chile
Fil: Valenti, S.. University of California at Davis; Estados Unidos - Materia
-
Dust, Extinction
Supernovae: General
Supernovae: Individual: Sn 2007on
Supernovae: Individual: Sn 2011iv - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/82546
Ver los metadatos del registro completo
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Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011ivGall, C.Stritzinger, M. D.Ashall, C.Baron, E.Burns, C. R.Hoeflich, P.Hsiao, E. Y.Mazzali, P. A.Phillips, M. M.Filippenko, A. V.Anderson, J. P.Benetti, S.Brown, P. J.Campillay, A.Challis, P.Contreras, C.Elias De La Rosa, N.Folatelli, GastonFoley, R. J.Fraser, M.Holmbo, S.Marion, G. H.Morrell, N.Pan, Y. C.Pignata, G.Suntzeff, N. B.Taddia, F.Torres Robledo, S.Valenti, S.Dust, ExtinctionSupernovae: GeneralSupernovae: Individual: Sn 2007onSupernovae: Individual: Sn 2011ivhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by Δm15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B- and H-band magnitudes differ by ~ 0.60 mag and ~0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ~ 14% and ~ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B - V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B - V colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.Fil: Gall, C.. University Aarhus; DinamarcaFil: Stritzinger, M. D.. University Aarhus; DinamarcaFil: Ashall, C.. Liverpool John Moores University; Reino UnidoFil: Baron, E.. Oklahoma State University; Estados UnidosFil: Burns, C. R.. Carnegie Observatories; ChileFil: Hoeflich, P.. Florida State University; Estados UnidosFil: Hsiao, E. Y.. University Aarhus; Dinamarca. Florida State University; Estados UnidosFil: Mazzali, P. A.. Liverpool John Moores University; Reino UnidoFil: Phillips, M. M.. Las Campanas Observatory; ChileFil: Filippenko, A. V.. University of California at Berkeley; Estados UnidosFil: Anderson, J. P.. European Southern Observatory Santiago; ChileFil: Benetti, S.. Osservatorio Astronomico Di Padova; ItaliaFil: Brown, P. J.. Texas A&M University; Estados UnidosFil: Campillay, A.. Las Campanas Observatory; ChileFil: Challis, P.. European Southern Observatory Santiago; ChileFil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; ChileFil: Elias De La Rosa, N.. Osservatorio Astronomico Di Padova; ItaliaFil: Folatelli, Gaston. Texas A&M University; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Foley, R. J.. University of California; Estados UnidosFil: Fraser, M.. University College Dublin; IrlandaFil: Holmbo, S.. University Aarhus; DinamarcaFil: Marion, G. H.. University of Texas at Austin; Estados UnidosFil: Morrell, N.. Las Campanas Observatory; ChileFil: Pan, Y. C.. University of California; Estados UnidosFil: Pignata, G.. Millennium Institute Of Astrophysics; Chile. Universidad Andrés Bello; ChileFil: Suntzeff, N. B.. Texas A&M University; Estados UnidosFil: Taddia, F.. Stockholms Universitet; SueciaFil: Torres Robledo, S.. Las Campanas Observatory; ChileFil: Valenti, S.. University of California at Davis; Estados UnidosEDP Sciences2018-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82546Gall, C.; Stritzinger, M. D.; Ashall, C.; Baron, E.; Burns, C. R.; et al.; Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv; EDP Sciences; Astronomy and Astrophysics; 611; A58; 3-2018; 1-540004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201730886info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2018/03/aa30886-17/aa30886-17.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:46:27Zoai:ri.conicet.gov.ar:11336/82546instacron: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:34982025-09-29 09:46:27.513CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| title |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| spellingShingle |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv Gall, C. Dust, Extinction Supernovae: General Supernovae: Individual: Sn 2007on Supernovae: Individual: Sn 2011iv |
| title_short |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| title_full |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| title_fullStr |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| title_full_unstemmed |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| title_sort |
Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv |
| dc.creator.none.fl_str_mv |
Gall, C. Stritzinger, M. D. Ashall, C. Baron, E. Burns, C. R. Hoeflich, P. Hsiao, E. Y. Mazzali, P. A. Phillips, M. M. Filippenko, A. V. Anderson, J. P. Benetti, S. Brown, P. J. Campillay, A. Challis, P. Contreras, C. Elias De La Rosa, N. Folatelli, Gaston Foley, R. J. Fraser, M. Holmbo, S. Marion, G. H. Morrell, N. Pan, Y. C. Pignata, G. Suntzeff, N. B. Taddia, F. Torres Robledo, S. Valenti, S. |
