Same as Fig. 4, but compared to other direct or indirect IS flux determinations. Top panel a): green (Orion A) and grey (Perseus OB2) dashed areas are γ-ray derived limits from local giant molecular clouds using Fermi-LAT data (Yang et al. 2014); symbols are for low-energy Voyager 1 measurements (Stone et al. 2013) and high-energy data. Bottom panel b): thick lines are from the 68% CI of this analysis; shaded areas correspond to the 68%CI from a likelihood analysis of Fermi-LAT γ-ray emissivity, and PAMELA (2006−2008) plus AMS-01 (1998) p+He+e⁺+e⁻ analysis (Casandjian 2015); chained lines are from a χ²-minimisation analysis of BESS data (Shikaze et al. 2007).