[tel-00726959, v1] CaractÃ©riser le milieu interstellaire ... - HAL - INRIA

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A&A 464, L41–L44 (2007)DOI: 10.1051/0004-6361:20067009c○ ESO 2007Astronomy&AstrophysicsLetter to the EditorDeuterium fractionation in the Horsehead edge ⋆J. Pety 1,2 , J. R. Goicoechea 2 , P. Hily-Blant 1 ,M.Gerin 2 , and D. Teyssier 31 IRAM, 300 rue de la Piscine, 38406 Grenoble Cedex, Francee-mail: [pety;hilyblan]@iram.fr2 LERMA, UMR 8112, CNRS, Observatoire de Paris and École Normale Supérieure, 24 rue Lhomond,75231 Paris Cedex 05, Francee-mail: [javier;gerin]@lra.ens.fr3 European Space Astronomy Centre, Urb. Villafranca del Castillo, PO Box 50727, Madrid 28080, Spaine-mail: dteyssier@sciops.esa.intReceived 22 December 2006 / Accepted 22 January 2007ABSTRACTtel-00726959, version 1 - 31 Aug 2012Context. Deuterium fractionation is known to enhance the [DCO + ]/[HCO + ] abundance ratio over the D/H ∼ 10 −5 elemental ratio inthe cold and dense gas typically found in pre-stellar cores.Aims. We report the first detection and mapping of very bright DCO + J = 3−2 andJ = 2−1 lines (3 and 4 K respectively) towardsthe Horsehead photodissociation region (PDR) observed with the IRAM-30 m telescope. The DCO + emission peaks close to theilluminated warm edge of the nebula (
L42J. Pety et al.: Deuterium fractionation in the Horsehead edgeTable 1. Observation parameters. The projection center of all the data is α 2000 = 05 h 40 m 54.27 s , δ 2000 = −02 ◦ 28 ′ 00 ′′ .Molecule Transition Frequency Instrument # Pix. a aF effaB eff Resol. Resol. Int. Time a,b Noise c Obs. date aGHz arcsec km s −1 hours KH 13 CO + J = 3−2 260.255339 30 m/HERA 9 0.90 0.46 13.5 ′′ 0.20 5.9/11.3 0.06 Mar. 2006H 13 CO + J = 1−0 86.754288 30 m+PdBI 2 0.95 0.78 6.7 ′′ 0.20 2.6/4.5 0.10 Sep. 2006DCO + J = 3−2 216.112582 30 m/HERA 9 0.90 0.52 11.4 ′′ 0.11 1.5/2.0 0.10 Mar. 2006DCO + J = 2−1 144.077289 30 m/CD150 2 0.93 0.69 18.0 ′′ 0.08 5.9/8.7 0.18 Sep. 2006C 18 O J = 2−1 219.560319 30 m/HERA 9 0.91 0.55 11.2 ′′ 0.11 – 0.26 May 2003Continuum at 1.2 mm 30 m/MAMBO 117 – – 11.7 ′′ – – – –a Those columns apply to the 30 m data but not to the PdBI data for the H 13 CO + J = 1−0 line. b Two values are given for the integration time: theon-source time and the telescope time. c Noise values estimated at the position of the DCO + peak.tel-00726959, version 1 - 31 Aug 2012scanning direction. This ensured Nyquist sampling between therows except at the edges of the map. The DCO + J = 2−1 was observedduring 11.3 h using the C150 and D150 single-side bandreceivers of the IRAM-30 m under ∼8.5 mm of water vapor. Weused the frequency-switched, on-the-fly observing mode over a160 ′′ × 170 ′′ portion of the sky. Scanned lines and rows wereseparatedby8 ′′ ensuring Nyquist sampling. A detailed descriptionof the C 18 O J = 2−1 and 1.2 mm continuum observationsand data reductions can be found in Hily-Blant et al. (2005). Weestimate the absolute position accuracy to be 3 ′′ .We also use a small part of the H 13 CO + (J = 1−0 andJ = 3−2) data, which were obtained with the IRAM PdBIand 30 m telescopes. The whole data set will be comprehensivelydescribed in a forthcoming paper studying the fractional ionizationacross the Horsehead edge (Hily-Blant et al. 2007, in prep.).In short, the H 13 CO + J = 3−2 line was observed under averagedwinter weather (∼3.5 mm of water vapor) in rasters along thedirection of the exciting star using the first polarization of theunrotated HERA. Each pointing of the rasters was observed infrequency-switched mode. This resulted in a 140 ′′ × 75 ′′ map,Nyquist sampled along the direction of the exciting star butslightly undersampled in the orthogonal direction (i.e. rows separatedby 6 ′′ instead of 4.75 ′′ ). The noise increases quickly atthe map edges which were seen only by a fraction of the HERApixels. We finally used a frequency-switched, on-the-fly map ofthe H 13 CO + J = 1−0 line, obtained at the IRAM-30 m usingthe A100 and B100 3 mm receivers (∼7 mm of water vapor) toproduce the short-spacings needed to complement a 7-field mosaicacquired with the 6 PdBI antennae in the CD configuration(baseline lengths from 24 to 176 m).The data processing was done with the GILDAS 1 softwares(Pety 2005). The IRAM-30 m data were first calibratedto the TA ∗ scale using the chopper wheel method (Penzias &Burrus 1973), and finally converted to main beam temperatures(T mb ) using the forward and main beam efficiencies (F effand B eff ) displayed in Table 1. The resulting amplitude accuracyis ∼10%. Frequency-switched spectra were folded using thestandard shift-and-add method, after baseline subtraction. Theresulting spectra were finally gridded through convolution by aGaussian.2. Results and discussionFigure 1 presents the DCO + J = 2−1 andJ = 3−2 andtheC 18 O J = 2−1 integrated intensity maps, together with 1.2 mmcontinuum emission. All maps are presented in a coordinate systemadapted to the source geometry, as described in the figure1 See http://www.iram.fr/IRAMFR/GILDAS for more informationabout the GILDAS softwares.Fig. 1. IRAM-30 m integrated intensity maps. Maps have been rotatedby 14 ◦ counter-clockwise around the projection center, shown as thegreen cross at (δx,δy) = (20 ′′ , 0 ′′ ), to bring the exciting star direction inthe horizontal direction and the horizontal zero has been set at the PDRedge, delineated by the dashed blue vertical line. The spatial resolutionis plotted in the bottom left corner. Values of contour levels are shownon each image lookup table. The emission of all lines is integrated between10.1 and 11.1 km s −1 .caption. The DCO + emission is concentrated in a narrow, arclikestructure, delineating the left edge of the dust continuumemission. A second maximum is found at the extreme left of themap, associated with a smaller dust continuum peak. Figure 2shows the H 13 CO + and DCO + spectra in a cut along the directionof the exciting star at δy = 15 ′′ (horizontal dashed line of Fig. 1).This cut intersects the DCO + emission peak which is close to theilluminated edge of the nebula (
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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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