| author |
Gall, C. |
| author_facet |
Gall, C. Stritzinger, M. D. Ashall, C. Baron, E. Burns, C. R. Hoeflich, P. Hsiao, E. Y. Mazzali, P. A. Phillips, M. M. Filippenko, A. V. Anderson, J. P. Benetti, S. Brown, P. J. Campillay, A. Challis, P. Contreras, C. Elias De La Rosa, N. Folatelli, Gaston Foley, R. J. Fraser, M. Holmbo, S. Marion, G. H. Morrell, N. Pan, Y. C. Pignata, G. Suntzeff, N. B. Taddia, F. Torres Robledo, S. Valenti, S. |
| author_role |
author |
| author2 |
Stritzinger, M. D. Ashall, C. Baron, E. Burns, C. R. Hoeflich, P. Hsiao, E. Y. Mazzali, P. A. Phillips, M. M. Filippenko, A. V. Anderson, J. P. Benetti, S. Brown, P. J. Campillay, A. Challis, P. Contreras, C. Elias De La Rosa, N. Folatelli, Gaston Foley, R. J. Fraser, M. Holmbo, S. Marion, G. H. Morrell, N. Pan, Y. C. Pignata, G. Suntzeff, N. B. Taddia, F. Torres Robledo, S. Valenti, S. |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Dust, Extinction Supernovae: General Supernovae: Individual: Sn 2007on Supernovae: Individual: Sn 2011iv |
| topic |
Dust, Extinction Supernovae: General Supernovae: Individual: Sn 2007on Supernovae: Individual: Sn 2011iv |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by Δm15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B- and H-band magnitudes differ by ~ 0.60 mag and ~0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ~ 14% and ~ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B - V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B - V colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on. Fil: Gall, C.. University Aarhus; Dinamarca Fil: Stritzinger, M. D.. University Aarhus; Dinamarca Fil: Ashall, C.. Liverpool John Moores University; Reino Unido Fil: Baron, E.. Oklahoma State University; Estados Unidos Fil: Burns, C. R.. Carnegie Observatories; Chile Fil: Hoeflich, P.. Florida State University; Estados Unidos Fil: Hsiao, E. Y.. University Aarhus; Dinamarca. Florida State University; Estados Unidos Fil: Mazzali, P. A.. Liverpool John Moores University; Reino Unido Fil: Phillips, M. M.. Las Campanas Observatory; Chile Fil: Filippenko, A. V.. University of California at Berkeley; Estados Unidos Fil: Anderson, J. P.. European Southern Observatory Santiago; Chile Fil: Benetti, S.. Osservatorio Astronomico Di Padova; Italia Fil: Brown, P. J.. Texas A&M University; Estados Unidos Fil: Campillay, A.. Las Campanas Observatory; Chile Fil: Challis, P.. European Southern Observatory Santiago; Chile Fil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; Chile Fil: Elias De La Rosa, N.. Osservatorio Astronomico Di Padova; Italia Fil: Folatelli, Gaston. Texas A&M University; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Foley, R. J.. University of California; Estados Unidos Fil: Fraser, M.. University College Dublin; Irlanda Fil: Holmbo, S.. University Aarhus; Dinamarca Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos Fil: Morrell, N.. Las Campanas Observatory; Chile Fil: Pan, Y. C.. University of California; Estados Unidos Fil: Pignata, G.. Millennium Institute Of Astrophysics; Chile. Universidad Andrés Bello; Chile Fil: Suntzeff, N. B.. Texas A&M University; Estados Unidos Fil: Taddia, F.. Stockholms Universitet; Suecia Fil: Torres Robledo, S.. Las Campanas Observatory; Chile Fil: Valenti, S.. University of California at Davis; Estados Unidos |
| description |
We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by Δm15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B- and H-band magnitudes differ by ~ 0.60 mag and ~0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ~ 14% and ~ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B - V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B - V colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on. |
| publishDate |
2018 |
| dc.date.none.fl_str_mv |
2018-03 |
| 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/11336/82546 Gall, C.; Stritzinger, M. D.; Ashall, C.; Baron, E.; Burns, C. R.; et al.; Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv; EDP Sciences; Astronomy and Astrophysics; 611; A58; 3-2018; 1-54 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/82546 |
| identifier_str_mv |
Gall, C.; Stritzinger, M. D.; Ashall, C.; Baron, E.; Burns, C. R.; et al.; Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv; EDP Sciences; Astronomy and Astrophysics; 611; A58; 3-2018; 1-54 0004-6361 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201730886 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2018/03/aa30886-17/aa30886-17.html |
| 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 |
EDP Sciences |
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EDP Sciences |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |