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The Structure of Young Stellar Jets and Winds Revealed by High Resolution [Fe II] λ1.644μm Line Observations |
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| Authors: | Tae-Soo Pyo Masahiko Hayashi Naoto Kobayashi Alan T Tokunaga Hiroshi Terada Miwa Goto Takuya Yamashita Yoichi Itoh Hideki Takami Naruhisa Takato Yutaka Hayano Wolfgang Gaessler Yukiko Kamata Yosuke Minowa Masanori Iye |
| Institution: | 1. National Astronomical Observatory of Japan, 650 North A`ohōokū Place, Subaru Telescope, Hilo, HI, 96720, USA 2. Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, 96822, USA 3. National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan 4. Graduate School of Science and Technology, Kobe University, Kobe, 657-8501, Japan 5. Department of Astronomy, School of Science, University of Tokyo, Tokyo, 113-0033, Japan |
| Abstract: | We present high angular resolution spectra taken along the jets from L1551 IRS 5 and DG Tau obtained with the Subaru Telescope. The position-velocity diagrams of the Fe II] λ 1.644 μmemission line revealed remarkably similar characteristics for the two sources, showing two distinct velocity components separated from each other in both velocity and space with the entire emission range blueshifted with respect to the stellar velocity. The high velocity component (HVC) has a velocity of –200 ––300 km s-1 with a narrow line width, while the low velocity component (LVC) is around –100 km s-1 exhibitinig a broad line width. The HVC is located farther away from the origin and is more extended than the LVC. Our results suggest that the HVC is a well-collimated jet originating from the region close to the star, while the LVC is a widely-opened wind accelerated in the region near the inner edge of the accretion disk. |
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