@Article{Wampfler_etal2010,
author="Wampfler, S. F.
and Herczeg, G. J.
and Bruderer, S.
and Benz, A. O.
and van Dishoeck, E. F.
and Kristensen, L. E.
and Visser, R.
and Doty, S. D.
and Melchior, M.
and van Kempen, T. A.
and Y{\i}ld{\i}z, U. A.
and Dedes, C.
and Goicoechea, J. R.
and Baudry, A.
and Melnick, G.
and Bachiller, R.
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 Giannini, T.
and de Graauw, Th
and Helmich, F.
and Herpin, F.
and Hogerheijde, M. R.
and Jacq, T.
and Johnstone, D.
and J{\o}rgensen, J. K.
and Larsson, B.
and Lis, D.
and Liseau, R.
and Marseille, M.
and Mc Coey, C.
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 der Tak, F. F. S.
and Wyrowski, F.
and Roelfsema, P.
and Jellema, W.
and Dieleman, P.
and Caux, E.
and Stutzki, J.",
title="Herschel observations of the hydroxyl radical (OH) in young stellar objects",
journal="Astron. Astrophys.",
year="2010",
volume="521",
pages="L36",
optkeywords="HEB mixer applications; HIFI; Herschel; astrochemistry / stars: formation / ISM: molecules / ISM: jets and outflows / ISM: individual objects: HH 46",
abstract="Aims. {\^a}{\texteuro}{\oe}Water In Star-forming regions with Herschel{\^a}{\texteuro} (WISH) is a Herschel key program investigating the water chemistry in young stellar objects (YSOs) during protostellar evolution. Hydroxyl (OH) is one of the reactants in the chemical network most closely linked to the formation and destruction of H2O. High-temperature (T  250 K) chemistry connects OH and H2O through the OH + H2  H2O + H reactions. Formation of H2O from OH is efficient in the high-temperature regime found in shocks and the innermost part of protostellar envelopes. Moreover, in the presence of UV photons, OH can be produced from the photo-dissociation of H2O through H2O + $\gamma$UV  OH + H.Methods. High-resolution spectroscopy of the 163.12 $\mu$m triplet of OH towards HH 46 and NGC 1333 IRAS 2A was carried out with the Heterodyne Instrument for the Far Infrared (HIFI) on board the Herschel Space Observatory. The low- and intermediate-mass protostars HH 46, TMR 1, IRAS 15398-3359, DK Cha, NGC 7129 FIRS 2, and NGC 1333 IRAS 2A were observed with the Photodetector Array Camera and Spectrometer (PACS) on Herschel in four transitions of OH and two [O i] lines.Results. The OH transitions at 79, 84, 119, and 163 $\mu$m and [O i] emission at 63 and 145$\mu$m were detected with PACS towards the class I low-mass YSOs as well as the intermediate-mass and class I Herbig Ae sources. No OH emission was detected from the class 0 YSO NGC 1333 IRAS 2A, though the 119 $\mu$m was detected in absorption. With HIFI, the 163.12 $\mu$m was not detected from HH 46 and only tentatively detected from NGC 1333 IRAS 2A. The combination of the PACS and HIFI results for HH 46 constrains the line width (FWHM  11 km s-1) and indicates that the OH emission likely originates from shocked gas. This scenario is supported by trends of the OH flux increasing with the [O i] flux and the bolometric luminosity, as found in our sample. Similar OH line ratios for most sources suggest that OH has comparable excitation temperatures despite the different physical properties of the sources.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=1103), last updated on Fri, 17 Jun 2016 18:09:50 -0500",
doi="10.1051/0004-6361/201015112",
opturl="https://doi.org/10.1051/0004-6361/201015112"
}