Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling
- Autores
- Martinez, Laureano; Bersten, Melina Cecilia; Anderson, J. P.; Hamuy, Mario; González Gaitán, S.; Förster, F.; Orellana, Mariana Dominga; Stritzinger, Maximilian; Phillips, M. M.; Gutiérrez, C. P.; Burns, C.; Contreras, C.; de Jaeger, T.; Ertini, Keila Yael; Folatelli, Gaston; Galbany, Lluís; Hoeflich, Peter; Hsiao, Eric; Morrell, Nidia Irene; Pessi, Priscila Jael; Suntzeff, Nicholas B.
- Año de publicación
- 2022
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Linking supernovae to their progenitors is a powerful method for furthering our understanding of the physical origin of their observed differences while at the same time testing stellar evolution theory. In this second study of a series of three papers where we characterise type II supernovae (SNe II) to understand their diversity, we derive progenitor properties (initial and ejecta masses and radius), explosion energy, and 56Ni mass and its degree of mixing within the ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie Supernova Project-I and is characterised by a high cadence of SNe II optical and near-infrared light curves and optical spectra that were homogeneously observed and processed. A large grid of hydrodynamical models and a fitting procedure based on Markov chain Monte Carlo methods were used to fit the bolometric light curve and the evolution of the photospheric velocity of 53 SNe II. We infer ejecta masses of between 7.9 and 14.8 M, explosion energies between 0.15 and 1.40 foe, and 56Ni masses between 0.006 and 0.069 M. We define a subset of 24 SNe (the gold sample) with well-sampled bolometric light curves and expansion velocities for which we consider the results more robust. Most SNe II in the gold sample (88%) are found with ejecta masses in the range of 810 M, coming from low zero-age main-sequence masses (912 M). The modelling of the initial-mass distribution of the gold sample gives an upper mass limit of 21.3{+3.8} {-0.4}M and a much steeper distribution than that for a Salpeter massive-star initial mass function (IMF). This IMF incompatibility is due to the large number of low-mass progenitors found when assuming standard stellar evolution. This may imply that high-mass progenitors lose more mass during their lives than predicted. However, a deeper analysis of all stellar evolution assumptions is required to test this hypothesis.
Fil: Martinez, Laureano. 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: Bersten, Melina Cecilia. 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: Anderson, J. P.. European Southern Observatory Chile.; Chile
Fil: Hamuy, Mario. Texas A&M University; Estados Unidos
Fil: González Gaitán, S.. Universidade de Lisboa; Portugal
Fil: Förster, F.. Universidad de Chile.; Chile
Fil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; Argentina
Fil: Stritzinger, Maximilian. University Aarhus; Dinamarca
Fil: Phillips, M. M.. Carnegie Observatories; Estados Unidos
Fil: Gutiérrez, C. P.. University Of Turku; Finlandia
Fil: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados Unidos
Fil: Contreras, C.. Carnegie Observatories; Estados Unidos
Fil: de Jaeger, T.. University Of Hawaii; Estados Unidos
Fil: Ertini, Keila Yael. 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: Folatelli, Gaston. 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: Galbany, Lluís. Institute Of Space Sciences; España
Fil: Hoeflich, Peter. Florida State University; Estados Unidos
Fil: Hsiao, Eric. Florida State University; Estados Unidos
Fil: Morrell, Nidia Irene. Carnegie Observatories; 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: Pessi, Priscila Jael. 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. European Southern Observatory Chile.; Chile
Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos - Materia
-
STARS: EVOLUTION
STARS: MASSIVE
SUPERNOVAE: GENERAL - 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:11336/211912
Ver los metadatos del registro completo
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Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modellingMartinez, LaureanoBersten, Melina CeciliaAnderson, J. P.Hamuy, MarioGonzález Gaitán, S.Förster, F.Orellana, Mariana DomingaStritzinger, MaximilianPhillips, M. M.Gutiérrez, C. P.Burns, C.Contreras, C.de Jaeger, T.Ertini, Keila YaelFolatelli, GastonGalbany, LluísHoeflich, PeterHsiao, EricMorrell, Nidia IrenePessi, Priscila JaelSuntzeff, Nicholas B.STARS: EVOLUTIONSTARS: MASSIVESUPERNOVAE: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Linking supernovae to their progenitors is a powerful method for furthering our understanding of the physical origin of their observed differences while at the same time testing stellar evolution theory. In this second study of a series of three papers where we characterise type II supernovae (SNe II) to understand their diversity, we derive progenitor properties (initial and ejecta masses and radius), explosion energy, and 56Ni mass and its degree of mixing within the ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie Supernova Project-I and is characterised by a high cadence of SNe II optical and near-infrared light curves and optical spectra that were homogeneously observed and processed. A large grid of hydrodynamical models and a fitting procedure based on Markov chain Monte Carlo methods were used to fit the bolometric light curve and the evolution of the photospheric velocity of 53 SNe II. We infer ejecta masses of between 7.9 and 14.8 M, explosion energies between 0.15 and 1.40 foe, and 56Ni masses between 0.006 and 0.069 M. We define a subset of 24 SNe (the gold sample) with well-sampled bolometric light curves and expansion velocities for which we consider the results more robust. Most SNe II in the gold sample (88%) are found with ejecta masses in the range of 810 M, coming from low zero-age main-sequence masses (912 M). The modelling of the initial-mass distribution of the gold sample gives an upper mass limit of 21.3{+3.8} {-0.4}M and a much steeper distribution than that for a Salpeter massive-star initial mass function (IMF). This IMF incompatibility is due to the large number of low-mass progenitors found when assuming standard stellar evolution. This may imply that high-mass progenitors lose more mass during their lives than predicted. However, a deeper analysis of all stellar evolution assumptions is required to test this hypothesis.Fil: Martinez, Laureano. 