Relative humidity (slices of one horizontal dimension) during convective storms, from methane-rich latitudes to methane-poor latitudes, taken from our simulations in ice giants and inspired by latitudinal and vertical variations shown by observations. The simulations were run with different theoretical methane concentrations in the deep atmosphere. Uranus: Observations show latitudinal variations of 1–4% in methane at 2 bar (Sromovsky et al. 2019), from pole to equator. The relative humidity is plotted from simulations with three different methane specific concentrations: 0.05, 0.125, and 0.20 kg/kg. These correspond to volume mixing ratios of 0.8, 2.1, and 3.6% respectively. Neptune: Observations show latitudinal variations of 2–6% in methane at 4 bar (Irwin et al. 2021), from pole to equator. The relative humidity is plotted from our simulations with three different methane specific concentrations: 0.125, 0.20, and 0.30 kg/kg. These correspond to volume mixing ratios of 2.1, 3.6, and 6.2% respectively. The simulation with q_deep = 0.05 kg/kg is no longer plotted since this configuration might not exist on Neptune. We see powerful but rare storms at methane-poor latitudes and weak but frequent storms at methane-rich latitudes. The more methane there is, the more frequent storms are, but also the weaker they are. To make these plots, we ran three more short simulations with q_deep = 0.125 kg/kg CH₄ in Uranus, q_deep = 0.125 and 0.20 kg/kg CH₄ in Neptune, in addition to our simulations already presented and detailed in this article.