[Fe ii] EMISSIONS ASSOCIATED WITH THE YOUNG INTERACTING BINARY UY AURIGAE

We present high-resolution 1.06–1.28 μm spectra toward the interacting binary UY Aur obtained with GEMINI/NIFS and the adaptive optics system Altair. We have detected [Fe ii] λ1.257 μm and He i λ1.083 μm lines from both UY Aur A (the primary source) and UY Aur B (the secondary). In [Fe ii] UY Aur A drives fast and widely opening outflows with an opening angle of ∼90° along a position angle of ∼40°, while UY Aur B is associated with a redshifted knot. The blueshifted and redshifted emissions show a complicated structure between the primary and secondary. The radial velocities of the [Fe ii] emission features are similar for UY Aur A and B: ∼ −100 km s−1 for the blueshifted emission and ∼ +130 km s−1 for the redshifted component. The He i line profile observed toward UY Aur A comprises a central emission feature with deep absorptions at both blueshifted and redshifted velocities. These absorption features may be explained by stellar wind models. The He i line profile of UY Aur B shows only an emission feature.