| Issue |
A&A
Volume 571, November 2014
|
|
|---|---|---|
| Article Number | A52 | |
| Number of page(s) | 24 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201424031 | |
| Published online | 06 November 2014 | |
Online material
Appendix A: IR images
In Figs. A.1 and A.2, we show the IR and submillimeter images of G35.03 from the Spitzer GLIMPSE survey, Subaru COMICS, the Herschel Hi-GAL survey, and the CSO BGPS survey at representative wavelengths.
 |
Fig. A.1
Spitzer 3.6, 4.5, and 8.0 μm (from the GLIMPSE survey), and Subaru COMICS 25 μm images on linear scale toward the star-forming region G35.03. The crosses indicate the positions of the submillimeter continuum cores (Table 3). |
| Open with DEXTER | |
 |
Fig. A.2
Herschel 70, 160, 250, 350, and 500 μm (from the Hi-GAL survey), and CSO 1100 μm (from the Bolocam survey) images on linear scale toward the star-forming region G35.03. The crosses indicate the positions of the submillimeter continuum cores (Table 3). |
| Open with DEXTER | |
Appendix B: CH3OH myXCLASS fits
In Figs. B.1–B.6, we show the spectra of the methanol lines observed toward cores A, B, C, D, E, and F. The observed spectra (black lines) have been fitted (red lines) using myXCLASS (see Sect. 4.1). The procedure searches, by minimizing the χ2, the best fit of five input parameters: size (in arcsec), temperature (in K), column density (in cm-2), line width (in km s-1), and LSR velocity (in km s-1). In Table 5, we list the values of the temperature, column density, and line width obtained in the best fits.
 |
Fig. B.1
Observed CH3OH lines (black lines) toward core A in G35.03. The red line shows the best fit obtained with myXCLASS (see Sect. 4.1). The fit includes ground-state CH3OH and 13CH3OH and torsionally excited CH3OH lines in the frequency ranges shown in the panel. |
| 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 | |
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Fig. B.4
Same as Fig. B.1 for core D. |
| Open with DEXTER | |
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Fig. B.5
Same as Fig. B.1 for core E. |
| Open with DEXTER | |
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Fig. B.6
Same as Fig. B.1 for core F. |
| Open with DEXTER | |
© ESO, 2014
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