CO Study of the GM Aurigae Keplerian Disk

A.Dutrey , S.Guilloteau , L.Prato , M.Simon , G.Duvert , K.Schuster , and F.Ménard
IRAM, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France
Dept. of Physics and Astronomy, State Univ. of New York, Stony Brook, NY 11794-3800, U.S.A.
Laboratoire d'Astrophysique de Grenoble, B.P. 53, F-38041 Grenoble Cedex 9, France
Abstract: We report new high resolution (0.6 - 1.7'') images of GM Aur in the CO (2-1) line and the 1.3 and 2.7 mm continuum (see Fig. 6). The dust disk, located at the center of the CO disk, is resolved by the 0.6'' beam of the interferometer. We derive a minimum radius of AU, and a total mass (dust+gas) of about . Our CO observations also resolve the Keplerian rotation of the gas disk. Since the CO emission is optically thick, the CO data does not allow a disk mass measurement but we can estimate the dynamical mass of the system, i.e. the stellar mass, although a solution with a more inclined disk and lower stellar mass ( ) is also possible.

 

Figure: Channel maps of the CO data in GM Aur (top) and the best model processed in identical way (bottom). Contour steps are 0.25 mJy/beam (or 1.9 K). Velocities are indicated in the upper left corner of each panel .

Astronomy & Astrophysics Letter, in press. Preprints: dutrey@iram.fr

 

Figure 7: Channel maps of the SiO J = 2 1 line emission in SVS13B/ HH7-11 averaged over velocity intervals from -17 to 6.5 km s (left panel), from 6.5 to 10.5 km s (center), and from 10.5 to 17 km s (right). First contour and step are 10 mJy beam . The positions of the HH7-11 objects are marked by black squares. Some spectra obtained at particular map positions are shown in the upper panels. The direction of the SiO jet driven by SVS13B is indicated by the thick lines in the high velocity maps.