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We present new results of [Fe II] 1.644-micron spectroscopy toward the jetsfrom HL Tau and RW Aur carried out with the Subaru Telescope combined with theadaptive optics system. We observed the regions within 2" - 3" from the starswith the sub-arcsecond resolutions of 0."5 and 0."2 for HL Tau and RW Aur,respectively. In addition to the strong, high velocity emission extended alongeach jet, we detected a blueshifted low velocity emission feature seen as awing or shoulder of the high velocity emission at each stellar position.Detailed analysis shows that the position-velocity diagrams (PVDs) of HL Tauand RW Aur show a characteristic similar to those of the cold disk wind andX-wind models in that the [Fe II] line width is broad in the vicinity of thestellar position and is narrower at the extended jet. A closer comparisonsuggests, however, that the disk wind model tends to have too large line widthat the jet while the X-wind model has excess emission on the redshifted side atthe stellar position. The narrow velocity width with symmetric line profiles ofthe observed high velocity emission supports an X-wind type model where thelaunching region is localized in a small radial range, while the low velocityemission located away from the star favors the presence of a disk wind. The [FeII] emission from the HL Tau jet shows a gap of 0."8 between the redshifted jetand the star, indicating the presence of an optically thick disk of ~ 160 AU inradius. The [Fe II] emission from the RW Aur jet shows a marked drop from theredshifted peak at Y ~ -0."2 toward the star, suggesting that its disk radiusis smaller than 40 AU.Comment: Accepted in the ApJ (October 2006, v649n2), AAS LaTEX macros v 5.2,  Total 25 pages with 7 figure

Adaptive Optics Spectroscopy of the [Feii] Outflows from HL Tauri and RW Aurigae