  We present 2.0-2.4micron integral field spectroscopy at adaptive optics
spatial resolution (~0.''1) obtained with the Near-infrared Integral Field
Spectrograph (NIFS) at Gemini North Observatory of six Classical T Tauri stars:
T Tau, DG Tau, XZ Tau, HL Tau, RW Aur and HV Tau C. In all cases, the v=1-0
S(1) (2.12 micron) emission is detected at spatially extended distances from
the central stars. The bulk of the H_2 emission is typically not spatially
coincident with the location of continuum flux. Multiple transitions detected
in the K-band spectra show that H_2 level populations are typical of gas in
thermal equilibrium with excitation temperatures in the 1800K-2300 K range.
Three of the stars have H_2 velocity profiles that are centered at the stellar
radial velocity, and three show velocity shifts with respect to the system.
Each of the stars studied here show observed excitation temperatures, spatial
extents, and kinematics of the H_2 that are most consistent with shock excited
emission from the inner regions of the known Herbig-Haro energy flows or from
wide-angle winds encompassing the outflows rather than predominantly from UV or
X-ray stimulated emission from the central stars. The data presented in this
study highlights the sensitivity of adaptive optics-fed integral field
spectroscopy for spatially resolving emission line structures in the
environments of bright young stars.
