The orbiting gas disk in the Red Rectangle

Abstract

We present accurate maps of the CO J = 2-1 and 1-0 lines made with the Plateau de Bure interferometer of the gas disk around the central star(s) of the Red Rectangle, a well known protoplanetary nebula. We confirm that the molecular gas in this source forms a disk perpendicular to the conspicuous axis of symmetry of the optical nebula and that this disk is in rotation. We present detailed modeling of the CO emission and extensive discussion of the accuracy of the values fitted for the different parameters. Theouterradius of the disk is ∼2.7 × 1016 (D(pc)/710) cm, as a function of the assumed distance D, which is thought to vary between 380 and 710 pc. The rotation is found to be Keplerian, at least in the inner disk. From this velocity field, we derive a central mass between 0.9 M⊙, for a distance of 380 pc, and 1.7 M⊙, for 710 pc. Previous studies of the nature of the stellar component favor the highest values. In the outer disk, we deduce the presence of a slow expansion velocity (∼0.8 km s -1), superimposed on rotation. We find gas temperatures decreasing from ∼400 to 30 K across the disk and densities ≳3 × 10 4 cm-3. © ESO 2005.