Strong winds are ubiquitous in active galactic nuclei (AGNs) and are widely believed to play a crucial role in AGN feedback and galaxy evolution. However, in galaxy-scale simulations, the effects of winds must typically be implemented through sub-grid prescriptions due to limited resolution. It is therefore essential to constrain wind properties using small-scale studies. Previous work has provided constraints on several wind properties. In this study, we analyze numerical simulation data to investigate the angular distribution of winds launched from both hot and cold accretion flows. For hot accretion flows, we consider both Standard and Normal Evolution and Magnetically Arrested Disk modes. For cold accretion flows, we include models incorporating both line driving and magnetic fields. We further provide fitting formulae for the angular profiles of key wind properties, including density, velocity, and temperature, which can be readily implemented in sub-grid models for AGN feedback simulations. We find that winds from thin disks in our simulations satisfy the criteria for broad absorption line outflows, arising at near-equatorial angles with a covering factor consistent with observations.