@Article{Benz_etal2010,
author="Benz, A. O.
and Bruderer, S.
and van Dishoeck, E. F.
and St{\"a}uber, P.
and Wampfler, S. F.
and Melchior, M.
and Dedes, C.
and Wyrowski, F.
and Doty, S. D.
and van der Tak, F.
and B{\"a}chtold, W.
and Csillaghy, A.
and Megej, A.
and Monstein, C.
and Soldati, M.
and Bachiller, R.
and Baudry, A.
and Benedettini, M.
and Bergin, E.
and Bjerkeli, P.
and Blake, G. A.
and Bontemps, S.
and Braine, J.
and Caselli, P.
and Cernicharo, J.
and Codella, C.
and Daniel, F.
and di Giorgio, A. M.
and Dieleman, P.
and Dominik, C.
and Encrenaz, P.
and Fich, M.
and Fuente, A.
and Giannini, T.
and Goicoechea, J. R.
and de Graauw, Th
and Helmich, F.
and Herczeg, G. J.
and Herpin, F.
and Hogerheijde, M. R.
and Jacq, T.
and Jellema, W.
and Johnstone, D.
and J{\o}rgensen, J. K.
and Kristensen, L. E.
and Larsson, B.
and Lis, D.
and Liseau, R.
and Marseille, M.
and McCoey, C.
and Melnick, G.
and Neufeld, D.
and Nisini, B.
and Olberg, M.
and Ossenkopf, V.
and Parise, B.
and Pearson, J. C.
and Plume, R.
and Risacher, C.
and Santiago-Garc{\'i}a, J.
and Saraceno, P.
and Schieder, R.
and Shipman, R.
and Stutzki, J.
and Tafalla, M.
and Tielens, A. G. G. M.
and van Kempen, T. A.
and Visser, R.
and Y{\i}ld{\i}z, U. A.",
title="Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system",
journal="Astron. Astrophys.",
year="2010",
volume="521",
pages="L35 (1 to 5)",
optkeywords="HEB mixer applications; HIFI; Herschel",
abstract="Context. Hydrides of the most abundant heavier elements are fundamental molecules in cosmic chemistry. Some of them trace gas irradiated by UV or X-rays.Aims. We explore the abundances of major hydrides in W3 IRS5, a prototypical region of high-mass star formation.Methods. W3 IRS5 was observed by HIFI on the Herschel Space Observatory with deep integration (2500 s) in 8 spectral regions.Results. The target lines including CH, NH, H3O+, and the new molecules SH+, H2O+, and OH+ are detected. The H2O+ and OH+ J = 1--0 lines are found mostly in absorption, but also appear to exhibit weak emission (P-Cyg-like). Emission requires high density, thus originates most likely near the protostar. This is corroborated by the absence of line shifts relative to the young stellar object (YSO). In addition, H2O+ and OH+ also contain strong absorption components at a velocity shifted relative to W3 IRS5, which are attributed to foreground clouds.Conclusions. The molecular column densities derived from observations correlate well with the predictions of a model that assumes the main emission region is in outflow walls, heated and irradiated by protostellar UV radiation.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=1082), last updated on Sat, 04 Jun 2016 09:37:08 -0500",
doi="10.1051/0004-6361/201015111",
opturl="https://doi.org/10.1051/0004-6361/201015111"
}