Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 308609.0, MPI für Astronomie / Publikationen_mpia
Adaptive optics spectroscopy of the [Fe II] outflows from HL Tauri and RW Aurigae
Authors:Pyo, T.-S.; Hayashi, M.; Kobayashi, N.; Tokunaga, A. T.; Terada, H.; Takami, H.; Takato, N.; Davis, C. J.; Takami, M.; Hayashi, S. S.; Gaessler, W.; Oya, S.; Hayano, Y.; Kamata, Y.; Minowa, Y.; Iye, M.; Usuda, T.; Nishikawa, T.; Nedachi, K.
Date of Publication (YYYY-MM-DD):2006
Journal Abbrev.:The Astrophysical Journal
Volume:649
Start Page:836
End Page:844
Audience:Not Specified
Abstract / Description:We present new results of [Fe II] lambda1.644 mum 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. Based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.
Free Keywords:ISM: Herbig-Haro Objects; ISM: individual (HL Tauri: HH 150); ISM: individual (RW Aurigae: HH 229); ISM: Jets and Outflows; Stars: Formation; Stars: Pre-Main-Sequence; Techniques: High Anular Resolution
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi...
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.