Pre-supernova abundance profiles for the M25Zm3V0 (non-rotating, left panel) and M25Zm3V4 (rotating, υ_ini/υ_crit = 0.4, right panel) models computed with the rate of ¹⁷O(α,γ)²¹Ne from Best et al. (2013). The abundances of trans-iron elements are not explicitly followed from core O-burning ignition (see text for details). The dashed grey line shows the pre-supernova temperature profile, the scale of which is indicated on the right axis. The shaded grey area represents the remnant. The cyan area represents the zone in which the maximum temperature during a spherical 10⁵¹ erg explosion ranges between 1.8 and 3.7 GK (i.e. the zone in which the explosive p-process takes place).