Abstract
We discuss the use of the Fourier fast transform technique in the determination of stellar rotational velocities and its applicability to slow rotators. Specifically, we identify the limiting (smallest) rotational velocity that can be measured as a function of the resolution and signal-to-noise ratio of the observations. We apply this technique to new observations of five T Tauri stars with strong emission. The first measurements of |$v$| sin i for one of these stars, LkHα 264, are presented.
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