| Issue |
A&A
Volume 569, September 2014
|
|
|---|---|---|
| Article Number | A11 | |
| Number of page(s) | 24 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201424032 | |
| Published online | 09 September 2014 | |
Online material
Appendix A: Hot core intensity and velocity maps
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.
 |
Fig. A.1
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)
CH |
| Open with DEXTER | |
 |
Fig. A.2
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. |
| Open with DEXTER | |
Appendix B: CH3OH and CH3CN myXCLASS fits
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).
 |
Fig. B.1
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 CH |
| Open with DEXTER | |
 |
Fig. B.2
Same as Fig. B.1 for core B. |
| Open with DEXTER | |
 |
Fig. B.3
Same as Fig. B.1 for core C. |
| Open with DEXTER | |
 |
Fig. B.4
Same as Fig. B.1 for core D, and only for CH3OH lines. |
| Open with DEXTER | |
© ESO, 2014
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