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: Bersten, Melina Cecilia. 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: Anderson, J. P.. European Southern Observatory Chile.; ChileFil: Hamuy, Mario. Texas A&M University; Estados UnidosFil: González Gaitán, S.. Universidade de Lisboa; PortugalFil: Förster, F.. Universidad de Chile.; ChileFil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; ArgentinaFil: Stritzinger, Maximilian. University Aarhus; DinamarcaFil: Phillips, M. M.. Carnegie Observatories; Estados UnidosFil: Gutiérrez, C. P.. University Of Turku; FinlandiaFil: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados UnidosFil: Contreras, C.. Carnegie Observatories; Estados UnidosFil: de Jaeger, T.. University Of Hawaii; Estados UnidosFil: Ertini, Keila Yael. 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: Folatelli, Gaston. 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: Galbany, Lluís. Institute Of Space Sciences; EspañaFil: Hoeflich, Peter. Florida State University; Estados UnidosFil: Hsiao, Eric. Florida State University; Estados UnidosFil: Morrell, Nidia Irene. Carnegie Observatories; 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: Pessi, Priscila Jael. 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. European Southern Observatory Chile.; ChileFil: Suntzeff, Nicholas B.. Texas A&M University; Estados UnidosEDP Sciences2022-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/211912Martinez, Laureano; Bersten, Melina Cecilia; Anderson, J. P.; Hamuy, Mario; González Gaitán, S.; et al.; Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling; EDP Sciences; Astronomy and Astrophysics; 660; A41; 4-2022; 1-260004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202142076info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2022/04/aa42076-21/aa42076-21.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 Técnicas2025-10-22T11:18:52Zoai:ri.conicet.gov.ar:11336/211912instacron: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:34982025-10-22 11:18:52.935CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| title |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| spellingShingle |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling Martinez, Laureano STARS: EVOLUTION STARS: MASSIVE SUPERNOVAE: GENERAL |
| title_short |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| title_full |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| title_fullStr |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| title_full_unstemmed |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| title_sort |
Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling |
| dc.creator.none.fl_str_mv |
Martinez, Laureano Bersten, Melina Cecilia Anderson, J. P. Hamuy, Mario González Gaitán, S. Förster, F. Orellana, Mariana Dominga Stritzinger, Maximilian Phillips, M. M. Gutiérrez, C. P. Burns, C. Contreras, C. de Jaeger, T. Ertini, Keila Yael Folatelli, Gaston Galbany, Lluís Hoeflich, Peter Hsiao, Eric Morrell, Nidia Irene Pessi, Priscila Jael Suntzeff, Nicholas B. |
| author |
Martinez, Laureano |
| author_facet |
Martinez, Laureano Bersten, Melina Cecilia Anderson, J. P. Hamuy, Mario González Gaitán, S. Förster, F. Orellana, Mariana Dominga Stritzinger, Maximilian Phillips, M. M. Gutiérrez, C. P. Burns, C. Contreras, C. de Jaeger, T. Ertini, Keila Yael Folatelli, Gaston Galbany, Lluís Hoeflich, Peter Hsiao, Eric Morrell, Nidia Irene Pessi, Priscila Jael Suntzeff, Nicholas B. |
| author_role |
author |
| author2 |
Bersten, Melina Cecilia Anderson, J. P. Hamuy, Mario González Gaitán, S. Förster, F. Orellana, Mariana Dominga Stritzinger, Maximilian Phillips, M. M. Gutiérrez, C. P. Burns, C. Contreras, C. de Jaeger, T. Ertini, Keila Yael Folatelli, Gaston Galbany, Lluís Hoeflich, Peter Hsiao, Eric Morrell, Nidia Irene Pessi, Priscila Jael Suntzeff, Nicholas B. |
| author2_role |
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 |
STARS: EVOLUTION STARS: MASSIVE SUPERNOVAE: GENERAL |
| topic |
