Top row: AME amplitude (A_sp) as a function of the 100 μm (left), 60 μm (middle), and 12 μm (right) flux density. Bottom row: same as top row, except that the FIR flux densities have been divided by G₀. Symbols are as in Fig. 6. The best-fitting slope fitted to the significant AME regions only is plotted. The Perseus (P) and ρ Ophiuchi (R) clouds are indicated. There is a strong correlation between the AME intensity and infrared tracers of dust, with an improved correlation after dividing by G₀. At 12 μm the fit is made excluding the outlier source G239.40−4.70 (marked).