  Energy levels, lifetimes, and transition probabilities for transitions
between computed levels of 3d^5 of Fe IV are reported. The E2 and M1 transition
probabilities are compared with earlier theoretical results, often only the
values published by Garstang in 1958. From the available astronomical
observations of optical emission lines arising from the same level, a few
direct tests are now possible and they show consistency with the theoretical
calculations.
