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tokens: In Fig. 11 we have plotted both IGAPS r and GaiaG magnitudes on the horizontal axis: despite their being very similar for modest r − i , the relation between them has a growing colour dependence for large r − i , as can be seen in Fig. 12 . A minor factor affecting Fig. 11 is that some IGAPS sources might not have a measured r magnitude (either r I or r U ), and so could not be included. Fig. 12. Differences between IGAPS r I and GaiaG magnitudes as a function of IGAPS r I − i colour. The colour scales according to the density of sources in each bin, with square root intervals. Yellow represents the lowest density of at least four sources per 0.02 × 0.02 mag 2 bin. In the same two areas of 1 sq. deg, we have compared the IGAPS catalogue with Pan-STARRS ( Chambers et al. 2016 ). In this case there are more sources in the Pan-STARRS catalogue. In Fig. 13 we can see that Pan-STARRS is only slightly deeper in the r band. In this figure we are directly comparing Pan-STARRS and IGAPS AB magnitudes that are the same by construction. Crowding accounts for less of the difference in this comparison since both catalogues come from ground-based photometric surveys with a similar pixel scale (0.333 vs. 0.258′′ pixel −1 ) and typical seeing. Fig. 13. Results of the cross-match between IGAPS and Pan-STARRS at l = 60°. In blue, rAB magnitude distribution for the IGAPS sources. In red, r magnitude distribution from Pan-STARRS. In green, sources with both IGAPS and Pan-STARRS values. In cyan, sources in IGAPS not crossmatched with Pan-STARRS. In orange, sources in Pan-STARRS but not in IGAPS. When two r magnitudes are available for an IGAPS source ( rAB I and rAB U ) the mean value is plotted. If only one of the two magnitudes has a value, that value is used and the object is included. 8.5. The fully calibrated colour–colour diagrams The creation of the IGAPS catalogue adds to the available colour–colour diagrams. The first of these to mention is the g − r U , r I − i diagram, which uses the three fully calibrated broad bands. An example, constructed as a density plot from the Galactic longitude range 60° l 65°, is shown in Fig. 14 . The tracks overplotted in red have been computed via synthetic photometry using library spectra (see Appendix D ). As the main sequence (MS) and giant tracks sit very nearly on top of each other, we show only the MS track as a red solid line. A reddening line for an A2V star is also included as a dashed line. The comparison of the catalogue data with these reference tracks points out that all stars to K-type fall within a neat linear strip that follows the reddening vector. Only the M stars break away from this trend, creating the roughly horizontal thinly populated spur at g − r U ∼ 1.5 where nearly unreddened M dwarfs are located. This can be echoed at greater g − r U and r I − i by an even sparser distribution of stars to the right of the main stellar locus. Indeed, in the example shown in Fig. 14 , the density of stars