TY - JOUR
T1 - SN 2017dio
T2 - A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium
AU - Kuncarayakti, Hanindyo
AU - Maeda, Keiichi
AU - Ashall, Christopher J.
AU - Prentice, Simon J.
AU - Mattila, Seppo
AU - Kankare, Erkki
AU - Fransson, Claes
AU - Lundqvist, Peter
AU - Pastorello, Andrea
AU - Leloudas, Giorgos
AU - Anderson, Joseph P.
AU - Benetti, Stefano
AU - Bersten, Melina C.
AU - Cappellaro, Enrico
AU - Cartier, Regis
AU - Denneau, Larry
AU - Della Valle, Massimo
AU - Elias-Rosa, Nancy
AU - Folatelli, Gaston
AU - Fraser, Morgan
AU - Galbany, Lluis
AU - Gall, Christa
AU - Gal-Yam, Avishay
AU - Gutierrez, Claudia P.
AU - Hamanowicz, Aleksandra
AU - Heinze, Ari
AU - Inserra, Cosimo
AU - Kangas, Tuomas
AU - Mazzali, Paolo
AU - Melandri, Andrea
AU - Pignata, Giuliano
AU - Rest, Armin
AU - Reynolds, Thomas
AU - Roy, Rupak
AU - Smartt, Stephen J.
AU - Smith, Ken W.
AU - Sollerman, Jesper
AU - Somero, Auni
AU - Stalder, Brian
AU - Stritzinger, Maximilian
AU - Taddia, Francesco
AU - Tomasella, Lina
AU - Tonry, John
AU - Weiland, Henry
AU - Young, David R.
N1 - We thank the referee and Sung-Chul Yoon for useful suggestions. K.M. acknowledges the FINCA visitor program, Japan Society for the Promotion of Science (JSPS) through KAKENHI Grant 17H02864 and JSPS Open Partnership Bilateral Joint Research Project between Japan and Chile. L.G. was supported by the US National Science Foundation, Grant AST-1311862. C.P.G. acknowledges EU/FP7-ERC grant No. [615929]. A.P., S.B., L.T., and N.E.R. are supported by the PRIN-INAF 2014 project Transient Universe: unveiling new types of stellar explosions with PESSTO. Support for G.P. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. C.G. is supported by the Carlsberg Foundation. M.D.S. is supported by a research grant (13261) from the VILLUM FONDEN. NUTS is supported in part by IDA (Instrumentcenter for Danish Astrophysics). The ATLAS surveys are funded through NASA grants NNX12AR55G. A.G.-Y. is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program and by a Kimmel award.
PY - 2018/2/10
Y1 - 2018/2/10
N2 - 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, M similar to 0.02 (epsilon(H alpha)/0.01)(-1) (nu(wind)/500 km s(-1)) (nu(shock)/10,000 km s(-1))M--3(circle dot) 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.
AB - 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, M similar to 0.02 (epsilon(H alpha)/0.01)(-1) (nu(wind)/500 km s(-1)) (nu(shock)/10,000 km s(-1))M--3(circle dot) 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.
UR - http://www.scopus.com/inward/record.url?scp=85042130903&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/aaaa1a
DO - 10.3847/2041-8213/aaaa1a
M3 - مقالة
SN - 2041-8205
VL - 854
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - 14
ER -