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OPTICAL AND ULTRAVIOLET OBSERVATIONS OF THE VERY YOUNG TYPE IIP SN 2014cx IN NGC 337
Huang, Fang1; Wang, Xiaofeng1; Zampieri, Luca2; Pumo, Maria Letizia3; Arcavi, Iair4,5; Brown, Peter J.6; Graham, Melissa L.7; Filippenko, Alexei V.7; Zheng, WeiKang7; Hosseinzadeh, Griffin4; Howell, D. Andrew4,8; McCully, Curtis4; Rui, Liming1; Valenti, Stefano9; Zhang, Tianmeng10; Zhang JJ(张居甲)11,12; Zhang, Kaicheng1; Wang, Lifan6; Huang, F
发表期刊ASTROPHYSICAL JOURNAL
2016-12-01
卷号832期号:2
DOI10.3847/0004-637X/832/2/139
产权排序第11完成单位
收录类别SCI
关键词Galaxies: Individual (Ngc 337) Supernovae: General Supernovae: Individual (Sn 2014cx)
摘要Extensive photometric and spectroscopic observations are presented for SN 2014cx, a type IIP supernova (SN) exploding in the nearby galaxy NGC 337. The observations are performed in optical and ultraviolet bands, covering from -20 to +400 days from the peak light. The stringent detection limit from prediscovery images suggests that this supernova was actually detected within about 1 day after explosion. Evolution of the very early-time light curve of SN 2014cx is similar to that predicted from a shock breakout and post-shock cooling decline before reaching the optical peak. Our photometric observations show that SN 2014cx has a plateau duration of similar to 100 days, an absolute V-band magnitude of similar to -16.5 mag at t approximate to 50 days, and a nickel mass of 0.056 +/- 0.008 M-circle dot. The spectral evolution of SN 2014cx resembles that of normal SNe IIP like SN 1999em and SN 2004et, except that it has a slightly higher expansion velocity (similar to 4200 km/ s(-1) at approximate to 50 days). From the cooling curve of photospheric temperature, we derive that the progenitor has a pre-explosion radius of similar to 640 R-circle dot, consistent with those obtained from SNEC modeling (similar to 620 R-circle dot) and hydrodynamical modeling of the observables (similar to 570 R-circle dot). Moreover, the hydrodynamical simulations yield a total explosion energy of similar to 0.4 x 10(51) erg, and an ejected mass of similar to 8 M-circle dot. These results indicate that the immediate progenitor of SN 2014cx is likely a red supergiant star with a mass of similar to 10 M-circle dot.
项目资助者Major State Basic Research Development Program(2013CB834903) ; National Natural Science Foundation of China (NSFC grant)(11178003, 11325313, 11633002) ; Strategic Priority Research Program of Emergence of Cosmological Structures of the Chinese Academy of Sciences(XDB09000000) ; NSFC(11203034, 11403096) ; Key Research Program of the CAS(KJZD-EW-M06) ; CAS "Light of West China" Program ; NSF grant(1313484, AST-1211916, PHY-1066293) ; TABASGO Foundation ; Gary and Cynthia Bengier ; Christopher R. Redlich Fund
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-637X
URL查看原文
WOS记录号WOS:000389049800010
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CORE-COLLAPSE SUPERNOVAE ; EXPANDING PHOTOSPHERE METHOD ; EARLY LIGHT CURVES ; DIGITAL SKY SURVEY ; SHOCK BREAKOUT ; P SUPERNOVAE ; DUST FORMATION ; PROGENITORS ; TELESCOPE ; PHOTOMETRY
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被引频次:4[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9784
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
通讯作者Huang, F
作者单位1.Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing, 100084, China
2.INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
3.INAF-Osservatorio Astronomico di Palermo "Giuseppe S. Vaiana," Piazza del Parlamento 1, I-90134 Palermo, Italy
4.Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117, USA
5.Kavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106-4030, USA
6.George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy, Texas A&M University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843, USA
7.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
8.Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USA
9.Department of Physics, University of California, Davis, CA 95616, USA
10.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
11.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
12.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
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Huang, Fang,Wang, Xiaofeng,Zampieri, Luca,et al. OPTICAL AND ULTRAVIOLET OBSERVATIONS OF THE VERY YOUNG TYPE IIP SN 2014cx IN NGC 337[J]. ASTROPHYSICAL JOURNAL,2016,832(2).
APA Huang, Fang.,Wang, Xiaofeng.,Zampieri, Luca.,Pumo, Maria Letizia.,Arcavi, Iair.,...&Huang, F.(2016).OPTICAL AND ULTRAVIOLET OBSERVATIONS OF THE VERY YOUNG TYPE IIP SN 2014cx IN NGC 337.ASTROPHYSICAL JOURNAL,832(2).
MLA Huang, Fang,et al."OPTICAL AND ULTRAVIOLET OBSERVATIONS OF THE VERY YOUNG TYPE IIP SN 2014cx IN NGC 337".ASTROPHYSICAL JOURNAL 832.2(2016).
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