中国科学院机构知识库网格
Chinese Academy of Sciences Institutional Repositories Grid
Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

文献类型:期刊论文

AuthorLi, W.1,2; Wang, X.1; Vinko, J.3,4,5; Mo, J.1; Hosseinzadeh, G.2,6,7; Sand, D. J.8; Zhang JJ(张居甲)9,10,11; Lin, H.1; Zhang, T.12; Wang, L.13,14
SourceASTROPHYSICAL JOURNAL
Issued Date2019
Volume870Issue:1Pages:33
ISSN0004-637X
Keywordsupernovae: general supernovae: individual (SN 2018oh)
DOI10.3847/1538-4357/aaec74
Rank第9完成单位
SubtypeArticle
English Abstract

Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically confirmed Type Ia supernova (SN Ia) observed in the Kepler field. The Kepler data revealed an excess emission in its early light curve, allowing us to place interesting constraints on its progenitor system. Here we present extensive optical, ultraviolet, and nearinfrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3 +/- 0.3 days and Delta m(15)(B) = 0.96 +/- 0.03 mag, but it seems to have bluer B - V colors. We construct the "UVOIR" bolometric light curve having a peak luminosity of 1.49. x. 10(43) erg s(-1), from which we derive a nickel mass as 0.55 +/- 0.04M(circle dot) by fitting radiation diffusion models powered by centrally located Ni-56. Note that the moment when nickel-powered luminosity starts to emerge is + 3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e. g., mixing of Ni-56 to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C. II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

