Others.

VLBI observations of HI absorption (3420-3590 kms^-1) against the active nucleus (0016 or 5 pc) of the highly luminous spiral galaxy NGC 5793 ($v_{\rm sys}$ = 3521 kms^-1; D = 70 Mpc) reveal several components (Gardner et al. 1992). The authors claim that these are probably caused by various clouds moving outwards, and not by a single rotating cloud complex surrounding the nucleus. But a higher sensitivity study and larger bandwidth are definitely needed to solve the issue.

Several strong absorption lines in the radio galaxy 3C293 (z=0.045) have been detected by Haschick & Baan (1985). They can resolve the broad ($\Delta v$ = 480 kms^-1) HI absorption spectrum into more than 10 components, which can be attributed to two different structures: --a) the strongest features are part of a rapidly rotating disk surrounding the nucleus of the galaxy and --b) several high-velocity features which are either red- or blue-shifted are interpreted as clouds falling into and being expelled from the nucleus of 3C293. The observed velocity gradient across the whole 22 continuum structure is 179 kms^-1.

Recent VLA observations of CygnusA, the nearest powerful FRII galaxy (z=0.0565), by Conway & Blanco (1995) also revealed a broad ($\Delta v$ = 270 kms^-1) absorption line against its 15-pc nucleus. It most likely consists of two components arising from a rotating nuclear torus.

Another radio galaxy, NGC 4261 (3C270), shows a rather narrow ($\Delta v$ = 65 kms^-1) HI absorption feature against its nucleus, near the systemic velocity at $\sim$2200 kms^-1 (Jaffe & McNamara 1994).