Cumulative halo model power spectra as a function of the upper-limit of halo mass at z = 0. Left-hand panel: matter–matter power spectrum as the upper limit is raised from 10¹⁰ to 10¹⁶ h⁻¹ M_⊙ (i.e. the lightest coloured curve shows the contribution from only haloes below 10¹⁰ h⁻¹ M_⊙), right-hand panel: same but for the matter–electron pressure spectrum. In both cases the converged spectrum from all halo masses is shown in thick black and this has been reached with an upper limit of 10¹⁶ h⁻¹ M_⊙. We see that the matter–matter spectrum builds up fairly gradually with halo mass and that all scales receive contributions from a wide range of halo masses. In contrast, the matter–electron pressure spectrum receives very little contribution from haloes less massive than 10¹³ h⁻¹ M_⊙, with the vast majority of the power coming from haloes between 10¹⁴ and 10¹⁵ h⁻¹ M_⊙.