The saturation in the case of bright stars is shown in
Figure 5.44. The impact of the saturation on the
results of the fluxes and magnitudes has decreased with respect to Gaia EDR2
because of changes in several steps of the calibrations. The figure shows the
residuals when fitting as a function of , or as a function
of and plotting them against the magnitude. Tycho-2 and
Hipparcos data were combined to derive empirical corrections. The corrected magnitudes from the
mean magnitudes in Gaia DR3, can be obtained with the
following equations:
The relationship should only be used in the range mag, the relationship only for mag, and
the relationship only for mag.