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

Journal
Date Issued
2018
Author(s)
Kuncarayakti, Hanindyo
•
Maeda, Keiichi
•
Ashall, Christopher J.
•
Prentice, Simon J.
•
Mattila, Seppo
•
Kankare, Erkki
•
Fransson, Claes
•
Lundqvist, Peter
•
•
Leloudas, Giorgos
•
Anderson, Joseph P.
•
•
Bersten, Melina C.
•
•
Cartier, Régis
•
Denneau, Larry
•
•
•
Folatelli, Gastón
•
Fraser, Morgan
•
Galbany, Lluís
•
Gall, Christa
•
Gal-Yam, Avishay
•
Gutiérrez, Claudia P.
•
Hamanowicz, Aleksandra
•
Heinze, Ari
•
Inserra, Cosimo
•
Kangas, Tuomas
•
Mazzali, Paolo
•
•
Pignata, Giuliano
•
Rest, Armin
•
Reynolds, Thomas
•
Roy, Rupak
•
Smartt, Stephen J.
•
Smith, Ken W.
•
Sollerman, Jesper
•
Somero, Auni
•
Stalder, Brian
•
Stritzinger, Maximilian
•
Taddia, Francesco
•
•
Tonry, John
•
Weiland, Henry
•
Young, David R.
DOI
Abstract
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 {M}g=-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, \dot{M}∼ 0.02{({∊ }{{H}α }/0.01)}-1 ({v}{wind}/500 km s-1) ({v}{shock}/10,000 km s-1)-3 M ☉ 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.

Based on observations made with the NOT, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. This work is based (in part) on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO program 188.D-3003, 191.D-0935, 197.D-1075. Based on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.

Volume
854
Issue
1
Start page
L14
Uri
Url
Issn Identifier
2041-8205
Ads BibCode
2018ApJ...854L..14K
Rights
open.access
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