ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software O O O O O O O O O O O O B-Software O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O B-Survey I-Survey I-Survey O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O B-Survey I-Survey O O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: spectra belong to the bright configuration, while lower panel spectra belong to the faint configuration. V total magnitude is in the bottom right inset. The overall S/N is 55, 39, and 15 for the bright spectra, and 9, 6, and 4 for the faint ones. 5. Redshifts We measured galaxy redshifts on the spliced spectra, that is, those extending over the entire wavelength range (3800–9000 Å), in order to gather information both from the blue part of the spectra (where at our redshifts, most optical absorption lines are present) and from the red part of the spectra (where the H + NII region is located). The night sky residuals, present in specific regions of the spectra, have been replaced by interpolated values before measuring the redshifts. On these cleaned spectra we measured both the redshift obtained by cross-correlating the spectrum with that of a template at zero velocity (using the IRAF/xcsao package) and the one obtained from the match of emission lines ( IRAF/emsao ). Each single spectrum was visually inspected by members of the team (A.M., B.P., D.B., J.F., M.G., A.P., A.C.) to ensure that the automatic estimation was correct, and to assign a flag that was then used to derive the final redshift determination. We used: the weighted average of the two determinations if both wereflagged as good; the emission line redshift if the cross-correlation was not convincing; and the cross-correlation redshift if spectra did not contain emission lines (and the cross correlation was reliable). Errors on the redshifts are the errors of the combined measurements of both absorption features and emission features if the two redshift estimates were averaged together, and are single errors on the measurements that do not have emission lines, or where we did not trust the absorption line cross-correlation. Among the original 18 995 spectra, we were able to measure 17 985 redshifts, with a median error of 50 km s and average completeness 95. Figure 4 shows the distribution in redshift of all the OmegaWINGS targets (black line). The filled histogram represents the redshift determinations obtained with the previous WINGS spectroscopic survey ( Cava et al. 2009 ), all in the inner cluster regions. The red histogram shows the new Omega WINGS redshifts. When a new redshift was present, we used this determination instead of the old WINGS one (the difference between the two determinations being peaked at , with a few cases of real mismatches in spectra with low S/N). The number of cluster members with a AAOmega redshift is 7497, that adds to the 2732 galaxies belonging to the clusters for which we had a previous WINGS measurement. This means that the total number of cluster members rises to 10 229 in total. 5.1. Completeness To ensure that we could properly derive global properties from the clusters under scrutiny, and from their galaxy populations, we calculated the spectroscopic completeness as a function of both magnitude and radial distance. The first term is