HeI 1.083 micron emission and absorption in DG Tau: line excitation in jet, hot wind, and accretion flow

Abstract

We present long-slit spectroscopy and spectro-astrometry of HeI 1.083 micron emission in the T Tauri star, DG Tau. We identify three components in the HeI feature: (1) a blueshifted emission component atv -200 km s^-1, (2) a bright emission component at zero-velocity with a FWZI of ~500 km s^-1, and (3) a blueshifted absorption feature at velocities between -250 and -500 km s^-1. The position and velocity of the blueshifted HeI emission coincide with a high-velocity component (HVC) of the [FeII] 1.257 micron emission, which arises from a jet within an arcsecond of the star. The presence of such a high excitation line (excitation energy ~ 20 eV) within the jet supports the scenario of shock heating. The bright HeI component does not show any spatial extension, and it is likely to arise from magnetospheric accretion columns. The blueshifted absorption shows greater velocities than that in H-alpha, suggesting that these absorption features arise from the accelerating wind close to the star.

10 pages including 2 figures, accepted for publication in the Astrophysical Journal Letters

References in corpus (3)

• HST/STIS spectroscopy of the optical outflow from DG Tau: structure and kinematics on sub-arcsecond scales
• The Structure and Emission of the Accretion Shock in T Tauri Stars II: the Ultraviolet Continuum Emission
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