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.

We present observational results from optical long-slit spectroscopy of parsec-scale jets of DG Tau. From HH 158 and HH 702, the optical emission lines of H, [O i] 6300, 6363, [N ii] 6548, 6584, and [S ii] 6716, 6731 are obtained. The kinematics and physical properties (i.e., electron density, electron temperature, ionization fraction, and mass-loss rate) are investigated along the blueshifted jet up to 650′′ distance from the source. For HH 158, the radial velocity ranges from -50 to -250 km s-1. The proper motion of the knots is 0:′′196 - 0:′′272 yr-1. The electron density is 104 cm-3 close to the star, and decreases to 102 cm-3 at 14′′ away from the star. Ionization fraction indicates that the gas is almost neutral in the vicinity of the source. It increases up to over 0.4 along the distance. HH 702 is located at 650′′ from the source. It shows  -80 km s-1 in the radial velocity. Its line ratios are similar to those at knot C of HH 158. The mass-loss rate is estimated to be about  10-7 M⊙ yr-1, which is similar to values obtained from previous studies.

We present medium resolution (R = 5000 - 6000) spectra in the near-infrared band, 1.4 - 1.8 μm, for template stars in G, K, and M types observed by the echelle spectrometer, IRCS, at the SUBARU 8.2 m telescope. The identification of lines is based on the spectra of Arcturus (K2 III) in the literature. We measured the equivalent of widths and compared our results to those of Meyer et al. (1998). We conclude that our spectral resolution (R = 6000) data can investigate more accurately the properties of lines in stellar spectra. The library of the template stellar spectra in ASCII format are available for download on the World Wide Web.