SN 2017dio: A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium

• Autores: Kuncarayakti, Hanindyo; Maeda, Keiichi; Ashall, Christopher J.; Prentice, Simon J.; Mattila, Seppo; Kankare, Erkki; Fransson, Claes; Lundqvist, Peter; Pastorello, Andrea; Leloudas, Giorgos; Anderson, Joseph P.; Benetti, Stefano; Bersten, Melina Cecilia; Cappellaro, Enrico; Cartier, Régis; Denneau, Larry; Della Valle, Massimo; Elias Rosa, Nancy; Folatelli, Gaston; Fraser, Morgan; Galbany, Lluís; Gall, Christa; Gal-Yam, Avishay; Gutiérrez, Claudia P.; Hamanowicz, Aleksandra; Heinze, Ari; Inserra, Cosimo; Kangas, Tuomas; Mazzali, Paolo; Melandri, Andrea; Pignata, Giuliano; Rest, Armin; Reynolds, Thomas; Roy, Rupak; Smartt, Stephen J.; Smith, Ken W.; Sollerman, Jesper; Somero, Auni; Stalder, Brian; Stritzinger, Maximilian; Taddia, Francesco; Tomasella, Lina; Tonry, John; Weiland, Henry; Young, David R.
• Año de publicación: 2018
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: SUPERNOVAE: GENERAL; SUPERNOVAE: INDIVIDUAL (SN 2017DIO)
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

SN 2017dio shows both spectral characteristics of a type-Ic supernova (SN) and signs of a hydrogen-rich circumstellar medium (CSM). Prominent, narrow emission lines of H and He are superposed on the continuum. Subsequent evolution revealed that the SN ejecta are interacting with the CSM. The initial SN Ic identification was confirmed by removing the CSM interaction component from the spectrum and comparing with known SNe Ic and, reversely, adding a CSM interaction component to the spectra of known SNe Ic and comparing them to SN 2017dio. Excellent agreement was obtained with both procedures, reinforcing the SN Ic classification. The light curve constrains the pre-interaction SN Ic peak absolute magnitude to be around Mg = -17.6 mag. No evidence of significant extinction is found, ruling out a brighter luminosity required by an SN Ia classification. These pieces of evidence support the view that SN 2017dio is an SN Ic, and therefore the first firm case of an SN Ic with signatures of hydrogen-rich CSM in the early spectrum. The CSM is unlikely to have been shaped by steady-state stellar winds. The mass loss of the progenitor star must have been intense, M ∼ 0.02 ϵ Hα/0.01) -1 (v wind /500 km s -1 ) (v shock 10,000 km s-1 ) -3 Me yr -1 , peaking at a few decades before the SN. Such a high mass-loss rate might have been experienced by the progenitor through eruptions or binary stripping.
Fil: Kuncarayakti, Hanindyo. University of Turku; Finlandia
Fil: Maeda, Keiichi. University of Turku; Finlandia
Fil: Ashall, Christopher J.. Kyoto University; Japón
Fil: Prentice, Simon J.. University of Tokyo; Japón
Fil: Mattila, Seppo. Liverpool John Moores University; Reino Unido
Fil: Kankare, Erkki. Florida State University; Estados Unidos
Fil: Fransson, Claes. Liverpool John Moores University; Reino Unido
Fil: Lundqvist, Peter. Kyoto University; Japón
Fil: Pastorello, Andrea. The Queens University of Belfast; Irlanda
Fil: Leloudas, Giorgos. Stockholms Universitet; Suecia
Fil: Anderson, Joseph P.. Stockholms Universitet; Suecia
Fil: Benetti, Stefano. Osservatorio Astronomico Di Padova; Italia
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: Cappellaro, Enrico. European Southern Observatory; Chile
Fil: Cartier, Régis. Osservatorio Astronomico Di Padova; Italia
Fil: Denneau, Larry. University of Tokyo; Japón
Fil: Della Valle, Massimo. International Center For Relativistic Astrophysics; Estados Unidos
Fil: Elias Rosa, Nancy. Osservatorio Astronomico Di Padova; Italia
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: Fraser, Morgan. Cerro Tololo Inter American Observatory; Chile
Fil: Galbany, Lluís. University of Hawaii at Manoa; Estados Unidos
Fil: Gall, Christa. nternational Center For Relativistic Astrophysics; Estados Unidos
Fil: Gal-Yam, Avishay. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Gutiérrez, Claudia P.. Osservatorio Astronomico Di Padova; Italia
Fil: Hamanowicz, Aleksandra. European Southern Observatory; Chile
Fil: Heinze, Ari. University Of Tokyo; Japón
Fil: Inserra, Cosimo. The Queens University of Belfast; Irlanda
Fil: Kangas, Tuomas. University College Dublin; Irlanda
Fil: Mazzali, Paolo. University of Pittsburgh at Johnstown; Estados Unidos
Fil: Melandri, Andrea. University of Pittsburgh; Estados Unidos
Fil: Pignata, Giuliano. University Aarhus; Dinamarca
Fil: Rest, Armin. Niels Bohr Institute; Alemania
Fil: Reynolds, Thomas. Weizmann Institute Of Science Israel; Israel
Fil: Roy, Rupak. University of Southampton; Reino Unido
Fil: Smartt, Stephen J.. European Southern Observatory; Chile
Fil: Smith, Ken W.. Uniwersytet Warszawski; Argentina
Fil: Sollerman, Jesper. University of Hawaii at Manoa; Estados Unidos
Fil: Somero, Auni. University of Southampton; Reino Unido
Fil: Stalder, Brian. The Queens University of Belfast; Irlanda
Fil: Stritzinger, Maximilian. Space Telescope Science Institute; Estados Unidos
Fil: Taddia, Francesco. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Tomasella, Lina. Liverpool John Moores University; Reino Unido
Fil: Tonry, John. Osservatorio Astronomico Di Brera; Italia
Fil: Weiland, Henry. Universidad Andrés Bello; Chile
Fil: Young, David R.. Space Telescope Science Institute; Estados Unidos