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Interstellar OH+ , H2O+ and H3O+ along the sight-line to G10.6-0.4
Maryvonne Gerin 1, M. De Luca 1, John Black 2, Eric Herbst 3, 4, Javier R.Goicoechea 5, 6, Edith Falgarone 1, Benjamin Godard 1, John C. Pearson 7, Dariucz C. Lis 8, Thomas G. Phillips 8, Thomas A. Bell 8, Paule Sonnentrucker 9, Francois Boulanger 10, José Cernicharo 5, 6, Audrey Coutens 11, Emmanuel Dartois 10, Pierre Encrenaz 1, Thomas Giesen 12, Paul F. Goldsmith 7, Harshal Gupta 7, Cecile Gry 13, Patrick Hennebelle 1, Pierre Hily-Blant 14, Christine Joblin 11, Maja Kazmierczak 15, Robert Kolos 16, Jacek Krelowski 15, Jesus Martin-Pintado 17, Raquel Monje 8, Bhaswati Mookerjea 18, Michel Pérault 1, Carina Persson 2, René Plume 19, Paul B. Rimmer 3, 4, Morvan Salez 1, Mirisloaw Schmidt 20, David Teyssier 1, Charlotte Vastel 11, Shan Shan Yu 7, Alessandra Contursi 21, Karl Menten 22, Thomas Geballe 23, Stephan Schlemmer 12, Russ Shipman 24, Alexander G.G.M. Tielens 25, Sabine Philipp-May 22, 26, Alain Cros 27, Jonas Zmuidzinas 8, L. A Samoska 7, K. Klein 26, D.A. Neufeld 9, A. Lorenzani 28, Jürgen Stutzki 12
For the PRISMAS collaboration(s)
(2010-05-21)

We report the detection of absorption lines by the reactive ions OH+, H2O+ and H3O+ along the line of sight to the submillimeter continuum source G10.6$-$0.4 (W31C). We used the Herschel HIFI instrument in dual beam switch mode to observe the ground state rotational transitions of OH+ at 971~GHz, H2O+ at 1115 and 607~GHz, and H3O+ at 984 GHz. The resultant spectra show deep absorption over a broad velocity range that originates in the interstellar matter along the line of sight to G10.6$-$0.4 as well as in the molecular gas directly associated with that source. The OH+ spectrum reaches saturation over most velocities corresponding to the foreground gas, while the opacity of the H2O+ lines remains lower than 1 in the same velocity range, and the H3O+ line shows only weak absorption. For LSR velocities between 7 and 50 kms$^{-1}$ we estimate total column densities of $N$(OH+) $> 2.5 \times 10^{14}$ cm$^{-2}$, $N$(H2O+) $\sim 6 \times 10^{13}$ cm$^{-2}$ and $N$(H3O+) $\sim 4.0 \times 10^{13}$ cm$^{-2}$. These detections confirm the role of O$^+$ and OH$^+$ in initiating the oxygen chemistry in diffuse molecular gas and strengthen our understanding of the gas phase production of water. The high ratio of the OH+ by the H2O+ column density implies that these species predominantly trace low-density gas with a small fraction of hydrogen in molecular form.
1:  Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA)
CNRS : UMR8112 – INSU – Observatoire de Paris – Université Pierre et Marie Curie [UPMC] - Paris VI – Université de Cergy Pontoise – Ecole normale supérieure de Paris - ENS Paris
2:  Onsala space observatory (oso)
Chalmers University of Technology
3:  Department of Physics (OHIO STATE UNIVERSITY)
Ohio State University
4:  Departments of Astronomy and Chemistry
The Ohio State University
5:  centro de astrobiologia (CAB-INTA)
Instituto Nacional de Técnica Aeroespacial
6:  Centro de Investigaciones Biológicas (CSIC)
Consejo Superior de Investigaciones Cientificas
7:  Jet Propulsion Laboratory [NASA] (JPL)
NASA – California Institute of Technology
8:  CalTech-CSO (CSO)
California Institute of Technology
9:  Department of physics and astronomy
The John Hopkins University
10:  Institut d'astrophysique spatiale (IAS)
CNRS : UMR8617 – INSU – Université Paris XI - Paris Sud
11:  Centre d'étude spatiale des rayonnements (CESR)
CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III
12:  I physikalisches institut
University of Cologne
13:  Laboratoire d'Astrophysique de Marseille (LAM)
CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
14:  Laboratoire d'Astrophysique de Grenoble (LAOG)
CNRS : UMR5571 – OSUG – INSU – Université Joseph Fourier - Grenoble I
15:  Center for astronomy
Nicolaus Copernicus University
16:  Institute of physical chemistry
Polish Academy of Sciences
17:  Instituto de Estructura de la Materia (IEM)
Consejo Superior de Investigaciones Cientificas
18:  Tata Institute for fundamental research
tata institute for fundamental research
19:  Department of physics and astronomy
Univetsity of calgary – University of Calgary
20:  Nicolaus Copernicus Astronomical Center
Polish Academy of Sciences
21:  MPI fur Extraterrestrische Physik (MPE)
Max-Planck-Institut
22:  MPI f"ur Radioastronomie (MpIfR)
Max-Planck-Institut
23:  Gemini Telescope
Gemini Telescope
24:  Institute for Space Research Netherlands (SRON)
SRON Netherlands Institute for Space Research
25:  Sterrewacht Leiden
Leiden University
26:  Deutsches Zentrum fur Luft- und Raumfahrt
Deutsches Zentrum fur Luft and Raumfahrt
27:  Laboratoire Lasers, Plasmas et Procédés photoniques (LP3)
CNRS : UMR6182 – Université de la Méditerranée - Aix-Marseille II
28:  Osservatorio Astrofisico di Arcetri
INAF
Sciences of the Universe/Astrophysics/Galactic Astrophysics

Physics/Astrophysics/Galactic Astrophysics
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