Top: Production rate of ULXs in terms of the SN rate, and number of observable ULXs per M_⊙ yr^-1 of SFR. Bottom: Final outcomes after a ULX phase, represented as the fraction of the total of ULXs. Wide NS-BH and BH-BH systems correspond to binaries for which the merger time from GWs is longer than 13.8 Gyr, while merging NS-BH and BH-BH systems are compact and/or eccentric enough to merge in less than a Hubble time. Disrupted NS-BH systems correspond to binaries that were disrupted by the kick imparted on the NS, while the number of disrupted BH-BH systems is negligible. Systems marked as Deep Case BB widen significantly, due to mass transfer stripping hydrogen depleted layers of the donor, and we do not model them until core-carbon depletion. A small fraction of systems marked as PISN have secondaries massive enough to explode as PISNe, leaving only the BH produced by the primary. The values for NS-BH binaries and for wide BH-BH binaries depend on the choice of threshold mass for BH formation.