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892 J. Pety et al.: Are PAHs precursors of small hydrocarbons in photo-dissociation regions?tel-00726959, version 1 - 31 Aug 2012Fig. 5. Emission profiles along the exciting star direction (PA = −104 ◦ in the equatorial coordinate system). To improve the signal-to-noiseratio, those emission profiles have been integrated along the perpendicular direction between −15 ′′
J. Pety et al.: Are PAHs precursors of small hydrocarbons in photo-dissociation regions? 893Table 3. Molecular column densities and abundances at 3 differentpositions of the PDR named “Cloud”, “IR peak” and “IR edge”.Equatorial offsets refer to the Mosaic 2 map center given in Table 1.(δx,δy)offsets refer to the coordinate system defined in Fig. 3. H 2 columndensities have been derived from the 1.2 mm dust continuumemission using a dust temperature range of 20 to 40 K for the “Cloud”position and 40 to 80 K for the IR positions. Others column densitiesused LVG models with a representative set of densities and kinetictemperature. 1-σ uncertainties thus reflect the systematics dueto the approximate knowledge of density and kinetic temperature.Abundances are computed with respect to the number of protons, i.e.[X] = 0.5 N(X)/N(H 2 ).δRA δDec δx δyCloud +6 ′′ −4 ′′ +24.9 ′′ −5.3 ′′IR peak −6 ′′ −4 ′′ +12.2 ′′ −2.4 ′′IR edge −12 ′′ −4 ′′ +7.4 ′′ −1.0 ′′tel-00726959, version 1 - 31 Aug 2012Fig. 6. Spatial variation along the direction of the exciting star of a) the12 CO J = 2−1 brightness temperature (convolved at the same angularresolution as the J = 1−0 transition); b) 1−0/2−1 ratio and c), d),e) the kinetic temperature. (δx,δy)offsets refer to the coordinate systemdefined in Fig. 3. The cuts at δy =+10 ′′ are drawn in blue, thoseat δy = +5 ′′ in green and those δy = +0 ′′ in red. The data cutshave been taken from the 10.6 km s −1 velocity channel correspondingto the 12 CO line peak. The kinetic temperature is derived from anLVG model assuming i) unity beam filling factor; and ii) uniform totalhydrogen density of n H = 1.6 × 10 4 cm −3 (dashed lines), 2 × 10 4 cm −3(full lines), 4 × 10 4 cm −3 (dotted lines) and 10 5 cm −3 (dotted-dashedlines). Arrows indicate lower limits.parameters. As the observations involve complex carbonmolecules, we have used the so-called “new standard model”chemical rate file of Herbst and collaborators (Lee et al. 1998),available on the web site 3 . In a previous paper (Teyssier et al.2004), we have found that the other extensive chemical rate fileprovided by the UMIST group (Le Teuff et al. 2000) gave close3 http://www.physics.ohio-state.edu/˜eric/research_files/cddata.july03Quantity Unit Cloud IR peak IR edgeS 1.2mm mJy/Beam 38 ± 2 35± 2 12± 2N(H 2 ) 10 21 cm −2 27 ± 9.5 10.5 ± 4 3.6± 1.7N(C 18 O) 10 15 cm −2 5.8 ± 0.5 4 ± 0.5 1 ± 0.3N(CCH) 10 13 cm −2 5.5 ± 1 30± 5 11± 3N(c-C 3 H 2 ) 10 12 cm −2 2.3 ± 0.7 24 ± 10 9.5 ± 5N(C 4 H) 10 12 cm −2 20 ± 10 40 ± 10 37 ± 10Quantity Unit Cloud IR peak IR edge[C 18 O] 10 −7 1.07 1.9 1.4[CCH] 10 −8 0.10 1.4 1.5[c-C 3 H 2 ] 10 −10 0.43 11.4 13.2[C 4 H] 10 −9 0.37 1.9 5.2results for the carbon chain molecules. As C 18 O observationsare reported, we have added to this reaction set the main isotopicmolecules involving 18 O and introduced the correspondingfractionation reactions (Graedel et al. 1982). We have alsointroduced the photo-dissociation rates given by van Dishoeck(1988), when available, which have been calculated specificallywith the Draine ISRF and which were different from the valuesreported in the chemical rate file. The resulting chemical networkinvolves about 450 chemical species and 5000 reactions.Only the most stable isomeric forms of hydrocarbons are consideredhere.We define a reference model (hereafter named model A)of the Horsehead nebula as a uniform sheet of gas and dustof total hydrogen density n H = 10 5 cm −3 exposed to a ISRFof 100 measured in Draine units. The cosmic ray ionizationrate has a value of 5 × 10 −17 s −1 and the elemental abundancesare as follows: C/H = 1.38 × 10 −4 ,O/H = 3.02 × 10 −4 ,18 O/H = 6 × 10 −7 ,N/H = 7.95 × 10 −5 ,S/H = 5.8 × 10 −8 ,Cl/H = 1.86 × 10 −9 ,P/H = 9.3 × 10 −10 ,Fe/H = 1.7 × 10 −9 ,Mg/H = 10 −8 ,Na/H = 2.3 × 10 −9 . The properties of the grainsare the same as described in Le Petit et al. (2002), i.e. the sizedistribution law is taken from Mathis et al. (1977) with an exponentof −3.5 and we describe the attenuation of grains from theArticle published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx.doi.org/10.1051/0004-6361:20041170
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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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4.2 ETUDES DIRECTES EN ÉMISSION 19
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4.4 LA LUMINOSITY CO PAR MOLÉCULE
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356 E. Falgarone et al.: Extreme ve
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Table 1. Observation parameters for
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CLASS evolution: I. Improved OTF su
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CLASS evolution: I. Improved OTF su
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Table C.1. Definition of the symbol
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IRAM Memo 2011-2WIFISYN:The GILDAS
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WIFISYN3. practiceWIFISYN3. practic
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WIFISYNA. implementation planWIFISY
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A EXHAUSTIVE DESCRIPTION OF THE CHA
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9.3 ACTIVITÉS 2008-2011 237tel-007
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Contribution de l'Action Spécique
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