E.F. van Dishoeck
T.A. van Kempen
A.M. Di Giorgio
T. de Graauw
F.F.S. van der Tak
- Herschel observations of the hydroxyl radical (OH) in young stellar objects
- Astronomy & Astrophysics
- Pages (from-to)
- Number of pages
- Document type
- Faculty of Science (FNWI)
- Anton Pannekoek Institute for Astronomy (API)
Aims. "Water In Star-forming regions with Herschel" (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 greater than or similar to 250 K) chemistry connects OH and H2O through the OH + H-2 double left right arrow 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) double right arrow 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 [OI] lines.
Results. The OH transitions at 79, 84, 119, and 163 mu m and [OI] 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 greater than or similar to 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 [OI] 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.
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