differs from the previous work in that it uses rotation curves obtained from 2-dimensional velocity fields. In a number of cases this allows a more accurate determination of the rotation curves than was possible with slit spectroscopy. Additionally, a fuller characterization of the kinematics of each galaxy is possible. We show that, with these new data, the T-F relation for compact group galaxies is similar to that for galaxies in less dense environments. The exceptions to this conclusion are seen for some of the least massive galaxies in our sample.

This paper is organized as follows. In Section 2 we present the set of rotation curves that are used. In Section 3 we illustrate and discuss comparisons of rotation curves for several galaxies in common with R1991 and N2000 and we show that 2-D spectroscopy is needed if one wants to accurately describe the kinematics of interacting galaxies. Sections 4 and 5 show the results on the T-F relation and a discussion respectively.

Data
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The data used in this paper are gathered from three publications which studied the kinematics of galaxies in nine compact groups (HCG 10, 16, 19, 87, 88, 89, 90, 91, 96, 100). A detailed description 