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Ho, Anna Y. Q.; Goldstein, Daniel A.; Schulze, Steve; Khatami, David K.; Perley, Daniel A.; Ergon, Mattias; Gal-Yam, Avishay; Corsi, Alessandra; Andreoni, Igor; Barbarino, Cristina; Bellm, Eric C.; Blagorodnova, Nadia; Bright, Joe S.; Burns, E.; Cenko, S. Bradley; Cunningham, Virginia; De, Kishalay; Dekany, Richard; Dugas, Alison; Fender, Rob P.; Fransson, Claes; Fremling, Christoffer; Goldstein, Adam; Graham, Matthew J.; Hale, David; Horesh, Assaf; Hung, Tiara; Kasliwal, Mansi M.; M. Kuin, N. Paul; Kulkarni, S. R.; Kupfer, Thomas; Lunnan, Ragnhild; Masci, Frank J.; Ngeow, Chow-Choong; Nugent, Peter E.; Ofek, Eran O.; Patterson, Maria T.; Petitpas, Glen; Rusholme, Ben; Sai, Hanna; Sfaradi, Itai; Shupe, David L.; Sollerman, Jesper; Soumagnac, Maayane T.; Tachibana, Yutaro; Taddia, Francesco; Walters, Richard; Wang, Xiaofeng; Yao, Yuhan; Zhang, Xinhan
The Astrophysical journal, 12/2019, Letnik: 887, Številka: 2Journal Article
We present detailed observations of ZTF18abukavn (SN2018gep), discovered in high-cadence data from the Zwicky Transient Facility as a rapidly rising (1.4 0.1 mag hr−1) and luminous ( mag) transient. It is spectroscopically classified as a broad-lined stripped-envelope supernova (Ic-BL SN). The high peak luminosity ( ), the short rise time ( in g band), and the blue colors at peak ( ) all resemble the high-redshift Ic-BL iPTF16asu, as well as several other unclassified fast transients. The early discovery of SN2018gep (within an hour of shock breakout) enabled an intensive spectroscopic campaign, including the highest-temperature ( ) spectra of a stripped-envelope SN. A retrospective search revealed luminous ( mag) emission in the days to weeks before explosion, the first definitive detection of precursor emission for a Ic-BL. We find a limit on the isotropic gamma-ray energy release , a limit on X-ray emission , and a limit on radio emission . Taken together, we find that the early ( ) data are best explained by shock breakout in a massive shell of dense circumstellar material (0.02 ) at large radii ( ) that was ejected in eruptive pre-explosion mass-loss episodes. The late-time ( ) light curve requires an additional energy source, which could be the radioactive decay of Ni-56.
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