1997PASP..109..483T

begin{tex}We present Hαradial velocities of KT Per taken during quiescence (1989 November) and outburst (1990 February). Both data sets indicate an orbital period near 3.90 h, confirming the result of Ratering, Bruch, & Diaz (1993). We could not refine the period unambiguously; combining our velocities with those of Ratering, Bruch & Diaz (1993) shows that the period is most likely near 0.1627 d, but a period near 0.1618 d is just possible if one forces coherence between the the outburst and quiescent velocities. Another possibility is that the phase of the emission line velocities in outburst lags that of the quiescent velocities by ∼1/4 cycle. We detect the secondary star, estimate its spectral type as M3, and from this derive a distance of 245±100 pc. After subtracting the secondary contribution, we find that the near-infrared continuum steepens considerably during outburst. KT Per appears to be a normal dwarf nova, although its period is among the shorter dwarf nova periods longward of the 2- to 3-hour gap. An absorption feature near λ6280, which had been noted by Ratering et al., is identified as a telluric O_2 band.