A micro-molecular bipolar outflow from HL Tauri

We present detailed geometry and kinematics of the inner outflow toward HL Tau observed using Near Infrared Integral Field Spectrograph (NIFS) at the Gemini-North 8 m Observatory. We analyzed H-2 2.122 mu m emission and [Fe II] 1.644 mu m line emission as well as the adjacent continuum observed at a <0.2 resolution. The H-2 emission shows (1) a bubble like geometry to the northeast of the star, as briefly reported in the previous paper, and ( 2) faint emission in the southwest counterflow, which has been revealed through careful analysis. The emission on both sides of the star shows an arc 1.0 away from the star, exhibiting a bipolar symmetry. Different brightnesses and morphologies in the northeast and southwest flows are attributed to absorption and obscuration of the latter by a flattened envelope and a circumstellar disk. The H 2 emission shows a remarkably different morphology from the collimated jet seen in [Fe II] emission. The positions of some features coincide with scattering continuum, indicating that these are associated with cavities in the dusty envelope. Such properties are similar to millimeter CO outflows, although the spatial scale of the H 2 outflow in our image (similar to 150 AU) is strikingly smaller than the millimeter outflows, which often extend over 1000-10000 AU scales. The position velocity diagrams of the H-2 and [Fe II] emission do not show any evidence for kinematic interaction between these flows. All results described above support the scenario that the jet is surrounded by an unseen wide-angled wind, which interacts with the ambient gas and produces the bipolar cavity and shocked H-2 emission.