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Type Ibn supernovae (SNe Ibn) are intriguing stellar explosions whose spectraexhibit narrow helium lines with little hydrogen. They trace the presence ofcircumstellar material (CSM) formed via pre-SN eruptions of theirstripped-envelope progenitors. Early work has generally assumed that SNe Ibncome from massive Wolf-Rayet (WR) stars via single star evolution. In thispaper, we report ultraviolet (UV) and optical observations of two nearby TypeIbn SNe 2006jc and 2015G conducted with the Hubble Space Telescope (HST) atlate times. A point source is detected at the position of SN 2006jc, and weconfirm the conclusion of Maund et al. that it is the progenitor's binarycompanion. Its position on the Hertzsprung-Russell (HR) diagram corresponds toa star that has evolved off the main sequence (MS); further analysis implies alow initial mass for the companion star ($M_2$ $\le$ 11.9$^{+1.2}_{-0.8}$$M_\odot$) and a secondary-to-primary initial mass ratio very close to unity($q$ = $M_2/M_1$ $\sim$ 1); the SN progenitor's hydrogen envelope had beenstripped through binary interaction. We do not detect the binary companion ofSN 2015G. For both SNe, the surrounding stellar populations have relatively oldages and argue against any massive WR stars as their progenitors. These resultssuggest that SNe Ibn may have lower-mass origins in interacting binaries. As aresult, they also provide evidence that the giant eruptions commonly seen inmassive luminous blue variables (LBVs) can also occur in much lower-mass,stripped-envelope stars just before core collapse.

Origins of Type Ibn SNe 2006jc/2015G in interacting binaries and implications for pre-SN eruptions