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

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dc.creatorPyo, Tae-Soo
dc.creatorHayashi, Masahiko
dc.creatorKobayashi, Naoto
dc.creatorTokunaga, Alan T.
dc.creatorTerada, Hiroshi
dc.creatorTakami, Hideki
dc.creatorTakato, Naruhisa
dc.creatorDavis, Christoper J.
dc.creatorTakami, Michihiro
dc.creatorHayashi, Saeko S.
dc.creatorGaessler, Wolfgang
dc.creatorOya, Shin
dc.creatorHayano, Yutaka
dc.creatorKamata, Yukiko
dc.creatorMinowa, Yosuke
dc.creatorIye, Masanori
dc.creatorUsuda, Tomonori
dc.creatorNishikawa, Takayuki
dc.creatorNedachi, Ko
dc.date2006-06-24
dc.date.accessioned2026-07-07T10:39:23Z
dc.date.available2026-07-07T10:39:23Z
dc.descriptionWe present new results of [Fe II] 1.644-micron spectroscopy toward the jets from HL Tau and RW Aur carried out with the Subaru Telescope combined with the adaptive optics system. We observed the regions within 2" - 3" from the stars with 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 along each jet, we detected a blueshifted low velocity emission feature seen as a wing or shoulder of the high velocity emission at each stellar position. Detailed analysis shows that the position-velocity diagrams (PVDs) of HL Tau and RW Aur show a characteristic similar to those of the cold disk wind and X-wind models in that the [Fe II] line width is broad in the vicinity of the stellar position and is narrower at the extended jet. A closer comparison suggests, however, that the disk wind model tends to have too large line width at the jet while the X-wind model has excess emission on the redshifted side at the stellar position. The narrow velocity width with symmetric line profiles of the observed high velocity emission supports an X-wind type model where the launching region is localized in a small radial range, while the low velocity emission located away from the star favors the presence of a disk wind. The [Fe II] emission from the HL Tau jet shows a gap of 0."8 between the redshifted jet and the star, indicating the presence of an optically thick disk of ~ 160 AU in radius. The [Fe II] emission from the RW Aur jet shows a marked drop from the redshifted peak at Y ~ -0."2 toward the star, suggesting that its disk radius is smaller than 40 AU.
dc.descriptionAccepted in the ApJ (October 2006, v649n2), AAS LaTEX macros v 5.2, Total 25 pages with 7 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0606605
dc.identifierhttp://arxiv.org/abs/astro-ph/0606605
dc.identifierAstrophys.J.649:836-844,2006
dc.identifierdoi:10.1086/506929
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/181010
dc.subjectAstrophysics
dc.titleAdaptive Optics Spectroscopy of the [Fe II] Outflows from HL Tauri and RW Aurigae
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