Major merger rate RMM as a function of redshift and colour for MB ≤ −20−1.1z galaxies. The stars are from the ALHAMBRA photometric survey, the circles from the VVDS-Deep spectroscopic survey, and the inverted triangles from the MGC spectroscopic survey. The dashed line in both panels is the best fit of a power-law to the data. The power-law index of the best fit is labelled in the panels. The coloured area marks the 68% confidence interval of the fit. The dotted lines and the grey areas mark the best fit to the global population shown in Fig. 13. Top panel: red population, selected as galaxies with E/S0 templates in ALHAMBRA, galaxies with NUV − r ≥ 4.25 in the VVDS-Deep, and galaxies with u − r ≥ 2.1 in the MGC. Bottom panel: blue population, selected as galaxies with S/SB templates in ALHAMBRA, galaxies with NUV − r < 4.25 in the VVDS-Deep, and galaxies with u − r < 2.1 in the MGC.
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