Bisectors (tenfold expanded top axes) and profiles (bottom) for differently strong Fe I (left column) and Fe II lines (right) in the flux from the full stellar disks for five different stellar models. Temperatures increase top down for the models ‘K8 V’, ‘K2 V’, ‘G1 V’, ‘F7 V’, and ‘F3 V’. Stellar rotation is zero, gravitational redshifts are neglected. For the coolest model, only lines from Fe I were well measurable. Continuum intensity scale is that of the overall stellar spectrum; in crowded spectra of the coolest models, not all lines reach the full continuum.