Left panel: mean metallicity and dispersion taken from the MCMC fit. Errors are taken from the 16th and 68th percentiles of the samples, where a dispersion is resolved; otherwise, an upper limit is shown at the 84th percentile, as seen for ED-2. The grey dashed line in the left panel corresponds to a [Fe/H] of −2 dex, the typical separation between classical dwarf spheroidals and ultra-faint dwarf galaxies. Right panel: FeII dispersion against the velocity dispersion. For the streams with multiple clumps (all except ED-2) in velocity space, the velocity dispersions were calculated from the clump with more than four members. For those outlined in green, the velocity clump from which the dispersion was calculated corresponds to the negative v_z (or v_x for ED-6) stream, and those outlined in blue correspond to the positive v_z stream. The red dashed line in both panels at 0.3 dex represents the typical minimal [Fe/H] spread seen in dwarf galaxies (Simon 2019).