We present [Fe ii] ⋋ 1.257 μm spectra toward the interacting binary UY Aur with 0:0014 angular resolution, obtained with the Near infrared Integral Field Spectrograph (NIFS) combined with the adaptive optics system Altair of the GEMINI observatory. In the [Fe ii] emission, UY Aur A (primary) is brighter than UY Aur B (secondary). The blueshifted and redshifted emission between the primary and secondary show a complicated structure. The radial velocities of the [Fe ii] emission features are similar for UY Aur A and B: ~ —100 km s-1 and ~ +130 km s-1 for the blueshifted and redshifted components, respectively. Considering the morphologies of the [Fe ii] emissions and bipolar out ow context, we concluded that UY Aur A drives fast and widely opening out ows with an opening angle of ~90° while UY Aur B has micro collimated jets.

ABSTRACT
1. INTRODUCTION
2. OBSERVATIONS AND DATA REDUCTION
3. BLUESHIFTED AND REDSHIFTED [Fe ii] emission
REFERENCES

• Tae-Soo Pyo(Subaru Telescope, National Astronomical Observatory of Japan/School of Mathematical and Physical Science, The Graduate University for Advanced Studies (SOKENDAI))
• Masahiko Hayashi(School of Mathematical and Physical Science, The Graduate University for Advanced Studies (SOKENDAI)/National Astronomical Observatory of Japan)
• Tracy Beck(Space Telescope Science Institute)
• Christopher J. Davis(Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park)
• Michihiro Takami(Institute of Astronomy and Astrophysics, Academia Sinica)