Comparison of the observed solar Fe I lines from the FTS KPNO flux atlas (Kurucz et al. 1984) with the synthetic line profiles computed using our 3D RHD Dispatch model (3D RHD) and the MARCS solar model (1D hydrostatic). For both models, the same iron abundance of A(Fe) = 7.50 was used. To compute the MARCS line profiles, we additionally include a microturbulence of 1 km s⁻¹. Except the solar rotation, no other broadening was applied and the synthetic lines were not fit to the observations in any way.