898 J. Pety et al.: Are PAHs precursors of small hydrocarbons in photo-dissociation regions?<strong>tel</strong>-<strong>00726959</strong>, version 1 - 31 Aug 2012interiors, probably because they coagulate and/or condense.Stepnik et al. (2003) describe a convincing case for such a processin a small filament of the Taurus cloud. Rapacioli et al.(2005) have found c<strong>le</strong>ar evidence for spatial variations of thearomatic infrared band profi<strong>le</strong>s, likely due to the spatial variationof the nature of their carriers. A sophisticated analysis ofISOCAM-CVF data allowed them to separate the mid-IR spectraof the ionized and neutral PAHs from the spectra of carbonaceousvery small grains (possibly PAH aggregates). Thevery small grains are located at a larger distance from the illuminatingstars than the PAHs, <strong>le</strong>nding support to the idea thatPAHs are produced from the photo-evaporation of these verysmall grains. Whi<strong>le</strong> more examp<strong>le</strong>s are needed to understandthe origin and fate of inters<strong>tel</strong>lar PAHs, it appears nonethe<strong>le</strong>ssthat these macro mo<strong>le</strong>cu<strong>le</strong>s are re<strong>le</strong>ased in the gas phase in theUV-illuminated regions of the inters<strong>tel</strong>lar medium, i.e. in thediffuse clouds, in PDRs, etc. In those regions, the destructionof the carbon ske<strong>le</strong>ton is the main process limiting the smal<strong>le</strong>stpossib<strong>le</strong> PAH size. It is likely that some carbon-bearingmo<strong>le</strong>cu<strong>le</strong>s are re<strong>le</strong>ased in the gas phase in the UV-illuminatedregions, either as a secondary product of the evaporation of thedust partic<strong>le</strong>s giving rise to PAHs, or as products of the destructionof the PAH carbon ske<strong>le</strong>ton.5. Summary and conclusionsWe have presented maps of the edge of the Horsehead nebula inrotational lines of excited H 2 ,CO,C 18 O and simp<strong>le</strong> hydrocarbonmo<strong>le</strong>cu<strong>le</strong>s, CCH, c-C 3 H 2 and C 4 H with 6 ′′ resolution. Allthe hydrocarbon maps are strikingly similar to each other, andto the mid-IR emission mapped by ISOCAM (Abergel et al.2003) whi<strong>le</strong> we measured a 3 to 5 ′′ offset between the hydrocarbonand H 2 peaks. State-of-the-art chemical models fail toreproduce both the PDR hydrocarbon stratification and the absoluteabundances of 2 of 3 observed hydrocarbons. We haveexamined three hypotheses to improve the models, and we concludethat the most likely explanation is that we are witnessingthe fragmentation of PAHs in the intense far-UV radiation dueto σOri.A detai<strong>le</strong>d modeling of the chemistry including this newmechanism is beyond the scope of this paper. Indeed, such amodeling requires rates for both the growth (by addition ofmo<strong>le</strong>cu<strong>le</strong>s or of carbon and hydrogen atoms) and the fragmentationof PAHs. This last item requires an accurate descriptionof the fragmentation cascade of PAHs, in all their possib<strong>le</strong>equilibrium states (ionized, neutral, partially or totally dehydrogenated,...). Laboratory experiments such as the ion cyclotronicresonance cell PIRENEA (Joblin 2003) are key instrumentsto provide such information. In addition, the rate fi<strong>le</strong>sused by the model need to be updated, especially the photodissociationrates of the simp<strong>le</strong> carbon chains. A critical reviewof the ro<strong>le</strong> of neutral-neutral reactions in inters<strong>tel</strong>lar chemistryis also warranted.Acknow<strong>le</strong>dgements. We are grateful to the IRAM staff at Plateau deBure, Grenob<strong>le</strong> and Pico Ve<strong>le</strong>ta for competent help with the observationsand data reduction. IRAM is supported by the INSU/CNRS(France), MPG (Germany) and IGN (Spain). This work has benefitedfrom many discussions with C. Joblin and C.M. Walms<strong>le</strong>y. We thankD. Lis for the communication of the (CI) map of the Horsehead nebulain advance of publication. We also thank E. Herbst for providingan updated chemical rate fi<strong>le</strong>. M.G. is grateful to the CSO for thehospitality of its office in Hilo where she worked on this paper. Weacknow<strong>le</strong>dge funding by the French CNRS/PCMI program. We thankthe referee, J. Black, for insightful comments which improved the presentationand the discussion of our results.ReferencesÁdámkovics, M., Blake, G. A., & McCall, B. J. 2003, ApJ, 595, 235Abergel, A., Bernard, J. 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2.7 ANIMATION ET DIFFUSION DE LA CU
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