  We report the results of a Submillimeter Array (SMA) interferometric
observation of 21-micron source IRAS 07134+1005 in the CO J=3-2 line. In order
to determine the morpho-kinematic properties of the molecular envelope of the
object, we constructed a model using the Shape software to model the observed
CO map. We find that the molecular gas component of the envelopes can be
interpreted as a geometrically thick expanding torus with an expanding velocity
of 8 km/s. The inner and outer radii of the torus determined by fitting Shape
models are 1.2" and 3.0", respectively. The inner radius is consistent with the
previous values determined by radiative transfer modeling of the spectral
energy distribution and mid-infrared imaging of the dust component. The radii
and expansion velocity of the torus suggest that the central star has left the
asymptotic giant branch about 1140-1710 years ago, and that the duration of the
equatorial enhanced mass loss is about 2560-3130 years. From the absence of an
observed jet, we suggest that the formation of a bipolar outflow may lack
behind in time from the creation of the equatorial torus.
