Notes. Shown here are the expected number of observable ULXs n_ULX per M_⊙ yr^-1 of SFR, the number of produced ULXs per SNe (i.e. the ratio between the formation rates of ULXs, R_ULX, and SN, R_SN), and the expected total X-ray luminosity of galaxies (from sources produced through CHE) per M_⊙ yr^-1 of SFR. In parentheses we indicate separately the number of objects with BHs below the pair-instability gap (M_BH < 60 M_⊙) and above it (M_BH > 130 M_⊙). Also included for the expected number of observable ULXs is the percentage of those systems that would accrete at 3 and 10 times their Eddington rates, while for the formation rates we include the average time that formed ULXs spend as such, ⟨ t_ULX ⟩. The last column is computed under the assumption that the bolometric luminosity from accreting sources is released as X-rays, and that accretion is strictly limited to the Eddington rate. Local rates are estimated using the metallicity distribution of Langer & Norman (2006) at redshift z = 0. A value for the locally weighted galactic L_X,gal is ignored, as the local environment contains many galaxies at higher metallicities, where the total luminosity would be dominated by HMXBs instead of the ULXs described in this work. Values given in terms of SFR are computed assuming a SN rate of 0.01 yr^-1 per 1 M_⊙ yr^-1 SFR.