Line bisectors of quiet and active solar regions from the disk center (μ = 1.0) to the limb (μ = 0.2). Continuous lines: line bisectors of quiet solar disk at 14 different heliocentric positions measured from Ellwarth et al. (2023), similar to Fig. 11 of Ellwarth et al. (2023). Unlike in Fig. 8 of Zhao & Dumusque (2023), we do not inject the bisectors of the quiet region into the spectra, as they are naturally included. Dotted lines: fit of the bisectors of the FeI 6301.5008 Å spectral line inside a facula region, as measured by the Fabry-Perot interferometer at the Donati Solar Tower (Cavallini et al. 1985). Below a depth of 0.5 a linear fit is performed, while a fifth-order polynomial is used to model the top part of the bisector. To prevent unrealistic values when interpolating the polynomial above a normalized flux of 0.9 where no measurement exists, we selected the most redshifted part of the top bisector, explaining the vertical values for very shallow depths. The bisector of active regions at different μ angles are all shifted by 350 m/s based on our hypothesis that convection is fully suppressed in magnetic regions.