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Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUESTSurvey and followed by the CSP II at optical and near-IR wavelengths. Ouranalysis indicates LSQ13abf was discovered within two days of explosion and itsfirst 10 days of evolution reveal a B-band light curve with an abrupt drop inluminosity. Contemporaneously, the V-band light curve exhibits a rise towards afirst peak and the r- and i-band light curves show no early peak. The earlylight-curve evolution of LSQ13abf is reminiscent of the post explosion coolingphase observed in the Type Ib SN 2008D, and the similarity between the twoobjects extends over weeks. Spectroscopically, LSQ13abf resembles SN 2008D withP Cygni He I features that strengthen over time. Spectral energy distributionsare constructed from broad-band photometry, and by fitting black-body (BB)functions a UVOIR light curve is constructed, and the underlying BB-temperatureand BB-radius profiles are estimated. Explosion parameters are estimated bysimultaneously fitting an Arnett model to the UVOIR light curve and thevelocity evolution derived from spectral features, and a post-shock breakoutcooling model to the first two epochs of the bolometric evolution. Thiscombined model suggests an explosion energy of 1.3x10$^{51}$ ergs, a relativelyhigh ejecta mass of 5.94 M$_{\odot}$, a Ni mass of 0.16 M$_{\odot}$, and aprogenitor-star radius of 28.0 R$_{\odot}$. The ejecta mass suggests theorigins of LSQ13abf lie with a >25 M$_{\odot}$ ZAMS progenitor and its radiusis three and nine times larger than values estimated from the same analysisapplied to observations of SNe 2008D and 1999ex, respectively. Alternatively,comparison of hydrodynamical simulations of >20-25 M$_{\odot}$ ZAMS progenitorsthat evolve to pre-SN envelope masses around 10 M$_{\odot}$ and extended (~100R$_{\odot}$) envelopes also match the observations of LSQ13abf.

The Carnegie Supernova Project II. Early observations and progenitor constraints of the Type Ib supernova LSQ13abf