We present Herschel/HIFI observations of fourteen water lines in W43-MM1, a massive protostellar object in the luminous star cluster-forming region W43. We analyze the gas dynamics from the line profiles using Herschel-HIFI observations (WISH-KP) of
fourteen far-IR water lines (H2O, H217O, H218O), CS(11-10), and C18O(9-8) lines, and using our modeling of the continuum spectral energy distribution. As for lower mass protostellar objects, the molecular line profiles are a mix of emission and absorption, and can be decomposed into medium, and broad velocity components. The broad component is the outflow associated with protostars of all masses. Our modeling shows that the remainder of the water profiles can be well fitted by an infalling and passively heated envelope, with highly supersonic turbulence varying from 2.2 km/s in the inner region to 3.5 km/s in the outer envelope. Also, W43-MM1 has a high accretion rate, between 4.0 x 10^{-4} and 4.0 x 10^{-2} msun /yr, derived from the fast (0.4-2.9 km/s) infall observed. We estimate a lower mass limit of gaseous water of 0.11 msun and total water luminosity of 1.5 lsun (in the 14 lines presented here). The central hot core is detected with a water abundance of 1.4 x 10^{-4} while the water abundance for the outer envelope is 8 x10^{-8}. The latter value is higher than in other sources, most likely related to the high turbulence and the micro-shocks created by its dissipation. Examining water lines of various energies, we find that the turbulent velocity increases with the distance to the center. While not in clear disagreement with the competitive accretion scenario, this behavior is predicted by the turbulent core model. Moreover, the estimated accretion rate is high enough to overcome the expected radiation pressure.
We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-H17O 110-101, p-H18O 111-000, p-H2O 22 202-111, p-H2O 111-000, o-H2O 221-212, and o-H2O 212-101 lines, covering a frequency range from 552 up to
1669 GHz, have been detected at high spectral resolution with HIFI. The water lines in W3 IRS5 show well-defined high-velocity wings that indicate a clear contribution by outflows. Moreover, the systematically blue-shifted absorption in the H2O lines suggests expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 111-000 and o-H2O 212-101 lines show absorption from the cold material (T ~ 10 K) in which the high-mass protostellar envelope is embedded. One-dimensional radiative transfer models are used to estimate water abundances and to further study the kinematics of the region. We show that the emission in the rare isotopologues comes directly from the inner parts of the envelope (T > 100 K) where water ices in the dust mantles evaporate and the gas-phase abundance increases. The resulting jump in the water abundance (with a constant inner abundance of 10^{-4}) is needed to reproduce the o-H17O 110-101 and p-H18O 111-000 spectra in our models. We estimate water abundances of 10^{-8} to 10^{-9} in the outer parts of the envelope (T < 100 K). The possibility of two protostellar objects contributing to the emission is discussed.
