Notes. The coordinates in columns two and three are measured in casa by fitting a 2D Gaussian to their spatial profile at 7250 Å for cluster galaxies, while for the other galaxies the wavelength of emission lines is used. In column four we present the isophotal magnitude in the F775W-band from HST as determined by Postman et al. (2012), where we matched the locations using the brightest source within 1′′. The fifth column gives the MUSE redshift measured here, with a quality flag (QF) in the sixth column. The quality flag of the redshift shows how accurately the redshift is measured, 1 represents a very certain redshift with multiple lines that give Δz< 0.001, 2 represents redshift where several lines are detected, but because of a lower signal-to-noise ratio or intrinsically wider lines, the redshift varies slightly between different lines (Δz< 0.003). The seventh and eighth columns contain previous redshift determination by Gómez et al. (2012), with their previous IDs. The ninth column quotes redshifts measured with VIMOS from Balestra et al. (in prep.). In the last column we show the classification as active (A) or passive (P) of each galaxy based on the presence of emission lines indicative of activity.