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By E. Nelson, Charles Best, W.G. McLean, Merle Potter

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4). Similarly, our seeingcorrected core parameters agree well provided that we both resolved the galaxy. 3 for 1 galaxy with resolution class III ("unresolved"). This shows (i) that the measurements agree well, (ii) that Lauer's seeing corrections are accurate when they are not too large, and (iii) that when his seeing corrections are large, they are underestimated. The same is probably true of my seeing corrections. 1 mag arcsec- 2 over many magnitudes. CCDs should be able to do better. However, this is accurate enough to allow large improvements over photographic work.

H. Freeman). , 1982. D. Thesis, Australian National University. M. , 1985. Mon. Not. R. astr. , 214, 177. Sandage, A. , 1981. A Revised Shapley-Ames Catalogue of Bright Galaxies (Washington: Carnegie Institution of Washington) . J. , 1985. Mon. Not. R. astr. , 217, 87. , 1983. In Internal Kinematics and Dynamics of Galaxies, ed. E. Athanassoula (Dordrecht: Reidel). , 1975. Astron. , 80, 175. , 1981. Astrophys. , 244, 458. ISOPHOTE SHAPES 45 DISCUSSION King: My impression, based on a small sample, was that galaxies with appreciable central ellipticities have steeper rotation curves, while if a galaxy is round in the center but flattened farther out, it has a rotation curve that rises very slowly.

Porter: You said that the different central values of the distribution function in ellipticals and disks argues against formation of ellipticals by dissipationless mergers of disks-but would you expect disks to merge without dissipation? Or do you think the differences in fo are large enough to argue against mergers anyway? Kormendy: This question should really be addressed to Ray Carlberg, whose work I was summarizing. As I understand it, the argument excludes only dissipationless mergers of stellar disks.

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