NGC 1068 is a barred galaxy with a very complex nuclear region. Although it is an archetype Seyfert2, at least half of the IR emission arises from star formation (Young, Kleinmann & Allen 1988). High-resolution ($\sim$2) VLA HI absorption measurements carried out by Gallimore et al. (1994) reveal several blue- and red-shifted features against the SW radio lobe and a jet as well as broad (FWHM = 128$\pm$25 kms^-1) double absorption lines against the radio nucleus. The absorption lines cover a total velocity range of $\sim$540 kms^-1, from $\sim$760 to 1300 kms^-1. The two lines against the core are centred at +66$\pm$12 kms^-1 and -295$\pm$9 kms^-1, resulting in a mean offset from $v_{\rm sys}$ of -181 kms^-1. Because of this large offset Gallimore et al. reject circular orbits (which are favoured for many of the galaxies presented here), but prefer a model with two distinct, near-nuclear cloud populations, one falling into and the other flowing out of the radio core, both associated with the fuelling of and exhaust from the central engine. In case of a fast-rotating nuclear ring I would expect the radius to coincide with the inner Lindblad resonance (ILR) induced by the bar potential. It is possible that the absorption lines observed in NGC 1068 are caused by outflow and a nuclear ring as suggested for NGC 253. For comparison see also the summary of HI absorption measurements against the Seyfert galaxy NGC 4151 and the peculiar galaxy NGC 4258 in Section 4.3.

A detailed discussion of NGC 1068 and NGC 4151 is given in the chapter by Brinks & Mundell in this volume.