Notes. (a) For the inner binaries: P, 𝒯₀, 𝒜_ETV, D are the period, reference time of a primary minimum, half-amplitude of the ETV curve, and the full duration of an eclipse, respectively. 𝒯₀ is given in BJD – 2 400 000, while the other quantities are in days. For all those triples where the inner eccentricities are very small and, hence, the shifts of the secondary eclipses relative to phase 0.5 are negligible (quantitatively, they are much smaller than the full durations of the individual eclipses), the same reference times and periods can be used to predict the times of the secondary eclipses. In the case of the three eccentric EBs we give a separate period and reference time for the secondary eclipses, listing them below the primary ephemerides. (b) For the outer orbits we give separate reference times for the third body eclipses around the inferior and superior conjunctions of the tertiary component. The eclipse durations, D, of the third-body eclipses do not give the extent of any specific third body events. Rather D represents the time difference corresponding to the very first and last moments around a given third-body conjunction when the first/last contact of a third-body event may occur). Double dots (:) call attention to the less certain superior/inferior conjunction times at those types of third-body events (i.e., primary vs. secondary outer eclipses) because they were not observed by TESS. Conjunction data, in parentheses, indicate that only very shallow third-body eclipses may occur which can hardly be observed with ground-based instruments.