Astron. Astrophys. 338, L63-L66 (1998)

Letter to the Editor

CO study of the GM Aurigae Keplerian disk

A. Dutrey ¹, S. Guilloteau ¹, L. Prato ², M. Simon ², G. Duvert ³, K. Schuster ¹ and F. Ménard <sup>3

1</sup> Institut de Radio Astronomie Millimétrique, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France
² Department of Physics and Astronomy, State University of New York, Stony Brook, NY 11794-3800, USA
³ Laboratoire d'Astrophysique de Grenoble, B.P. 53, F-38041 Grenoble Cedex 9, France

Received 15 June 1998 / Accepted 25 August 1998

Abstract

We report new high resolution () images of GM Aur in the   line and the 1.3 and 2.7 mm continuum. The dust disk, located at the center of the CO disk, is resolved by the 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.

Key words: stars: T Tauri circumstellar matter pre-main sequence radio-lines: stars

Send offprint requests to: A.Dutrey

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Contents

• 1. Introduction
• 2. Observations
• 3. Results
• 4. Disk Properties
• 5. Summary
• Acknowledgements
• References

© European Southern Observatory (ESO) 1998

Online publication: September 14, 1998
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