Understanding the Nature of RY Tau's Dark Lane

Details Understanding the Nature of RY Tau's Dark Lane Understanding the Nature of RY Tau's Dark Lane

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6214m&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.14; Bulletin of the American Astronomical Society, Vol. 39, p.849

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RY Tauri is a K7Ve classical T Tauri star located 140 parsecs away in the Taurus-Auriga association. In addition to molecular cloud material to the north of the star, there is a conspicuous dark lane visible to the east of the star. We combine archival imagery from DSS, HST, the Tautenburg Observatory and the Gemini Observatory with coronagraphic narrow-band imagery from the Goddard Fabry-Perot interferometer and long-slit optical spectra taken with the Dual Imaging Spectrograph (both attached to the Apache Point Observatory in New Mexico) to test the hypothesis that RY Tau is actually a low-mass analog to VV Ser, a star known to have a geometrical shadow cast by the accretion disk onto the surrounding nebulosity. Alternatively, RY Tau's dark lane might be a protrusion of the molecular cloud. By combining the available data, we see a parsec-scale chain of knots and a bipolar microjet associated with the star. We derived radial velocities, proper motion, system inclination, and also traced the extent of the microjet and will use this information to characterize the outflow and ultimately answer the question of the dark lane's nature. We will also compare RY Tau to other stars in the association with data from the GFP and DIS.
This project has been made possible by a fund from the Illinois Space Grant, the Summer in Engineering and Computer Applications program at NASA/Goddard Space Flight Center. The Goddard Fabry-Perot is funded through NASA grant RTOP 51-188-01-22 to Goddard Space Flight Center. Observing time at the Apache Point Observatory 3.5m for GFP was provided through a grant of Director's Discretionary Time.

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