CO J=3-2 Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959

We observed CO J = 3-2 emission from "water-fountain" sources, which exhibit high-velocity collimated stellar jets traced by H2O maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10m telescope. We detected CO emission from two sources: IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that could be well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158 +/- 6 km s(-1) and an intensity peak at V-LSR= 50 +/- 2 km s(-1). The mass-loss rate of the star is estimated to be similar to 2.9 x 10(-5) M-circle dot yr(-1). Our morpho-kinematic models suggest that the CO emission is optically thin, and associated with a bipolar outflow rather than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a velocity width (FWHM) of 3.0 +/- 0.2 km s(-1) smaller than typically seen in AGB envelopes. The narrow velocity width of-the CO emission suggests that it originates from either an interstellar molecular cloud or a slowly-rotating circumstellar envelope that harbors the H2O maser source.