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J. R. Goicoechea et al.: The ionization fraction gradient across the Horsehead edge: an archetype for molecular clouds 783tel-00726959, version 1 - 31 Aug 2012lower than 4 × 10 −9 (strong metal depletion). Conversely, assuminga standard metal abundance of [M] = 10 −9 , our observationscan only be reproduced with ζ = (5±3)×10 −17 s −1 .4. The inclusion of PAHs modifies the ionization fraction gradientand decreases the metal depletion required to reproducethe observations if [PAH] > 10 −8 (i.e., if not allPAHs coagulate/accrete onto bigger grains). In such a case,PAH − acquire large abundances also in the shielded gas.Recombination of atomic ions on PAH − is much more efficientthan on electrons and thus metal ions and molecularions are neutralized at similar rates. For [PAH] = 10 −7 ,themetal abundance consistent with observations increases to[M] = (3 ± 1) × 10 −6 (still below the heavy metals abundancein the diffuse ISM).Acknowledgements. We thank the IRAM staff for their support during observationsand D. Talbi and B. Godard for useful advice regarding the HCO + dissociativerecombination rate. Inelastic collisional rates of HCO + with electrons werekindly provided by A. Faure and J. Tennyson. We also thank M. Walmsely forseveral interesting comments. We acknowledge the use of OSU (http://www.physics.ohio-state.edu/~eric/research.html) andUDFA (http://www.udfa.net/) chemical reaction databases. We finally acknowledge financialsupport from CNRS/INSU research programme PCMI. JRG is supported bya Ramón y Cajal research contract from the Spanish MICINN and co-financedby the European Social Fund.ReferencesAbergel, A., Teyssier, D., Bernard, J. P., et al. 2003, A&A, 410, 577Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1985, ApJ, 290, L25Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1989, ApJS, 71, 733Anders, E., & Grevesse, N. 1989, Geochim. Cosmochim. Acta, 53, 197Bakes, E. L. O., & Tielens, A. G. G. 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A&A 494, 977–985 (2009)DOI: 10.1051/0004-6361:200810933c○ ESO 2009Astronomy&AstrophysicsHCO mapping of the Horsehead: tracing the illuminateddense molecular cloud surfaces ⋆,⋆⋆M. Gerin 1 , J. R. Goicoechea 1,⋆⋆⋆ ,J.Pety 2,1 , and P. Hily-Blant 31 LERMA–LRA, UMR 8112, CNRS, Observatoire de Paris and École Normale Supérieure, 24 Rue Lhomond, 75231 Paris, Francee-mail: maryvonne.gerin@lra.ens.fr; jrgoicoechea@fis.ucm.es2 IRAM, 300 rue de la Piscine, 38406 Grenoble cedex, Francee-mail: pety@iram.fr3 Laboratoire d’Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 09, Francee-mail: pierre.hilyblant@obs.ujf-grenoble.frReceived 8 September 2008 / Accepted 14 November 2008ABSTRACTtel-00726959, version 1 - 31 Aug 2012Context. Far-UV photons (FUV) strongly affect the physical and chemical state of molecular gas in the vicinity of young massivestars.Aims. Finding molecular tracers of the presence of FUV radiation fields in the millimeter wavelength domain is desirable becauseIR diagnostics (for instance PAHs) are not easily accessible along high extinction line-of-sights. Furthermore, gas phase diagnosticsprovide information on the velocity fields.Methods. We have obtained maps of the HCO and H 13 CO + ground state lines towards the Horsehead edge at 5 ′′ angular resolutionwith a combination of Plateau de Bure Interferometer (PdBI) and the IRAM-30 m telescope observations. These maps have beencomplemented with IRAM-30 m observations of several excited transitions at two different positions.Results. Bright formyl radical emission delineates the illuminated edge of the nebula, with a faint emission remaining towards theshielded molecular core. Viewed from the illuminated star, the HCO emission almost coincides with the PAH and CCH emission. HCOreaches a similar abundance to HCO + in the photon dissociation region (PDR), ≃1–2×10 −9 with respect to H 2 . To our knowledge, thisis the highest HCO abundance ever measured. Pure gas-phase chemistry models fail to reproduce the observed HCO abundance by∼2 orders of magnitude, except if reactions of atomic oxygen with carbon radicals abundant in the PDR (i.e., CH 2 ) play a significantrole in the HCO formation. Alternatively, HCO could be produced in the PDR by non-thermal processes such as photo-processing ofice mantles and subsequent photo-desorption of either HCO or H 2 CO, and further gas phase photodissociation.Conclusions. The measured HCO/H 13 CO + abundance ratio is large towards the PDR (≃50), and much lower toward the gas shieldedfrom FUV radiation (1). We propose that high HCO abundances (10 −10 ) together with large HCO/H 13 CO + abundance ratios (1)are sensitive diagnostics of the presence of active photochemistry induced by FUV radiation.Key words. astrochemistry – ISM: clouds – ISM: molecules – ISM: individual objects: Horsehead nebula – radiative transfer –radio lines: ISM1. IntroductionPhotodissociation region (PDR) models are used to understandthe evolution of far-UV (FUV; hν
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Table des matières1 Rapport de sou
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Rapport après soutenanceHabilitati
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Chapitre 2Curriculum vitaetel-00726
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2.7 ANIMATION ET DIFFUSION DE LA CU
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2.8 PARCOURS 131992-1993 ÉCOLE NOR
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Chapitre 3Copyright: IRAM/PdBIIntro
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4.4 LA LUMINOSITY CO PAR MOLÉCULE
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A&A 541, A58 (2012)Galactic Latitud
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5.2 UNE PHYSIQUE BIEN CONTRAINTE ET
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