Notes. Column 1: Source identification. Column 2: Redshift from the R2700 [OIII]-Hβ lines. Column 3: Relative velocity with respect to z = 6.902, as inferred for the W galaxy from the ALMA [CII] line (see Sect. 5.3). Column 4: Integrated velocity dispersion derived from the [OIII]-Hβ lines in the R2700 integrated spectra, after deconvolving the instrumental profile (Appendix A). Column 5: Effective radius estimated as the largest sigma of a 2D Gaussian fit to source emission, after deconvolving quadratically the PSF profile. To derive the properties of the PSF we used the datacube of the standard star (see Sect. 2.5). For sources with significant continuum emission (C1, C2, C3) the sizes were inferred from a panchromatic image generated from the R100 cube in the 1–5 μm spectral range. For the other sources, which have undetected (or very faint) continuum, the [OIII] image was preferred. For the E galaxy the combination of continuum plus [OIII] was used. The Gaussian fits provided unrealistically small errors. Instead, uncertainties are estimated to be 30%, except for some particularly problematic cases for which 50% was adopted instead, specifically for C3 (edge of the FoV), L2 (faint), and L4 (badly defined). For L5, which is very close to the edge of the FoV, R_e could not be estimated. Column 6: Dynamical mass of the source adopting the calibration by Cappellari et al. (2006) (see Sect. 5.1). Column 7: Distance to spaxel (74, 45), which is estimated to be at the centre of gravity of the system. ⁽¹⁾For L7, the kinematic properties were obtained after the 2D kinematic decomposition of this source and the main component of the E galaxy (Sect. 3.3.3).