Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties

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Fil: Martinez, Laureano. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina

Detalles Bibliográficos
Autores principales: Martínez, Laureano, Anderson, Joseph, Bersten, Melina C., Hamuy, Mario, González-Gaitán, S., Orellana, Mariana Dominga, Stritzinger, Maximilian, Phillips, Mark, Gutiérrez, Claudia, Burns, C., de Jaeger, T., Ertini, Keila, Folatelli, Gastón, Förster, Francisco, Galbany, L., Hoeflich, Peter, Hsiao, E.Y., Morrell, Nidia I., Pessi, Priscila J., Suntzeff, N.B.
Lenguaje:Inglés
Publicado: EDP Sciences 2022
Materias:
Astronomía
supernovae: general
stars: evolution
stars: massive
Acceso en línea:https://ui.adsabs.harvard.edu/abs/2022arXiv220211220M/abstract
http://rid.unrn.edu.ar/handle/20.500.12049/8458
Aporte de:
Repositorio Institucional Digital de la Universidad Nacional de Río Negro (UNRN) de Universidad Nacional de Río Negro
id I65-R171-20.500.12049-8458
record_format dspace
institution Universidad Nacional de Río Negro
institution_str I-65
repository_str R-171
collection Repositorio Institucional Digital de la Universidad Nacional de Río Negro (UNRN)
language Inglés
orig_language_str_mv en
topic Astronomía
supernovae: general
stars: evolution
stars: massive
Astronomía
spellingShingle Astronomía
supernovae: general
stars: evolution
stars: massive
Astronomía
Martínez, Laureano
Anderson, Joseph
Bersten, Melina C.
Hamuy, Mario
González-Gaitán, S.
Orellana, Mariana Dominga
Stritzinger, Maximilian
Phillips, Mark
Gutiérrez, Claudia
Burns, C.
de Jaeger, T.
Ertini, Keila
Folatelli, Gastón
Förster, Francisco
Galbany, L.
Hoeflich, Peter
Hsiao, E.Y.
Morrell, Nidia I.
Pessi, Priscila J.
Suntzeff, N.B.
Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
topic_facet Astronomía
supernovae: general
stars: evolution
stars: massive
Astronomía
description Fil: Martinez, Laureano. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina
author Martínez, Laureano
Anderson, Joseph
Bersten, Melina C.
Hamuy, Mario
González-Gaitán, S.
Orellana, Mariana Dominga
Stritzinger, Maximilian
Phillips, Mark
Gutiérrez, Claudia
Burns, C.
de Jaeger, T.
Ertini, Keila
Folatelli, Gastón
Förster, Francisco
Galbany, L.
Hoeflich, Peter
Hsiao, E.Y.
Morrell, Nidia I.
Pessi, Priscila J.
Suntzeff, N.B.
author_facet Martínez, Laureano
Anderson, Joseph
Bersten, Melina C.
Hamuy, Mario
González-Gaitán, S.
Orellana, Mariana Dominga
Stritzinger, Maximilian
Phillips, Mark
Gutiérrez, Claudia
Burns, C.
de Jaeger, T.
Ertini, Keila
Folatelli, Gastón
Förster, Francisco
Galbany, L.
Hoeflich, Peter
Hsiao, E.Y.
Morrell, Nidia I.
Pessi, Priscila J.
Suntzeff, N.B.
author_sort Martínez, Laureano
title Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
title_short Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
title_full Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
title_fullStr Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
title_full_unstemmed Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties
title_sort type ii supernovae from the carnegie supernova project-i: iii. understanding sn ii diversity through correlations between physical and observed properties
publisher EDP Sciences
publishDate 2022
url https://ui.adsabs.harvard.edu/abs/2022arXiv220211220M/abstract
http://rid.unrn.edu.ar/handle/20.500.12049/8458
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spelling I65-R171-20.500.12049-84582023-09-13T15:32:28Z application/pdf info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/4.0/ 2022 Fil: Martinez, Laureano. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina Fil: Martinez, Laureano. Universidad Nacional de Río Negro. Río Negro, Argentina. Fil: Bersten, Melina. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina. Fil: Anderson, Joseph. European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile Fil: Hamuy, Mario. Vice President and Head of Mission of AURA-O in Chile, Avda. Presidente Riesco 5335 Suite 507, Santiago, Chile Fil: González-Gaitán, S. CENTRA-Centro de Astrofísica e Gravitaçäo and Departamento de Física, Instituto Superio Técnico, Universidade de Lisboa, Avenida Rovisco Pais, 1049-001 Lisboa, Portugal Fil: Phillips, Mark M. Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile Fil: Gutiérrez, Claudia. Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku, Finland. Fil: Gutiérrez, Claudia. Tuorla Observatory, Department of Physics and Astronomy, FI-20014 University of Turku, Finland. Fil: Gutiérrez, Claudia. Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK. Fil: Burns, C. Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA Fil: de Jaeger, T. Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA Fil: de Jaeger, T. Department of Astronomy, University of California, 501 Campbell Hall, Berkeley, CA 94720-3411, USA. Fil: Ertini, Keila. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA,. La Plata, Argentina. Fil: Ertini, Keila. Instituto de Astrofísica de La Plata (IALP), CCT-CONICET-UNLP. Paseo del Bosque S/N, B1900FWA, La Plata, Argentina. Fil: Folatelli, Gastón.Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA,. La Plata, Argentina. Fil: Folatelli, Gastón. Instituto de Astrofísica de La Plata (IALP), CCT-CONICET-UNLP. Paseo del Bosque S/N, B1900FWA, La Plata, Argentina. Fil: Förster, Francisco. Millennium Institute of Astrophysics, Chile. Fil: Förster, Francisco. Department of Astronomy, Faculty of Physical and Mathematical Sciences, University of Chile Fil: Galbany, L. Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain. Fil: Hoeflich, P. Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA Fil: Hsiao, E. Y. Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA Fil: Morrell, Nidia I. Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile Fil: Orellana, Mariana. Universidad Nacional de Río Negro. Río Negro, Argentina. Fil: Orellana, Mariana. Consejo Nacional de Investigaciones Científicas y Tećnicas (CONICET), Argentina. Fil: Pessi, Priscila J. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA,. La Plata, Argentina. Fil: Pessi, Priscila J. European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile Fil: Suntzeff, N. B. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A\&M University, College Station, TX 77843 Type II supernovae from the Carnegie Supernova Project-I: III. Understanding SN II diversity through correlations between physical and observed properties Martínez, Laureano Anderson, Joseph Bersten, Melina C. Hamuy, Mario González-Gaitán, S. Orellana, Mariana Dominga Stritzinger, Maximilian Phillips, Mark Gutiérrez, Claudia Burns, C. de Jaeger, T. Ertini, Keila Folatelli, Gastón Förster, Francisco Galbany, L. Hoeflich, Peter Hsiao, E.Y. Morrell, Nidia I. Pessi, Priscila J. Suntzeff, N.B. Astronomía supernovae: general stars: evolution stars: massive Astronomía Type II supernovae (SNe II) show a large photometric and spectroscopic diversity which is attributed to the varied physical characteristics of their progenitor and explosion properties. In this study, the third of a series of papers where we analyse a large sample of SNe II observed by the Carnegie Supernova Project-I, we present correlations between their observed and physical properties. Our analysis shows that the explosion energy is the physical property that correlates with the highest number of parameters. We recover previously suggested relationships between the hydrogen-rich envelope mass and the plateau duration, and find that more luminous SNe II with higher expansion velocities, faster declining light curves, and higher 56 Ni masses are consistent with higher-energy explosions. In addition, faster declining SNe II (usually called SNe IIL) are also compatible with more concentrated 56 Ni in the inner regions of the ejecta. Positive trends are found between the initial mass, explosion energy, and 56 Ni mass. While the explosion energy spans the full range explored with our models, the initial mass generally arises from a relatively narrow range. Observable properties were measured from our grid of bolometric LC and photospheric velocity models to determine the effect of each physical parameter on the observed SN II diversity. We argue that the explosion energy is the physical parameter causing the greatest impact on SN II diversity, under the assumption of non-rotating solar-metallicity single-star models used in this study. The inclusion of pre-SN models assuming higher mass loss produces a significant increase in the strength of some correlations, particularly those between the progenitor hydrogen- rich envelope mass and the plateau and optically thick phase durations. These differences clearly show the impact of having different treatments of stellar evolution, implying that changes in the assumption of standard single-star evolution are necessary for a complete understanding of SN II diversity. true Las supernovas de tipo II (SNe II) muestran una gran diversidad fotométrica y espectroscópica que se atribuye a las variadas características físicas de sus progenitores y propiedades de explosión. En este estudio, el tercero de una serie de artículos en los que analizamos una gran muestra de SNe II observada por el Carnegie Supernova Project-I, presentamos correlaciones entre sus propiedades físicas y observadas. Nuestro análisis muestra que la energía de explosión es la propiedad física que se correlaciona con el mayor número de parámetros. Recuperamos las relaciones previamente sugeridas entre la masa de la envoltura rica en hidrógeno y la duración de la meseta, y encontramos que SNe II más luminoso con velocidades de expansión más altas, curvas de luz decrecientes más rápidas y masas de 56 Ni más altas son consistentes con explosiones de mayor energía. Además, los SNe II de disminución más rápida (generalmente llamados SNe IIL) también son compatibles con 56 Ni más concentrado en las regiones internas de la eyección. Se encuentran tendencias positivas entre la masa inicial, la energía de explosión y la masa de 56 Ni. Si bien la energía de la explosión abarca todo el rango explorado con nuestros modelos, la masa inicial generalmente surge de un rango relativamente estrecho. Las propiedades observables se midieron a partir de nuestra cuadrícula de LC bolométrica y modelos de velocidad fotosférica para determinar el efecto de cada parámetro físico en la diversidad SN II observada. Argumentamos que la energía de explosión es el parámetro físico que causa el mayor impacto en la diversidad SN II, bajo el supuesto de modelos de una sola estrella de metalicidad solar no rotatoria utilizados en este estudio. La inclusión de modelos pre-SN que asumen una mayor pérdida de masa produce un aumento significativo en la fuerza de algunas correlaciones, particularmente aquellas entre la masa de la envoltura rica en hidrógeno del progenitor y la meseta y la duración de la fase ópticamente gruesa. Estas diferencias muestran claramente el impacto de tener diferentes tratamientos de la evolución estelar, lo que implica que los cambios en la suposición de la evolución estándar de una sola estrella son necesarios para una comprensión completa de la diversidad SN II. Martínez et al. (2022), A&A, Type II supernovae from theCarnegie Supernova Project-I: paper 3 0004-6361 https://ui.adsabs.harvard.edu/abs/2022arXiv220211220M/abstract http://rid.unrn.edu.ar/handle/20.500.12049/8458 en https://www.aanda.org/ Astronomy & Astrophysics EDP Sciences

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