@Article{Chavarria_etal2010,
author="Chavarr{\textquoteright}{\i}a, L.
and Herpin, F.
and Jacq, T.
and Braine, J.
and Bontemps, S.
and Baudry, A.
and Marseille, M.
and van der Tak, F.
and Pietropaoli, B.
and Wyrowski, F.
and Shipman, R.
and Frieswijk, W.
and van Dishoeck, E. F.
and Cernicharo, J.
and Bachiller, R.
and Benedettini, M.
and Benz, A. O.
and Bergin, E.
and Bjerkeli, P.
and Blake, G. A.
and Bruderer, S.
and Caselli, P.
and Codella, C.
and Daniel, F.
and di Giorgio, A. M.
and Dominik, C.
and Doty, S. D.
and Encrenaz, P.
and Fich, M.
and Fuente, A.
and Giannini, T.
and Goicoechea, J. R.
and de Graauw, T.
and Hartogh, P.
and Helmich, F.
and Herczeg, G. J.
and Hogerheijde, M. R.
and Johnstone, D.
and J{\o}rgensen, J. K.
and Kristensen, L. E.
and Larsson, B.
and Lis, D.
and Liseau, R.
and McCoey, C.
and Melnick, G.
and Nisini, B.
and Olberg, M.
and Parise, B.
and Pearson, J. C.
and Plume, R.
and Risacher, C.
and Santiago-Garc{\textquoteright}{\i}a, J.
and Saraceno, P.
and Stutzki, J.
and Szczerba, R.
and Tafalla, M.
and Tielens, A.
and van Kempen, T. A.
and Visser, R.
and Wampfler, S. F.
and Willem, J.
and Y{\i}ld{\i}z, U. A.",
title="Water in massive star-forming regions: HIFI observations of W3 IRS5",
journal="Astron. Astrophys.",
year="2010",
volume="521",
pages="L37 (1 to 5)",
optkeywords="HEB mixer applications; HIFI; Herschel; stars: formation; stars: massive; ISM: molecules; ISM: abundances; dust; extinction; radio lines: ISM",
abstract="We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-H217O 110-101, p-H218O 111-000, p-H2O 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 {\textasciitilde} 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 {\^a}{\texttenthousand}<b3> 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-H217O 110-101 and p-H218O 111-000 spectra in our models. We estimate water abundances of 10-8 to 10-9 in the outer parts of the envelope (T {\^a}{\texttenthousand}<b2> 100 K). The possibility of two protostellar objects contributing to the emission is discussed.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=1086), last updated on Sat, 04 Jun 2016 17:25:36 -0500",
doi="10.1051/0004-6361/201015113",
opturl="https://doi.org/10.1051/0004-6361/201015113"
}