  We present observations of the T Tauri stars BP Tau, DG Tau, DI Tau, GM Aur,
LkCa 15, RW Aur and V830 Tau, using long baseline infrared interferometry at K
band (2.2 microns) from the Keck Interferometer. The target sources have a
range of mass accretion rates and excess near-infrared emission. The
interferometer is most sensitive to extended emission on characteristic size
scales of 1 to 5 millarcseconds. All sources show evidence for resolved K band
emission on these scales, although a few of the sources are marginally
consistent with being unresolved. We calculate the infrared excess based on
fitting stellar photosphere models to the optical photometry and estimate the
physical size of the emission region using simple geometric models for the
sources with a significant infrared excess. Assuming that the K band resolved
emission traces the inner edge of the dust disk, we compare the measured
characteristic sizes to predicted dust sublimation radii and find that the
models require a range of dust sublimation temperatures and possibly optical
depths within the inner rim to match the measured radii.
