Broad-Line Radio Galaxies (BLRG) are the most extreme species of AGN regarding line width and structure of their optical emission line spectra. The FWZI amounts to Δv ≃ 35,000 km s-1 for some objects. Furthermore, the broad line profiles are more structured than these of Seyfert galaxies and show often double hump features (Chen, Halpern, and Filippenko 1989; Halpern 1990; Veilleux and Zheng 1991). The detailed analysis of the line profile variations of these AGN provides a powerful tool to get information about fundamental parameters of the Broad-Line Region (BLR) like size, geometry and especially the kinematics of the line emitting gas (Robinson, Pérez, and Binette 1990; Welsh and Home 1991).

In 1989 we started a monitoring campaign of line profile variations of Broad-Line Radio Galaxies at Calar Alto Observatory/Spain on time scales of weeks to years. In the following we present some examples of emission line profile variations of BLRGs we are studying.

3C390.3 is a well known BLRG with prominent double-peaked Hα emission line profile. The spectra shown in Figure 1 were taken in October 89 and August 92. The line flux was scaled with respect to the narrow forbidden [OIII]λλ4959, 5007 and [OI]λ6300 emission lines. The corresponding difference spectrum is displayed at the bottom of Figure 1. The Hα and the Hβ line profiles show a double-peak structure in the difference spectrum. The humps are separated by Δv ≃ 9,000 km s-1. A component at vrel = 4600 km s-1 described by Veilleux and Zheng (1991) is not visible for these epochs.