"Causal horizon" is not a common name I have seen, but indeed there is a clear distinction made by Rindler (1956, MNRAS 116) between "event horizon" and a "particle horizon." Both types of cosmological horizons depends on the observer.
In short, "an event-horizon, for a given observer $A$, is a (hyper-) surface in space-time which divides all events into two non-empty classes: those that have been, are, or will be observable by A, and those that are forever outside A’s possible powers of observation". A "particle horizon", on the other hand, is defined for an observer $A$ and a time $t$, and divides the instantaneous 3-space (from $A$ perspective) in two regions: those which have been observable by $A$ (or which are causally connected with $A$, it is the same thing) and those which have not been.
FRW flat models with (dark & normal) mass but without cosmological constant (or dark energy) have particle horizons, but no cosmological event horizons: the whole universe will become observable given enough time. On the other hand, the $\Lambda$-CDM universe has both type of horizons. An expanding particle horizon, which will only expands until the dark energy dominates completely the cosmological dynamics. From that point on, the universe will expand very rapidly, our particle horizon will contract, and whatever it has not been at any time within our particle horizon will never be: they are beyond our event horizon.