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The Evolution of Galaxies and Stellar Populations', Yale University Observatory, New Haven, p. 157. M. B. ), 'The Evolution of Galaxies and Stellar Populations', Yale University Observatory, New Haven, p. 133. : 1977, Astrophys. , in press. : 1971, Publ. Astron. Soc. Pacific 83, 377. : 1976a, Comments Astrophys. and Space Phys. 6, 139. : 1976b, Monthly Notices Roy. Astron. Soc. 176, 31. M. B. ), 'The Evolution of Galaxies and Stellar Populations', Yale University Observatory, New Haven, p. 97.

This position angle is of particular interest because the position angles PA(R) and PA(L) of the two main constituents of these galaxies, the outer ring and the inner lens-bar system, differ by about 900 for NGC 1291 and by about 60 0 for NGC 1326 (cf. the photographs and the more detailed discussion in Mebold et al. 1978). We find that the HI gas distribution is sufficiently extended in both NGC 1326 (HPW of HI gas = 4 min) and NGC 1291 (lWW = 16 min) that a velocity gradient can be determined.

ROBERTS: We should be cautious in invoking intergalactic HI since we have yet to find such gas except for apparent tidal remnants and the gas in the Sculptor group. The latter is much more complex than described in the discovery paper by Mathewson et al. J. Dufour ultraviolet, blue and yellow plates obtained with the CTIO 4-m telescope have been combined to produce both real-colour (Dufour and Martins 1976, J. Appl. Photogr. Eng. 2, 93) and false-colour photographs of NGC 5128. J. 208, 673). Inspection of the real- and false-colour photographs and of composite images produced with the KPNO Image Picture Processing System shows the following: (I) The main body of NGC 5128 has a brightness profile that obeys de Vaucouleurs' a cr R-~ law for elliptical galaxies.

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