Velocity dispersion profiles and radial velocity curves have been derived for three E-S0 galaxies, namely NGC 1052, NGC 3998, and NGC 4125, both from the emission and the absorption lines. In addition central values of the gas and stellar velocity dispersion are determined for NGC 2749. The gas velocity dispersion is systematically lower than that of the stars by 40 percent-95 percent. There is some indication of similarity in the shape of the gas and stellar velocity dispersion profiles. The rotational properties of gas and stars appear to be strongly decoupled. The possibilities that gas in ellipticals is of internal or external origin are discussed.
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Bertola et al. (1984) studied this question.