2013ApJ...762...11F

We present Herschel/HIFI observations of the three ground state transitions of H₂ O (556, 1669, and 1113 GHz) and H¹⁸₂O (547, 1655, and 1101 GHz)–as well as the first few excited transitions of H₂ O (987, 752, and 1661 GHz)–toward six high-mass star-forming regions, obtained as part of the PRISMAS (PRobing InterStellar Molecules with Absorption line Studies) Guaranteed Time Key Program. Water vapor associated with the translucent clouds in Galactic arms is detected in absorption along every line of sight in all the ground state transitions. The continuum sources all exhibit broad water features in emission in the excited and ground state transitions. Strong absorption features associated with the source are also observed at all frequencies except 752 GHz. We model the background continuum and line emission to infer the optical depth of each translucent cloud along the lines of sight. We derive the column density of H₂ O or H¹⁸₂O for the lower energy level of each transition observed. The total column density of water in translucent clouds is usually about a few 10¹³/cm2. We find that the abundance of water relative to hydrogen nuclei is 1x10^–8 in agreement with models for oxygen chemistry in which high cosmic ray ionization rates are assumed. Relative to molecular hydrogen, the abundance of water is remarkably constant through the Galactic plane with X(H₂O) =5x10^–8, which makes water a good traced of H₂ in translucent clouds. Observations of the excited transitions of H₂ O enable us to constrain the abundance of water in excited levels to be at most 15%, implying that the excitation temperature, T_ex, in the ground state transitions is below 10 K. Further analysis of the column densities derived from the two ortho ground state transitions indicates that T_ex≃ 5 K and that the density n(H₂) in the translucent clouds is below 10⁴/cm3. We derive the water ortho-to-para ratio for each absorption feature along the line of sight and find that most of the clouds show ratios consistent with the value of 3 expected in thermodynamic equilibrium in the high-temperature limit. However, two clouds with large column densities exhibit a ratio that is significantly below 3. This may argue that the history of water molecules includes a cold phase, either when the molecules were formed on cold grains in the well-shielded, low-temperature regions of the clouds, or when they later become at least partially thermalized with the cold gas (∼25 K) in those regions; evidently, they have not yet fully thermalized with the warmer (∼50 K) translucent portions of the clouds.