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T.-S. Pyo, M. Hayashi (Subaru Telescope), N. Kobayashi (IfA, Japan), A. Tokunaga (IfA, UH), H. Terada (Subaru Telescope), M. Tsujimoto (Penn. State Univ.), S. Hayashi, T. Usuda, T. Yamashita, H. Takami, N. Takato (Subaru Telescope)
We present new velocity-resolved spectra of the [Fe II] 1.644 micron emission line toward the L1551 IRS 5 outflow taken by the Subaru Telescope. The spectra were taken toward the bright [Fe II] knots PHK1 and PHK2 with the slit positions perpendicular to the northern jet. (1) We found two subcomponents with their FWHMs of 0.83 and 2.84 arcseconds in the spatial profile of the low radial velocity component at VLSR ~-110 km s-1 at PHK1, which is located 1.2 arcsecond away from the L1551 IRS 5 VLA sources. The opening angle of the wide subcomponent is corresponding to ~100 degrees, which is consistent with the opening angle suggested by the broad velocity width of the narrow one. It prefer the interpretation that the both subcomponents of the LVC arise from the same outflow. The gas corresponding to the wide subcomponent fills the space between the optical jet and the shell of the CO molecular outflow, and may be sweeping up envelope material in the vicinity of the protostars. (2) We confirmed that the northern jet has two radial velocity components: VLSR ~-270 km s-1 and -140 km s-1 at PHK2, which is located ~4.2 arcsecond away from the VLA sources. The former velocity component is highly collimated at PHK 1 already because it has the same spatial width of 0.78 arcsecond at both of the two knots.
The author(s) of this abstract have provided an email address for comments about the abstract: pyo@subaru.naoj.org
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.