Figure 11.

Environment sampled by the SN 2014C shock evolves from the typical low-density environment around Ib/c SNe and WR stars, to the dense and rich environment typical of SNe that develop signatures of strong interaction with the medium (i.e., type-IIn SNe, here represented with black dots, data from Kiewe et al. 2012). H-poor SNe are represented with diagonal lines since the observations constrain the density ρ, which is $\propto \dot{M}/v_w$. Black, blue, and dotted purple lines are used for the sample of type Ic-BL, Ib/c, and IIb SNe from Drout et al. (2015). The properties of galactic WR stars are from Crowther (2007), while WN3/O3 stars are from Massey et al. (2015). Locations of red supergiants environments (RSG) are from de Jager et al. (1988), Marshall et al. (2004), and van Loon et al. (2005), while the typical locations of Luminous Blue Variable (LBV) winds and eruptions are inferred from Smith (2014) and Smith & Owocki (2006). For the common envelope (CE) ejection due to binary interaction, we use here a typical timescale of 1 year.