According to the reverberation model for broad emission line variability in active galactic nuclei, the emission-line luminosity at a given epoch may be expressed formally as the convolution of the input ionizing continuum light curve with a transfer function, the form of which depends on the properties of the emitting material. The transfer

High-dispersion long-slit spectra reveal several kinematically distinct components to the extended emission line gas in NGC 3516. The symmetry of the velocity field is best explained by a combination of rotational motions with a bent bipolar outflow. The present observations provide some of the best kinematic evidence for mass outflow, although

The activity phase of BF Cygni discovered in May 1989 and which lasted about two years is examined. The UV emission lines, usually strong during quiescence, were not detectable during the outburst. UV high-resolution spectra in the outburst indicate the development of an expanding shell giving rise to a considerable number of violet-shifted

Results of a chemodynamical study of the W-R ring nebula NGC 6888 around the WN6 star WR 136 are presented; the observations combine high spatial and spectral resolution covering most of the optical range in different zones of the nebula. The spectra show an emission system with three different velocity components: -64 km/s, +78 km/s, and +18 km/s

The peculiar giant extragalactic HII region NGC 588 has been observed with the TAURUS Fabry-Perot Spectrograph at the William Hershell Telescope of the Observatorio del Roque de los Muchachos. Velocity maps at the seeing limit were obtained in the lines of Hα and [OIII]lambda 5007. We have studied the kinematics of the gas and its relation with the

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