Subject天文学 ; 恒星与银河系
URL查看原文
Publish PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
WOS KeywordHIGH-VELOCITY FEATURES ; WHITE-DWARF MODELS ; LIGHT CURVES ; CIRCUMSTELLAR MATERIAL ; FACTORY OBSERVATIONS ; IMPROVED DISTANCES ; DATA RELEASE ; SN 2011FE ; SPECTRA ; ULTRAVIOLET
Funding ProjectMa Huateng Foundation ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of China (NSFC)[11325313] ; National Natural Science Foundation of China (NSFC)[11633002] ; National Natural Science Foundation of China (NSFC)[11761141001] ; National Program on Key Research and Development Project[2016YFA0400803] ; Tsinghua University Initiative Scientific Research Program[20161080144] ; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201702] ; NSFC[11403096] ; NSFC[11773067] ; NSFC[11573003] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS "Light of West China" Program ; US National Science Foundation[1313484] ; US National Science Foundation[AST-1311862] ; NASA through the Einstein Fellowship Program[PF6-170148] ; NASA's Astrophysics Data Analysis Program[NNX13AF35G] ; NSF[AST-1821967] ; NSF[1821987] ; NSF[1813708] ; NSF[1813466] ; NSF[AST-1515927] ; NSF[AST-0908816] ; NSF[AST-1518052] ; Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)[CE170100013] ; NASA[NNX16AB5G] ; NASA[NNG17PX03C] ; NASA[80NSSC18K0303] ; NASA[NAS5-26555] ; project "Transient Astrophysical Objects" of the National Research, Development and Innovation Office (NKFIH), Hungary - European Union[GINOP 2.3.2-15-2016-00033] ; "Lendulet" Program of the Hungarian Academy of Sciences[LP2012-31] ; "Lendulet" Program of the Hungarian Academy of Sciences[LP2018-7/2018] ; NKFIH[K-115709] ; National Research, Development and Innovation Fund of Hungary under PD_17 funding scheme[PD123910] ; NASA through Hubble Fellowship - Space Telescope Science Institute[HST-HF2-51357.001-A] ; NASA K2 Cycle 4[NNX17AE92G] ; ESO program[199.D-0143] ; STFC through an Ernest Rutherford Fellowship ; EU Horizon 2020 ERC grant[758638] ; EU/FP7-ERC[615929] ; Gordon and Betty Moore Foundation[GBMF5490] ; Mt. Cuba Astronomical Foundation ; Center for Cosmology and AstroParticle Physics at Ohio State University ; Chinese Academy of Sciences South America Center for Astronomy (CASSACA) ; Villum Foundation ; Strategic Priority Research Program-The Emergence of Cosmological Structures of the Chinese Academy of Sciences[11 XDB09000000] ; Special Fund for Astronomy from the Ministry of Finance ; Gordon & Betty Moore Foundation ; Heising-Simons Foundation ; Alfred P. Sloan Foundation ; David and Lucile Packard Foundation ; NASA Science Mission directorate ; NASA K2 cycle 4 grant[NNX17AI64G] ; HST[GO-12577] ; HST[HST AR-12851] ; NASA K2 cycle 5 grant[80NSSC18K0302] ; Chinese Academy of Sciences (CAS)
WOS Research AreaAstronomy & Astrophysics
Language英语
WOS IDWOS:000454551600001
PublisherIOP PUBLISHING LTD
Funding OrganizationMa Huateng Foundation ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of China (NSFC)[11325313, 11633002, 11761141001] ; National Program on Key Research and Development Project[2016YFA0400803] ; Tsinghua University Initiative Scientific Research Program[20161080144] ; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201702] ; NSFC[11403096, 11773067, 11573003] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS "Light of West China" Program ; US National Science Foundation[1313484, AST-1311862] ; NASA through the Einstein Fellowship Program[PF6-170148] ; NASA's Astrophysics Data Analysis Program[NNX13AF35G] ; NSF[AST-1821967, 1821987, 1813708, 1813466, AST-1515927, AST-0908816, AST-1518052] ; Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)[CE170100013] ; NASA[NNX16AB5G, NNG17PX03C, 80NSSC18K0303, NAS5-26555] ; project "Transient Astrophysical Objects" of the National Research, Development and Innovation Office (NKFIH), Hungary - European Union[GINOP 2.3.2-15-2016-00033] ; "Lendulet" Program of the Hungarian Academy of Sciences[LP2012-31] ; Lendulet Program of the Hungarian Academy of Sciences[LP2018-7/2018] ; NKFIH[K-115709] ; National Research, Development and Innovation Fund of Hungary under PD_17 funding scheme[PD123910] ; NASA through Hubble Fellowship - Space Telescope Science Institute[HST-HF2-51357.001-A] ; NASA K2 Cycle 4[NNX17AE92G] ; ESO program[199.D-0143] ; STFC through an Ernest Rutherford Fellowship ; EU Horizon 2020 ERC grant[758638] ; EU/FP7-ERC[615929] ; Gordon and Betty Moore Foundation[GBMF5490] ; Mt. Cuba Astronomical Foundation ; Center for Cosmology and AstroParticle Physics at Ohio State University ; Chinese Academy of Sciences South America Center for Astronomy (CASSACA) ; Villum Foundation ; Strategic Priority Research Program-The Emergence of Cosmological Structures of the Chinese Academy of Sciences[11 XDB09000000] ; Special Fund for Astronomy from the Ministry of Finance ; Gordon & Betty Moore Foundation ; Heising-Simons Foundation ; Alfred P. Sloan Foundation ; David and Lucile Packard Foundation ; NASA Science Mission directorate ; NASA K2 cycle 4 grant[NNX17AI64G] ; HST[GO-12577, HST AR-12851] ; NASA K2 cycle 5 grant[80NSSC18K0302] ; Chinese Academy of Sciences (CAS)
源URL[http://ir.ynao.ac.cn/handle/114a53/18805]  
Collection云南天文台_丽江天文观测站(南方基地)
云南天文台_中国科学院天体结构与演化重点实验室
Corresponding AuthorLi, W.
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People's Republic of China
2.Las Cumbres Observatory, 6740 Cortona Dr. Ste. 102, Goleta, CA 93117-5575, USA
3.Konkoly Observatory, MTA CSFK, Konkoly Thege M. ut 15-17, Budapest, 1121, Hungary
4.Department of Optics & Quantum Electronics, University of Szeged, Dom ter 9, Szeged, 6720 Hungary
5.Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
6.Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA
7.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
8.Steward Observatory, University of Arizona, 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USA
9.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, People's Republic of China
10.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
Recommended Citation
GB/T 7714
Li, W.,Wang, X.,Vinko, J.,et al. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations[J]. ASTROPHYSICAL JOURNAL,2019,870(1):33.
APA Li, W..,Wang, X..,Vinko, J..,Mo, J..,Hosseinzadeh, G..,...&Elsaesser, B..(2019).Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations.ASTROPHYSICAL JOURNAL,870(1),33.
MLA Li, W.,et al."Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations".ASTROPHYSICAL JOURNAL 870.1(2019):33.

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来源:云南天文台

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