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