SIMBAD references

2019ApJ...887..169H - Astrophys. J., 887, 169-169 (2019/December-3)

Evidence for late-stage eruptive mass loss in the progenitor to SN2018gep, a broad-lined IC supernova: pre-explosion emission and a rapidly rising luminous transient.

HO A.Y.Q., GOLDSTEIN D.A., SCHULZE S., KHATAMI D.K., PERLEY D.A., ERGON M., GAL-YAM A., CORSI A., ANDREONI I., BARBARINO C., BELLM E.C., BLAGORODNOVA N., BRIGHT J.S., BURNS E., CENKO S.B., CUNNINGHAM V., DE K., DEKANY R., DUGAS A., FENDER R.P., FRANSSON C., FREMLING C., GOLDSTEIN A., GRAHAM M.J., HALE D., HORESH A., HUNG T., KASLIWAL M.M., KUIN N.P.M., KULKARNI S.R., KUPFER T., LUNNAN R., MASCI F.J., NGEOW C.-C., NUGENT P.E., OFEK E.O., PATTERSON M.T., PETITPAS G., RUSHOLME B., SAI H., SFARADI I., SHUPE D.L., SOLLERMAN J., SOUMAGNAC M.T., TACHIBANA Y., TADDIA F., WALTERS R., WANG X., YAO Y. and ZHANG X.

Abstract (from CDS):

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 (Mg,peak=-20 mag) transient. It is spectroscopically classified as a broad-lined stripped-envelope supernova (Ic-BL SN). The high peak luminosity (Lbol≳3×1044ergs–1), the short rise time (trise=3days in g band), and the blue colors at peak (g–r∼-0.4) 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 (Teff≳40,000K) spectra of a stripped-envelope SN. A retrospective search revealed luminous (Mg∼Mr~-14 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 E_γ,iso_< 4.9×1048erg, a limit on X-ray emission LX< 1040ergs–1, and a limit on radio emission νLν≲1037ergs–1. Taken together, we find that the early (< 10days) data are best explained by shock breakout in a massive shell of dense circumstellar material (0.02 M) at large radii (3×1014cm) that was ejected in eruptive pre-explosion mass-loss episodes. The late-time (> 10days) light curve requires an additional energy source, which could be the radioactive decay of Ni-56.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): methods: observational - shock waves - stars: mass-loss - supernovae: individual - surveys

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 23

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2020.10.24-14:09:07

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