In this paper observations of Fe II emission lines of multiplet 49 are
presented for nine southern Be stars. The radial velocity measurement
s performed on the line profiles confirm the results previously obtain
ed by other authors which were derived using single Fe II lines of dif
ferent multiplets. They are of kinematic nature and concern the correl
ations of line widths with the V sin i and the extent of the Fe II lin
e formation region compared to that of Balmer emission lines. The stud
y of multiplet 49 leads us to conclude that its components are optical
ly thick.