Wind density profile (left column) and corresponding emissivity profile (middle column) for a range of outflow velocities (increasing from top to bottom, value given in top left corner of each row). The right column shows the column-density profile for varying lines of sight through the winds. These have all been calculated for a wind launched between r_in = 1000 and r_out = 3000, with $d_f=r_{\mathrm{in}}\sqrt{3}$ and f_cov = 0.9. The mass outflow rate has been set to ṁ = 0.1, for a 10⁸ M_⊙ black hole (where the mass is required to obtain physical units). The velocity profile has been given a scale length of r_v = 500 and exponent β = 1, and the initial density profile (at the base) has κ = −1, weighting the outflow towards smaller radii. As expected, when the outflow velocity increases, the overall density also reduces. In general, the emissivity is weighted more strongly towards the base of the wind, where the density is highest (hence stronger absorption and/or fluorescence). For low velocity (high density), the emission will be strongly weighted to the inner edge of the wind, as now the absorption is sufficiently strong that the internal wind regions do not see significant illumination. Our highest velocity examples are chosen for demonstrative purposes rather than an attempt at a realistic BLR wind.