STARS: EVOLUTION STARS: MASSIVE SUPERNOVAE: GENERAL |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Linking supernovae to their progenitors is a powerful method for furthering our understanding of the physical origin of their observed differences while at the same time testing stellar evolution theory. In this second study of a series of three papers where we characterise type II supernovae (SNe II) to understand their diversity, we derive progenitor properties (initial and ejecta masses and radius), explosion energy, and 56Ni mass and its degree of mixing within the ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie Supernova Project-I and is characterised by a high cadence of SNe II optical and near-infrared light curves and optical spectra that were homogeneously observed and processed. A large grid of hydrodynamical models and a fitting procedure based on Markov chain Monte Carlo methods were used to fit the bolometric light curve and the evolution of the photospheric velocity of 53 SNe II. We infer ejecta masses of between 7.9 and 14.8 M, explosion energies between 0.15 and 1.40 foe, and 56Ni masses between 0.006 and 0.069 M. We define a subset of 24 SNe (the gold sample) with well-sampled bolometric light curves and expansion velocities for which we consider the results more robust. Most SNe II in the gold sample (88%) are found with ejecta masses in the range of 810 M, coming from low zero-age main-sequence masses (912 M). The modelling of the initial-mass distribution of the gold sample gives an upper mass limit of 21.3{+3.8} {-0.4}M and a much steeper distribution than that for a Salpeter massive-star initial mass function (IMF). This IMF incompatibility is due to the large number of low-mass progenitors found when assuming standard stellar evolution. This may imply that high-mass progenitors lose more mass during their lives than predicted. However, a deeper analysis of all stellar evolution assumptions is required to test this hypothesis. Fil: Martinez, Laureano. 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: Bersten, Melina Cecilia. 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: Anderson, J. P.. European Southern Observatory Chile.; Chile Fil: Hamuy, Mario. Texas A&M University; Estados Unidos Fil: González Gaitán, S.. Universidade de Lisboa; Portugal Fil: Förster, F.. Universidad de Chile.; Chile Fil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; Argentina Fil: Stritzinger, Maximilian. University Aarhus; Dinamarca Fil: Phillips, M. M.. Carnegie Observatories; Estados Unidos Fil: Gutiérrez, C. P.. University Of Turku; Finlandia Fil: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados Unidos Fil: Contreras, C.. Carnegie Observatories; Estados Unidos Fil: de Jaeger, T.. University Of Hawaii; Estados Unidos Fil: Ertini, Keila Yael. 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: Folatelli, Gaston. 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: Galbany, Lluís. Institute Of Space Sciences; España Fil: Hoeflich, Peter. Florida State University; Estados Unidos Fil: Hsiao, Eric. Florida State University; Estados Unidos Fil: Morrell, Nidia Irene. Carnegie Observatories; 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: Pessi, Priscila Jael. 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. European Southern Observatory Chile.; Chile Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos |
| description |
Linking supernovae to their progenitors is a powerful method for furthering our understanding of the physical origin of their observed differences while at the same time testing stellar evolution theory. In this second study of a series of three papers where we characterise type II supernovae (SNe II) to understand their diversity, we derive progenitor properties (initial and ejecta masses and radius), explosion energy, and 56Ni mass and its degree of mixing within the ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie Supernova Project-I and is characterised by a high cadence of SNe II optical and near-infrared light curves and optical spectra that were homogeneously observed and processed. A large grid of hydrodynamical models and a fitting procedure based on Markov chain Monte Carlo methods were used to fit the bolometric light curve and the evolution of the photospheric velocity of 53 SNe II. We infer ejecta masses of between 7.9 and 14.8 M, explosion energies between 0.15 and 1.40 foe, and 56Ni masses between 0.006 and 0.069 M. We define a subset of 24 SNe (the gold sample) with well-sampled bolometric light curves and expansion velocities for which we consider the results more robust. Most SNe II in the gold sample (88%) are found with ejecta masses in the range of 810 M, coming from low zero-age main-sequence masses (912 M). The modelling of the initial-mass distribution of the gold sample gives an upper mass limit of 21.3{+3.8} {-0.4}M and a much steeper distribution than that for a Salpeter massive-star initial mass function (IMF). This IMF incompatibility is due to the large number of low-mass progenitors found when assuming standard stellar evolution. This may imply that high-mass progenitors lose more mass during their lives than predicted. However, a deeper analysis of all stellar evolution assumptions is required to test this hypothesis. |
| publishDate |
2022 |
| dc.date.none.fl_str_mv |
2022-04 |
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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/11336/211912 Martinez, Laureano; Bersten, Melina Cecilia; Anderson, J. P.; Hamuy, Mario; González Gaitán, S.; et al.; Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling; EDP Sciences; Astronomy and Astrophysics; 660; A41; 4-2022; 1-26 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/211912 |
| identifier_str_mv |
Martinez, Laureano; Bersten, Melina Cecilia; Anderson, J. P.; Hamuy, Mario; González Gaitán, S.; et al.; Type II supernovae from the Carnegie Supernova Project-I: II. Physical parameter distributions from hydrodynamical modelling; EDP Sciences; Astronomy and Astrophysics; 660; A41; 4-2022; 1-26 0004-6361 CONICET Digital CONICET |
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eng |
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eng |
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openAccess |
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EDP Sciences |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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