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Fig. 3.


Abundance of galaxies as a function of observed magnitude for the different SDSS bands. Symbols show a compilation of observational results from the different datasets, with the measurements from SDSS highlighted as large coloured circles (Yasuda et al. 2001). Shown in each panel are the predictions from our mock galaxy lightcone before and after a correction to apparent magnitudes (solid and dashed lines, respectively) designed to improve the agreement with observations (see Sect. 3.1). The drop in the Yasuda et al. (2001) data in the i and z SDSS bands at faint magnitudes is caused by selection effects. The sample used in that work was selected in r with a magnitude range of 12 ≤ r ≤ 21.

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