Volume 547, November 2012
|Number of page(s)||7|
|Section||Interstellar and circumstellar matter|
|Published online||24 October 2012|
1 Université de Toulouse, UPS-OMP, IRAP, Toulouse, France
2 CNRS, Institut pour la Recherche en Astrophysique et Planétologie, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
3 School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
4 Université Joseph Fourier and CNRS, Institut de Planétologie et d’Astrophysique, Grenoble, France
5 California Institute of Technology, Cahill Center for Astronomy and Astrophysics, Pasadena, CA 91125, USA
6 INAF Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
7 School of Earth and Environment, University of Leeds, Leeds LS2 9JT, UK
Received: 16 May 2012
Accepted: 28 September 2012
The H ion plays a key role in the chemistry of dense interstellar gas clouds where stars and planets are forming. The low temperatures and high extinctions of such clouds make direct observations of H impossible, but lead to large abundances of H2D+ and D2H+, which are very useful probes of the early stages of star and planet formation. The ground-state rotational ortho-D2H+ 11,1–00,0 transition at 1476.6 GHz in the prestellar core 16293E has been searched for with the Herschel HIFI instrument, within the CHESS (Chemical HErschel Surveys of Star forming regions) Key Program. The line has not been detected at the 21 mK km s-1 level (3σ integrated line intensity). We used the ortho-H2D+ 11,0–11,1 transition and para-D2H+ 11,0–10,1 transition detected in this source to determine an upper limit on the ortho-to-para D2H+ ratio as well as the para-D2H+/ortho-H2D+ ratio from a non-local thermodynamic equilibrium analysis. The comparison between our chemical modeling and the observations suggests that the CO depletion must be high (larger than 100), with a density between 5 × 105 and 106 cm-3. Also the upper limit on the ortho-D2H+ line is consistent with a low gas temperature (~11 K) with a ortho-to-para ratio of 6 to 9, i.e. 2 to 3 times higher than the value estimated from the chemical modeling, making it impossible to detect this high frequency transition with the present state of the art receivers.
Key words: astrochemistry / ISM: individual objects: 16293E / ISM: abundances / line: identification / radiative transfer
The chemical network is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/547/A33
© ESO, 2012
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