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

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H. S. Liszt and J. Pety: Imaging diffuse clouds: bright and dark gas mapped in CO54m30sΔδ=20"2.831m1 2 33.9α(J2000)-22H54m53m30s-14 -12 -10 -8 -6V LSR (KM S -1 )0.3α(J2000)-2H30m29m28m27m1 23tel-00726959, version 1 - 31 Aug 2012Fig. A.1. A right ascension-velocity diagram of CO emission 20 ′′ Northof B2251+158. The CO absorption spectrum toward B2251 is shownwith its 0-level at the location of the continuum source; the peak absorptionis 22%, see Fig. 7. Contours are shown at levels 1−3, ... K.α(J2000)-2H21m20m19m18m17m16m15m14m1-10 0V LSR (KM S -1 )122.80.3Fig. A.2. A right ascension-velocity diagram of CO emission acrossthe field of B0212+735. The CO absorption spectrum toward B0212is shown with its 0-level at the location of the continuum source; thestrongest absorption line is quite opaque, see Fig. 10. Contours areshown at levels 1−3, ... K.-10 0V LSR (KM S -1 )0.3Fig. A.3. A right ascension-velocity diagram of CO emission across thefield of B0224+671 at the declination of the continuum source. TheCO absorption spectrum toward B0224+671 is shown with its 0-levelat the location of the continuum source; the peak optical depth is 1.2,see Fig. 11. Contours are shown at levels 1−3, ... K.that occur in the absorption line profiles are somewhat haphazardsamples of the larger scale gas distribution traced in CO emissionbut toward B0212+735 the diagram also indicates how theCO emission underrepresents the molecular gas distribution.Appendix B: The galaxy viewed in atomic gasaround the background targetsTo provide context for the kinematics seen in the present work,Figs. B.1 and B.2 show large-galactic-scale H I latitude-velocitydiagrams for each of the sources studied here, using results ofthe LDSS survey of Hartmann & Burton (1997). The spatial resolutionof these data is 35 ′ and the data are on a 30 ′ grid. Thediagrams were constructed at the galactic longitude nearest thebackground target (see Table 1). The latitudes of the sources aremarked. Even if it was not apparent from the overlap of the H Iand molecular absorption in the figures in the text, these mapsmake it clear that the molecular gas studied here is part of “normal”galactic structure, mixed into the general ISM.Appendix A: CO line kinematicsaround three additional objectsShown in Figs. A.1−A.3 are position-velocity diagrams in rightascension across the positions of B2251+158, b0212+735 andB0224+671. As in Figs. 13 and 14 in the main text, theHCO + absorption spectrum toward the continuum backgroundtarget is superposed in the figures with its baseline positionedwhere the diagram most nearly crosses the location of the continuum.These diagrams are intended to show how the featuresA58, page 21 of 23
A&A 541, A58 (2012)Galactic LatitudeB0212+73510220˚ B0224+6712020˚20404010˚606010˚800˚20 40600˚20 80 40 60Galactic Latitude116-50 0V LSR (KM S -1 )0-10˚-50 0V LSR (KM S -1 )0B0355+50820 40116B0415+3792089tel-00726959, version 1 - 31 Aug 2012Galactic Latitude10˚0˚-10˚608010020 40-50 0V LSR (KM S -1 )B0528+13440 20Galactic Latitude10˚0˚-10˚0130B0736+01780406020 4060-50 0V LSR (KM S -1 )0101Galactic Latitude0˚-10˚60 8010020 4060Galactic Latitude10˚0˚204060 8010020 40 6080-10˚-20˚-40 -20 0 20V LSR (KM S -1 )00 50V LSR (KM S -1 )0Fig. B.1. Latitude-velocity diagrams of H I brightness around six background targets used for mm-wave molecular absorption studies, usingH I data from the LDSS survey (Hartmann & Burton 1997). The spatial resolution is 35 ′ and the diagrams were constructed at the nearestlongitude on the 0.5 ◦ grid of the survey datacube. The latitudes of the sources are marked. The line of sight toward B0415+379 (3C 111) is notdiscussed in this work.A58, page 22 of 23
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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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CLASS evolution: I. Improved OTF su
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3 REQUIREMENTS 44 CHANGES FOR END-U
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A EXHAUSTIVE DESCRIPTION OF THE CHA
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