TY  - JOUR
AU  - Benz, A. O.
AU  - Bruderer, S.
AU  - van Dishoeck, E. F.
AU  - Stäuber, P.
AU  - Wampfler, S. F.
AU  - Melchior, M.
AU  - Dedes, C.
AU  - Wyrowski, F.
AU  - Doty, S. D.
AU  - van der Tak, F.
AU  - Bächtold, W.
AU  - Csillaghy, A.
AU  - Megej, A.
AU  - Monstein, C.
AU  - Soldati, M.
AU  - Bachiller, R.
AU  - Baudry, A.
AU  - Benedettini, M.
AU  - Bergin, E.
AU  - Bjerkeli, P.
AU  - Blake, G. A.
AU  - Bontemps, S.
AU  - Braine, J.
AU  - Caselli, P.
AU  - Cernicharo, J.
AU  - Codella, C.
AU  - Daniel, F.
AU  - di Giorgio, A. M.
AU  - Dieleman, P.
AU  - Dominik, C.
AU  - Encrenaz, P.
AU  - Fich, M.
AU  - Fuente, A.
AU  - Giannini, T.
AU  - Goicoechea, J. R.
AU  - de Graauw, Th
AU  - Helmich, F.
AU  - Herczeg, G. J.
AU  - Herpin, F.
AU  - Hogerheijde, M. R.
AU  - Jacq, T.
AU  - Jellema, W.
AU  - Johnstone, D.
AU  - Jørgensen, J. K.
AU  - Kristensen, L. E.
AU  - Larsson, B.
AU  - Lis, D.
AU  - Liseau, R.
AU  - Marseille, M.
AU  - McCoey, C.
AU  - Melnick, G.
AU  - Neufeld, D.
AU  - Nisini, B.
AU  - Olberg, M.
AU  - Ossenkopf, V.
AU  - Parise, B.
AU  - Pearson, J. C.
AU  - Plume, R.
AU  - Risacher, C.
AU  - Santiago-García, J.
AU  - Saraceno, P.
AU  - Schieder, R.
AU  - Shipman, R.
AU  - Stutzki, J.
AU  - Tafalla, M.
AU  - Tielens, A. G. G. M.
AU  - van Kempen, T. A.
AU  - Visser, R.
AU  - Yıldız, U. A.
PY  - 2010
DA  - 2010//
TI  - Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system
JO  - Astron. Astrophys.
SP  - L35 (1 to 5)
VL  - 521
KW  - HEB mixer applications
KW  - HIFI
KW  - Herschel
AB  - 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.
UR  - https://doi.org/10.1051/0004-6361/201015111
DO  - 10.1051/0004-6361/201015111
N1  - exported from refbase (https://db.rplab.ru/refbase/show.php?record=1082), last updated on Sat, 04 Jun 2016 09:37:08 -0500
ID  - Benz_etal2010
ER  -