2006/06/24 by Tae‐Soo Pyo, Tae-Soo Pyo, Masahiko Hayashi +20 · 3 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Emission spectrum #Galaxy #Geometry #Jet (fluid) #Line (geometry) #Physics #Position angle #RADIUS #Redshift #Spectral line #Spectroscopy #Stars #Stellar, planetary, and galactic studies #Subaru Telescope #T Tauri star #astro-ph
paper · pdf · doi:10.1086/506929
published as Astrophys.J.649:836-844,2006 · Accepted in the ApJ (October 2006, v649n2), AAS LaTEX macros v 5.2, Total 25 pages with 7 figures
arxiv created 2006/06/24 · openalex publication_date 2006/09/27 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present new results of [Fe II] λ1.644 μm 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 subarcsecond resolutions of 0 5 and 0 2 for HL Tau and RW Aur, respectively. In addition to the strong high-velocity component (HVC) extended along each jet, we detected a blueshifted low-velocity component (LVC) seen as a wing or shoulder of the HVC at each stellar position. The position velocity diagrams of the two objects show a characteristic similar to those of the cold disk wind and X -wind models in that the [Fe II] line width is broad close to the stellar position and narrower at the extended jet. A closer comparison suggests, however, that the disk wind model tends to have too large a line width at the HVC, while the X -wind model has excess redshifted emission at the stellar position. The narrow velocity width with symmetric line profiles of the observed HVC supports an X -wind-type model, while the LVC, located away from the star, favors the presence of a disk wind. The [Fe II] emission shows a gap of 0 8 for HL Tau and a marked drop of Y ~ -0 2 for RW Aur between the redshifted jet and the star, which indicate optically thick disks of ~160 and <40 AU in radius, respectively. Part of the Br12 emission of HL Tau originates from the jet itself because its normalized line profile shows a signigicantly large deviation from the normalized continuum in spatial profile.