[tel-00726959, v1] Caractériser le milieu interstellaire ... - HAL - INRIA

A&A 541, A58 (2012)α(J2000)-19H57m56m55m3.8W CO [K km s -1 ]64206B0736+017100%50%25%0.08 0.10 0.12 0.14 0.16 0.18B1954+51364206B0954+6580.08 0.10 0.12 0.14 0.16 0.18B2251+15854m-2 0 2 4V LSR (KM S -1 )0.3W CO [K km s -1 ]420420tel-00726959, version 1 - 31 Aug 2012Fig. 13. A right ascension-velocity diagram of CO emission throughthe position of B1954+513. The HCO + (not CO) absorption spectrumtoward B1954 is shown with its 0-level at the location of the continuumsource; the peak absorption is 90%. Contours are shown atlevels 1−3, ... K.δ (J2000)51˚20'51˚10'51˚00'50˚50'6.40.08 0.10 0.12 0.14 0.16 0.18E BV0.08 0.10 0.12 0.14 0.16 0.18E BVFig. 15. Distribution of E B−V and W CO for four fields mapped herein CO. Each 20 ′′ pixel in the CO maps is plotted as a separate point.The (red) dashed lines in each panel show the CO emission expectedif 25%, 50% and 100% of the gas is in molecular form with a typicalvalue of the W CO -N(H 2 ) conversion factor, N(H 2 )/W CO = 2 ×10 20 H 2 cm −2 (K km s −1 ) −1 . In each panel a (green) filled diamond isshown at the value given in Table 1 toward the background source.W CO [K km s -1 ]20151050B0528+1340.8 1.020151050B2200+4200.25 0.30 0.35 0.4015B0212+73515B0224+67150˚40'-20 -10 0V LSR (KM S -1 )0.3W CO [K km s -1 ]10501050Fig. 14. A declination-velocity diagram of CO emission at theright ascension of B0355+508. The CO absorption spectrum towardB0355+508 is shown with its baseline level at the declination of thebackground source. The strongest CO absorption line is quite opaque,see Fig. 12.and BL Lac, using the original ARO data and versions of the datasmoothed to lower angular resolution 3 ′ (similar to NANTEN)and 5 ′ (similar to Planck). The brightness distribution of theCO around B0954+658 is compact in Fig. 3 but still sufficientlyextended that 4.5 K km s −1 integrated intensities are present at5 ′ resolution; this is well above the line for f H2 = 1inFig.15.The distribution of strongly emitting CO around BL Lacis sufficiently broad in angle that 20−30% of the pixels are0.65 0.70 0.75 0.80 0.85 0.90E BV1.0 1.2E BVFig. 16. As in Fig. 15 for four fields with larger reddening.occupied by CO with W CO ≥ 5Kkms −1 whether the angularresolution is 1 ′ or 5 ′ ; the very strongest CO lines haveW CO> ∼ 15 K km s −1 at 1−5 ′ resolution in the BL Lac field.This is consistent with our recent observations of CO emissionin the field around ζ Oph (Liszt et al. 2009) wherethesamepeak brightnesses were found in ARO and NANTEN data at3 ′ resolution.Because high CO brightness, and, therefore, impossiblyhigh ratios W CO /E B−V (requiring f H2 > 1 for the meanA58, page 16 of 23