Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv
Wang,Lingzhi1,2; Contreras,Carlos3; Hu,Maokai4; Hamuy,Mario A.5; Hsiao,Eric Y.6; Sand,David J.7; Anderson,Joseph P.8; Ashall,Chris6; Burns,Christopher R.9; Chen,Juncheng2,10; Diamond,Tiara R.11; Davis,Scott12; F?rster,Francisco13,14; Galbany,Lluís15; González-Gaitán,Santiago16; Gromadzki,Mariusz17; Hoeflich,Peter6; Li,Wenxiong18; Marion,G. H.19; Morrell,Nidia3; Pignata,Giuliano14,20; Prieto,Jose L.14,21; Phillips,Mark M.3; Shahbandeh,Melissa6; Suntzeff,Nicholas B.22; Valenti,Stefano12; Wang,Lifan22; Wang,Xiaofeng18; Young,D. R.23; Yu,Lixin1,2; Zhang,Jujia24,25
Source PublicationThe Astrophysical Journal
AbstractAbstract 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 BVRIYJHKs-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 Δm15(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 μ?=?30.58?±?0.05 mag and assuming H0?=?72 km s?1 Mpc?1, we found that 0.73 M⊙ 56Ni 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 Paβ 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 Mch delayed detonation models and sub-Mch double detonation models.
KeywordType Ia supernovae
WOS IDIOP:0004-637X-904-1-abba82
PublisherThe American Astronomical Society
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Document Type期刊论文
Corresponding AuthorWang,Lingzhi
Affiliation1.Chinese Academy of Sciences, South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, People’s Republic of China
2.CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China
3.Carnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, La Serena, Chile
4.Purple Mountain Observatory, Nanjing, 201008, Jiangsu, People’s Republic of China
5.Vice President and Head of Mission of AURA-O in Chile, Avda Presidente Riesco 5335 Suite 507, Santiago, Chile
6.Department of Physics, Florida State University, Tallahassee, FL 32306, USA
7.Department of Astronomy and Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA
8.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile
9.Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
10.School of Electronics and Information Engineering, Wuzhou University, Wuzhou 543002, People’s Republic of China
11.Private Astronomer;
12.Department of Physics, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USA
13.Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
14.Millennium Institute of Astrophysics, Santiago, Chile
15.Departamento de Física Teórica y del Cosmos, Universidad de Granada, E-18071 Granada, Spain
16.CENTRA/COSTAR, Instituto Superior Técnico, Universidade de Lisboa, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal
17.Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warszawa, Poland
18.Physics Department/Tsinghua Center for Astrophysics, Tsinghua University, Beijing, 100084, People’s Republic of China
19.Department of Astronomy, The University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259, USA
20.Departamento de Ciencias Físicas, Universidad Andres Bello, Avda. República 252, Santiago, 8320000, Chile
21.Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile
22.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, USA
23.Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK
24.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People’s Republic of China
25.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People’s Republic of China
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Wang,Lingzhi,Contreras,Carlos,Hu,Maokai,et al. Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv[J]. The Astrophysical Journal,2020,904(1).
APA Wang,Lingzhi.,Contreras,Carlos.,Hu,Maokai.,Hamuy,Mario A..,Hsiao,Eric Y..,...&Zhang,Jujia.(2020).Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv.The Astrophysical Journal,904(1).
MLA Wang,Lingzhi,et al."Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv".The Astrophysical Journal 904.1(2020).
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