@Article{Bruderer_etal2010,
author="Bruderer, S.
and Benz, A. O.
and van Dishoeck, E. F.
and Melchior, M.
and Doty, S. D.
and van der Tak, F.
and St{\"a}uber, P.
and Wampfler, S. F.
and Dedes, C.
and Y{\i}ld{\i}z, U. A.
and Pagani, L.
and Giannini, T.
and de Graauw, Th
and Whyborn, N.
and Teyssier, D.
and Jellema, W.
and Shipman, R.
and Schieder, R.
and Honingh, N.
and Caux, E.
and B{\"a}chtold, W.
and Csillaghy, A.
and Monstein, C.
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 Dominik, C.
and Encrenaz, P.
and Fich, M.
and Fuente, A.
and Goicoechea, J. R.
and Helmich, F.
and Herczeg, G. J.
and Herpin, F.
and Hogerheijde, M. R.
and Jacq, T.
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 Parise, B.
and Pearson, J. C.
and Plume, R.
and Risacher, C.
and Santiago-Garc{\'i}a, J.
and Saraceno, P.
and Shipman, R.
and Tafalla, M.
and van Kempen, T. A.
and Visser, R.
and Wyrowski, F.",
title="Herschel/HIFI detections of hydrides towards AFGL 2591. Envelope emission versus tenuous cloud absorption",
journal="Astron. Astrophys.",
year="2010",
volume="521",
pages="L44 (1 to 7)",
optkeywords="HEB mixer applications; HIFI; Herschel",
abstract="The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(JF,P = 3/22,- - 1/21,+ ) and CH+(J = 1--0, J = 2--1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=1083), last updated on Sat, 04 Jun 2016 10:20:38 -0500",
doi="10.1051/0004-6361/201015098",
opturl="https://doi.org/10.1051/0004-6361/201015098"
}