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Issue A&A
Volume 454, Number 2, August I 2006
APEX Special Booklet
Page(s) L99 - L102
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20065289



A&A 454, L99-L102 (2006)
DOI: 10.1051/0004-6361:20065289

Letter

APEX mapping of H $\mathsf{_3}$O $\mathsf{^+}$ in the Sgr B2 region

F. F. S. van der Tak1, 2, A. Belloche1, P. Schilke1, R. Güsten1, S. Philipp1, C. Comito1, P. Bergman3 and L.-Å. Nyman3

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2  National Institute for Space Research (SRON), Postbus 800, 9700 AV Groningen, The Netherlands
    e-mail: vdtak@sron.rug.nl
3  European Southern Observatory, Casilla 19001, Santiago, Chile

(Received 27 March 2006 / Accepted 22 May 2006)

Abstract
Context.The cosmic-ray ionization rate $\zeta_{\rm CR}$ of dense molecular clouds is a key parameter for their dynamics and chemistry.
Aims.Variations of $\zeta_{\rm CR}$ are well established, but it is unclear if these are related to source column density or to Galactic location.
Methods.Using the APEX telescope, we have mapped the 364 GHz line of H3O+ in the Sgr B2 region and observed the 307 GHz line at selected positions. With the IRAM 30-m telescope we have observed the H218O 203 GHz line at the same positions.
Results.Strong H3O+ emission is detected over a ~3 $\times$ 2 pc region, indicating an H3O+ column density of 1015-1016 cm-2 in an 18'' beam. The H3O+ abundance of ~ 3 $\times$ 10-9 and H3O+/H2O ratio of ~1/50 in the Sgr B2 envelope are consistent with models with $\zeta_{\rm CR}$ ~ 4 $\times$ 10-16  s-1, 3$\times$ lower than derived from H3+ observations toward Sgr A, but 10$\times$ that of local dense clouds.
Conclusions.The ionization rates of interstellar clouds thus seem to be to first order determined by the ambient cosmic-ray flux, while propagation effects cause a factor of ~3 decrease from diffuse to dense clouds.


Key words: ISM: clouds -- ISM: molecules -- ISM: cosmic rays -- molecular processes -- astrochemistry



© ESO 2006


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