Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau
Dong,Yize1; Valenti,S.1; Bostroem,K. A.1; Sand,D. J.2; Andrews,Jennifer E.2; Galbany,L.3; Jha,Saurabh W.4; Eweis,Youssef4,5; Kwok,Lindsey4; Hsiao,E. Y.6; Davis,Scott1; Brown,Peter J.7; Kuncarayakti,H.8,9; Maeda,Keiichi10,11; Rho,Jeonghee12; Amaro,R. C.2; Anderson,J. P.13; Arcavi,Iair14,15; Burke,Jamison16,17; Dastidar,Raya18,19; Folatelli,Gastón11,20,21; Haislip,Joshua22; Hiramatsu,Daichi16,17; Hosseinzadeh,Griffin23; Howell,D. Andrew16,17; Jencson,J.2; Kouprianov,Vladimir22; Lundquist,M.2; Lyman,J. D.24; McCully,Curtis16,17; Misra,Kuntal18; Reichart,Daniel E.22; Sánchez,S. F.25; Smith,Nathan2; Wang,Xiaofeng26; Wang,Lingzhi27,28; Wyatt,S.2
Source PublicationThe Astrophysical Journal
AbstractAbstract We present multiband photometry and spectroscopy of SN?2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN?2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of ?16.73?±?0.32 at maximum and a decline rate of 0.21?±?0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8?±?5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN?2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN?2018cuf was most likely a red supergiant of about 14.5 M⊙ that produced 0.04?±?0.01 M⊙ 56Ni during the explosion. We also found ~0.07 M⊙ of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ~11,000 km s?1 were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN.
KeywordCore-collapse supernovae Type II supernovae
WOS IDIOP:0004-637X-906-1-abc417
PublisherThe American Astronomical Society
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Document Type期刊论文
Corresponding AuthorDong,Yize
Affiliation1.Department of Physics and Astronomy, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USA;
2.Steward Observatory, University of Arizona, 933 North Cherry Avenue, Room N204, Tucson, AZ 85721-0065, USA
3.Departamento de Física Teórica y del Cosmos, Universidad de Granada, E-18071 Granada, Spain
4.Department of Physics and Astronomy, Rutgers, the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA
5.Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA
6.Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA
7.Department of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX 77843, USA
8.Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku FI-20014, Finland
9.Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Turku FI-20014, Finland
10.Department of Astronomy, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan
11.Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
12.SETI Institute, 189 North Bernardo Avenue, Mountain View, CA 94043, USA
13.European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 190001, Santiago, Chile
14.The School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
15.CIFAR Azrieli Global Scholars Program, CIFAR, Toronto, Canada
16.Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA
17.Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA
18.Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263 001, India
19.Department of Physics & Astrophysics, University of Delhi, Delhi-110 007, India
20.Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA La Plata, Argentina
21.Instituto de Astrofísica de La Plata (IALP), CONICET, Argentina
22.Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA
23.Center for Astrophysics∣Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA
24.Department of Physics, University of Warwick, Coventry CV4 7AL, UK
25.Instituto de Astronomía, Universidad Nacional Autónoma de México Circuito Exterior, Ciudad Universitaria, Ciudad de México 04510, Mexico
26.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of China
27.CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China
28.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, People’s Republic of China
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Dong,Yize,Valenti,S.,Bostroem,K. A.,et al. Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau[J]. The Astrophysical Journal,2020,906(1).
APA Dong,Yize.,Valenti,S..,Bostroem,K. A..,Sand,D. J..,Andrews,Jennifer E..,...&Wyatt,S..(2020).Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau.The Astrophysical Journal,906(1).
MLA Dong,Yize,et al."Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau".The Astrophysical Journal 906.1(2020).
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