Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...199.7603p&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #76.03; Bulletin of the American Astronomical Society, Vol. 33, p.1419
Astronomy and Astrophysics
Astronomy
Scientific paper
We present a new [Fe II] λ 1.644 μm line image of the L1551 IRS 5 jets and its velocity resolved spectrum. The continuum subtracted [Fe II] emission line image shows clearly separated two jet like features. A strong and spatially wide [Fe II] emission feature was found elongated along the northern jet at its base. The echelle spectrum taken along the elongated feature shows two prominent velocity components and pedestal and wing emissions with the entire emission range blueshifted with respect to the systemic velocity. The high velocity component (HVC) at VLSR=-300 km s-1 consistently shows narrow line width of ~40 km s-1 along the northern jet. The HVC has a corresponding Hα emission. The low velocity component (LVC) at VLSR=-100 km s-1 is located spatially closer to the IRS 5 (VLA) than is the HVC. The LVC shows broad line widths of 130--160 km s-1 (FWHM) with flat topped line profiles in the region within 0.8'' from IRS 5 (VLA), while the line width decreases with increasing distance from it. The LVC has no corresponding Hα emission. We interpreted the velocity components as follows. The HVC is a narrow and well-collimated ionized stellar jet. The LVC is a widely opened and partially-ionized disk wind under collimation process. The pedestal and red wing features may represent the LVC gas entrained and accelerated by the HVC. The high velocity molecular and neutral atomic outflows in the literature may be entrained and accelerated by the LVC. Finally, we point out the possibility that the two apparently parallel jets seen more than 6'' away from IRS 5 (VLA) might be the brightened edges of the partially ionized wind.
Goto Mario
Hayashi Masahito
Itoh Yusuke
Kobayashi Nami
Pyo Tae-Soo
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