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Optical and near-infrared observations of the nearby SN Ia 2017cbv

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2020
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Wang, Lingzhi
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Optical and near-infrared observations of the nearby SN Ia 2017cbv
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Author
  • Wang, Lingzhi;
  • Contreras, Carlos;
  • Hu, Maokai;
  • Hamuy, Mario A.;
  • Hsiao, Eric Y.;
  • Sand, David J.;
  • Anderson, Joseph P.;
  • Ashall, Chris;
  • Burns, Christopher R.;
  • Chen, Juncheng;
  • Diamond, Tiara R.;
  • Davis, Scott;
  • Forster, Francisco;
  • Galbany, Lluis;
  • González Gaitán, Santiago;
  • Gromadzki, Mariusz;
  • Hoeflich, Peter;
  • Li, Wenxiong;
  • Marion, G. H.;
  • Morrell, Nidia;
  • Pignata, Giuliano;
  • Prieto, José L.;
  • Phillips, Mark M.;
  • Shahbandeh, Melissa;
  • Suntzeff, Nicholas B.;
  • Valenti, Stefano;
  • Wang, Lifan;
  • Wang, Xiaofeng;
  • Young, D. R.;
  • Yu, Lixin;
  • Zhang, Jujia;
Abstract
Supernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHK(s)-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 0.006 mag, with a postmaximum magnitude decline of Delta m(15)(B) = 0.990 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus mu = 30.58 0.05 mag and assuming H-0 = 72 km s(-1) Mpc(-1), we found that 0.73 M Ni-56 was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Pa beta emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other well-observed normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some M-ch delayed detonation models and sub-M-ch double detonation models.
Patrocinador
Chinese Academy of Sciences NSF by the European Union's Horizon 2020 research and innovation program under Marie Sklodowska-Curie grant AST-1613426 AST-1613455 AST-1613472 839090 FCT under Project CRISP PTDC/FIS-AST-31546/2017 UIDB/00099/2020 National Science Foundation (NSF) AST-1821967 1821987 1813708 1813466 1908972 AST-1008962 National Science Foundation (NSF) AST-1817099 National Natural Science Foundation of China (NSFC) 11633002 11761141001 Polish NCN MAESTRO 2014/14/A/ST9/00121 Heising-Simons Foundation 2020-1864 Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) CONICYT FONDECYT 1191038 Ministry of Economy, Development, and Tourism's Millennium Science Initiative IC120009 Millennium Science Initiative ICN12_009 National Aeronautics & Space Administration (NASA) NNH14CK55B GS-2017A-Q-33
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Identifier
URI: https://repositorio.uchile.cl/handle/2250/179412
DOI: 10.3847/1538-4357/abba82
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Astrophysical Journal Volumen: 904 Número: 1 Nov 2020
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