Volume 566, June 2014
|Number of page(s)||4|
|Published online||20 June 2014|
Detection of chloronium and measurement of the 35Cl/37Cl isotopic ratio at z = 0.89 toward PKS 1830–211
Department of Earth and Space Sciences, Chalmers University of
Technology, Onsala Space Observatory, 43992
2 Institut de Radioastronomie Millimétrique, 300 rue de la piscine, 38406 St-Martin d’Hères, France
3 LRA/LERMA, CNRS UMR 8112, Observatoire de Paris & École Normale Supérieure, 75231 Paris, France
4 Max-Planck-Institut für Radioastonomie, Auf dem Hügel 69, 53121 Bonn, Germany
5 Astron. Dept., King Abdulaziz University, PO Box 80203, 21589 Jeddah, Saudi Arabia
6 Observatoire de Paris, LERMA, CNRS, 61 Av. de l’Observatoire, 75014 Paris, France
7 Institut d’Astrophysique Spatiale, Bât. 121, Université Paris-Sud, 91405 Orsay Cedex, France
8 Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA
9 Institute of Physics, Vietnam Academy of Science and Technology, 10 DaoTan, ThuLe, BaDinh, Hanoi, Vietnam
10 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany
Accepted: 28 April 2014
We report the first extragalactic detection of chloronium (H2Cl+) in the z = 0.89 absorber in front of the lensed blazar PKS 1830−211. The ion is detected through its 111-000 line along two independent lines of sight toward the North-East and South-West images of the blazar. The relative abundance of H2Cl+ is significantly higher (by a factor ~7) in the NE line of sight, which has a lower H2/H fraction, indicating that H2Cl+ preferably traces the diffuse gas component. From the ratio of the H235Cl+ and H237Cl+ absorptions toward the SW image, we measure a 35Cl/37Cl isotopic ratio of 3.1-0.2+0.3 at z = 0.89, similar to that observed in the Galaxy and the solar system.
Key words: quasars: absorption lines / galaxies: ISM / galaxies: abundances / ISM: molecules / radio lines: galaxies / quasars: individual: PKS 1830-211
© ESO, 2014
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