@article{oai:ir.kagoshima-u.ac.jp:00013283,
 author = {Imai, Hiroshi and 今井, 裕 and He, Jin-Hua and Nakashima, Jun-ichi and 中島, 淳一 and Ukita, Nobuharu and 浮田, 信治 and Deguchi, Shuji and 出口, 修至 and Koning, Nico},
 issue = {6},
 journal = {Publications of the Astronomical Society of Japan},
 month = {},
 note = {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 ~2.9×10^-5 M 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.},
 pages = {1365--1372},
 title = {CO J = 3–2 Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959},
 volume = {61},
 year = {2009}
}