Program: GN-2024B-SV-114

Mass accretion and outflows are essential processes in the formation of stars and planets, as they remove the angular momentum of the infalling material (Hartigan et al. 1995). It is believed that the formation mechanism and evolution pattern are different depending on the mass of the star (e.g, low-, intermediate, and massive star). In Particular, massive star formation is not understood well (Zinnecker & Yorke 2007) but they are thought to form in multiple systems and in filamentary structures in molecular clouds. LkHα 233 is a Herbig Ae/Be star of intermediate mass, with around 4 solar masses. Usually, low-mass stars have good collimation and outflow, but this object is a rare case of such a phenomenon among medium-mass stars. It is also known as one of the special examples of driving parsec scale outflow with a distribution spanning over 3 parsecs. Optical spectroscopic observations have shown jets over 100 km/s near the central star Lkhα 233 with various emission lines (e.g., Corcoran and Ray 1998), while there is a lack of study in the infrared region. IFU observations conducted using OSIRIS/Keck detected 1.64 um [FeII] emission at a speed close to 200 km/s (Perrin et al. 2007). In the case of the 2.12 um H2, it was detected very weakly, possibly because it was at the edge of the filter's coverage, or because it was actually weak. With IGRINS-2, multiple lines can be observed simultaneously with wider spatial and wavelength coverage, and more detailed velocity structures can be revealed with high spectral resolution. Since past observations (e.g., Oh et al. 2018) have proven that IGRINS is a very powerful tool for studying the kinematics and physics of outflow, we will also test this possibility with IGRINS-2.