Volume 569, September 2014
|Number of page(s)||24|
|Section||Interstellar and circumstellar matter|
|Published online||09 September 2014|
In Figs. A.1 and A.2, we present the zeroth (integrated intensity) and first (velocity field) moment maps of various hot-core tracers detected towards cores A and B. In Sect. 3.2.2, we describe how the moments have been obtained, while the symbols shown in these two figures are described in the caption of Fig. 4.
Maps of the integrated intensity (upper panels) and velocity field (bottom panels) of a) CH3CN K = 2 at 349.426 GHz; b) CH3CN K = 8 at 349.024 GHz; c) CHCN K = 2 at 349.254 GHz; and d) CH3CN v8 = 1K,l = 3,1 at 350.552 GHz towards cores A and B. For the different panels, the starting (and increasing contour levels in terms of σ, in Jy beam-1 km s-1) are 5σ (10σ, with σ = 0.15), 5σ (10σ, with σ = 0.15), 3σ (3σ, with σ = 0.10), and 5σ (10σ, with σ = 0.10) for core A; and 5σ (5σ, with σ = 0.09), 4σ (4σ, with σ = 0.09), 2σ (2σ, with σ = 0.06), and 3σ (3σ, with σ = 0.06) for core B. See details and description of symbols in Fig. 4.
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Maps of the integrated intensity (upper panels) and velocity field (bottom panels) of a) CH3OCHO (266,20–256,19); b) CH3OCHO (277,21–267,20); c) H2CS (101,9–91,8), d) HNCO (161,16–151,15); e) SO2 (184,14–183,15); and f) HC3N (37–36) towards cores A and B. For the different panels, the starting (and increasing contour levels in terms of σ, in Jy beam-1 km s-1) are 5σ (10σ, with σ = 0.06), 3σ (3σ, with σ = 0.04), 5σ (10σ, with σ = 0.16), 5σ (10σ, with σ = 0.10), 5σ (5σ, with σ = 0.20), and 5σ (10σ, with σ = 0.11) for core A; and 3σ (3σ, with σ = 0.03), 1σ (1σ, with σ = 0.02), 5σ (5σ, with σ = 0.09), 5σ (5σ, with σ = 0.06), 5σ (5σ, with σ = 0.10), and 5σ (10σ, with σ = 0.07) for core B. See details and description of symbols in Fig. 4.
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In Figs. B.1–B.4 we show the spectra of the bulge of methanol (CH3OH, black line in the top panels) and methyl cyanide (CH3CN, black line in the bottom panels) lines observed toward cores A, B, C and D. For this last core, the methyl cyanide lines are too weak and cannot be fitted. The observed spectra have been fitted (red lines) using myXCLASS (see Sect. 4.1). The procedure searches, by minimizing the χ2, for the best fit of five parameters: size (in arcsec), temperature (in K), column density (in cm-2), linewidth (in km s-1) and LSR velocity (in km s-1). The blue lines in the small panels show the χ2 of the fits for different values of the parameters. In Table 3, we list the values of the parameters obtained in the best fits. We note that we have simultaneously fitted optically thick and thin transitions (e.g., ground state, vibrationally excited and isotopologues of CH3CN and CH3OH), thus avoiding possible degeneracies (see Zernickel et al. 2012) between the parameters of the fit (e.g., column density and size).
Large panels: observed CH3OH (top panel) and CH3CN (bottom panel) lines toward core A in G35.20−0.74 N. The red line shows the best fitted obtained by myXCLASS (see Sect. 4.1). The fit in the top panel includes ground state CH3OH and 13CH3OH and torsionally excited CH3OH lines, while the fit in the bottom panel includes ground state CH3CN and CHCN and vibrationally excited CH3CN lines in the frequency ranges shown in the panels. Small panels: χ2 values obtained from the fits minimization. From left to right the panels show the size, the temperature, the column density, the linewidth and the LSR velocity.
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© ESO, 2014
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