Observations of the Circumstellar Water {aastex} {amsbsy} {amsfonts} {amssymb} {bm} {mathrsfs} {pifont} {stmaryrd} {textcomp} {portland,xspace} {amsmath,amsxtra} [OT2,OT1]{fontenc} { {wncyr} {wncyss} {OT2} } {}{} {empty} {10}{9}{7}{6} {document} 1₁₀arrow 1₀₁ {document} and Ammonia {aastex} {amsbsy} {amsfonts} {amssymb} {bm} {mathrsfs} {pifont} {stmaryrd} {textcomp} {portland,xspace} {amsmath,amsxtra} [OT2,OT1]{fontenc} { {wncyr} {wncyss} {OT2} } {}{} {empty} {10}{9}{7}{6} {document} 1₀arrow 0₀ {document} Lines in IRC +10216 by theOdinSatellite

Submillimeter lines of H 2 O and NH 3 have been detected in the carbon star IRC +10216 (CW Leo) with the Odin submillimeter satellite. The detection of the J = 1 10 → 1 01 557 GHz line of ortho-H 2 O confirms the earlier detection in the same source with SWAS . The detection of the J K = 1 0 → 0 0 572 GHz line represents the first observation of the ground-state rotational transition of NH 3 in a stellar envelope. By fitting a molecular line transfer model to the observed lines, we derive an ortho-H 2 O abundance of 2.4 × 10 -6 , which is consistent with estimates from the SWAS observation. The derived ortho-NH 3 abundance of 1 × 10 -6 relative to H 2 is significantly higher than those derived from 24 GHz inversion transitions and is slightly higher than those from vibrational transitions in the infrared band. The high H 2 O and NH 3 abundances in the carbon-rich star IRC +10216 underscore shortcomings in the conventional gas-phase LTE and non-LTE chemical models.