Free Access
Issue
A&A
Volume 579, July 2015
Article Number A51
Number of page(s) 20
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201321269
Published online 26 June 2015

Online material

Appendix A: Ammonia spectra

Table A.1

Summary of ammonia emission peaks shown in Figs. 16.

thumbnail Fig. A.1

VLA NH3 spectra of IRDC010.70 at the position p1. Left-hand side: NH3(1, 1) spectra and right-hand side: NH3(2, 2) spectra. The red line corresponds to the fit. As we do not observe the hyperfine structure of the NH3(2, 2) transition, we show a Gaussian fit to the main component. The fit parameters and coordinates of the spectra are given in Table A.1.

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thumbnail Fig. A.2

NH3 spectra of IRDC079.31. Left-hand side: NH3(1, 1) spectra and right-hand side: NH3(2, 2) spectra. Top two panels: Effelsberg 100 m observations, central panels: combined VLA and Effelsberg 100 m spectra at the position p1 and bottom panels: combined VLA and Effelsberg 100 m spectra at the position p2. The red line corresponds to the fit. As we do not observe the hyperfine structure of the NH3(2, 2) transition, we show a Gaussian fit to the main component. The fit parameters and coordinates of the spectra are given in Table A.1.

Open with DEXTER

thumbnail Fig. A.3

NH3 spectra of ISOSS18364. Left-hand side: NH3(1, 1) spectra and right-hand side: NH3(2, 2) spectra. Top two panels: Effelsberg 100 m observations and bottom panels: combined VLA and Effelsberg 100 m spectra at the position p1. The red line corresponds to the fit. As we do not observe the hyperfine structure of the NH3(2, 2) transition, we show a Gaussian fit to the main component. We do not detect the NH3(2, 2) line for the Effelsberg 100 m observations within the uncertainties. The fit parameters and coordinates of the spectra are given in Table A.1.

Open with DEXTER

thumbnail Fig. A.4

NH3 spectra of ISOSS20153. Left-hand side: NH3(1, 1) spectra and right-hand side: NH3(2, 2) spectra. Top two panels: Effelsberg 100 m observations, central panels: combined VLA and Effelsberg 100 m spectra at the position p1, and bottom panels: combined VLA and Effelsberg 100 m spectra at the position p2. The red line corresponds to the fit. Since we did not observe the hyperfine structure of the NH3(2, 2) transition, we show a Gaussian fit to the main component. We do not detect the NH3(2, 2) line at the position p2 within the uncertainties. The fit parameters and coordinates of the spectra are given in Table A.1.

Open with DEXTER

thumbnail Fig. A.5

NH3 spectra of ISOSS22478. Left-hand side: NH3(1, 1) spectra and right-hand side: NH3(2, 2) spectra. Top two panels: Effelsberg 100 m observations and bottom panels: combined VLA and Effelsberg 100 m spectra at the position p1. The red line corresponds to the fit. Within the uncertainties, we do not detect the NH3(2, 2) line. The fit parameters and coordinates of the spectra are given in Table A.1.

Open with DEXTER

thumbnail Fig. A.6

NH3 spectra of ISOSS23053. Left-hand side: NH3(1, 1) spectra, and right-hand side: NH3(2, 2) spectra. Top two panels: Effelsberg 100 m observations, central panels: combined VLA and Effelsberg 100 m spectra at the position p1, and bottom panels: combined VLA and Effelsberg 100 m spectra at the position p2. The red line corresponds to the fit. Since we do not observe the hyperfine structure of the NH3(2, 2) transition, we show a Gaussian fit to the main component. The fit parameters and coordinates of the spectra are given in Table A.1.

Open with DEXTER


© ESO, 2015

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