Notes. Columns 2 and 3 give the number of catalogue entries that fall within the Euclid FoV and the number matched sources within 3″.5, respectively. Columns (4)–(7) list properties of the surveys: the spatial coverage, the limiting surface brightness, the primary telescope used for the survey, and the filters used. The Kang et al. (2024), Meusinger et al. (2020), and Wittmann et al. (2019) samples are further separated into dwarf and non-dwarf members (see text) for better comparison. ^(a) Meusinger et al. (2020) also utilise several auxiliary data sources: spectra and u, g, r, i, and z imaging from SDSS; B, V, and R imaging and optical spectra from the CAHA telescope at Calar Alto; NED; WISE; and Hα data from the literature. ^(b)Here we define a dwarf as any galaxy with M_r,SDSS > −18 or log₁₀ M_*/M_⊙ ≤ 9.0. ^(c)In addition to the WHT imaging, Wittmann et al. (2019) used archival Subaru HSC data in g, r, and z bands as auxiliary datasets to obtain colours and the 0.″5 seeing conditions for the morphological classifications. The HSC g band reached a limiting surface brightness of 28.8 mag arcsec⁻⁻². ^(d)Only partial U band coverage is available.