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UNVEILING COMPLEX OUTFLOW STRUCTURE OF UY Aur

  • PYO, TAE-SOO (Subaru Telescope, National Astronomical Observatory of Japan) ;
  • HAYASHI, MASAHIKO (School of Mathematical and Physical Science, The Graduate University for Advanced Studies (SOKENDAI)) ;
  • BECK, TRACY (Space Telescope Science Institute) ;
  • DAVIS, CHRISTOPHER J. (Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park) ;
  • TAKAMI, MICHIHIRO (Institute of Astronomy and Astrophysics)
  • Received : 2014.11.30
  • Accepted : 2015.06.30
  • Published : 2015.09.30

Abstract

We present [$Fe\;{\small{II}}$] ${\lambda}1.257{\mu}m$ spectra toward the interacting binary UY Aur with 0".14 angular resolution, obtained with the Near infrared Integral Field Spectrograph (NIFS) combined with the adaptive optics system Altair of the GEMINI observatory. In the [$Fe\;{\small{II}}$] 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 [$Fe\;{\small{II}}$] emission features are similar for UY Aur A and B: ${\sim}-100km\;s^{-1}$ and ${\sim}+130km\;s^{-1}$ for the blueshifted and redshifted components, respectively. Considering the morphologies of the [$Fe\;{\small{II}}$] emissions and bipolar outflow context, we concluded that UY Aur A drives fast and widely opening outflows with an opening angle of ${\sim}90^{\circ}$ while UY Aur B has micro collimated jets.

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