Free Access
Volume 574, February 2015
Article Number A56
Number of page(s) 27
Section Interstellar and circumstellar matter
Published online 23 January 2015

Online material

Appendix A: Observed lines in this survey

thumbnail Fig. A.1

Detected spectra of HC7N and NH3 with transitions marked in the upper right of each panel. The NH3 (4, 4) and (6, 6) lines have been smoothed to have a channel width of ~3.3 km s-1, while the channel width of other lines is ~0.8 km s-1. In the NH3 (1, 1) panel, the positions of the satellites are indicated by red solid lines. The blue dashed line traces the systemic LSR velocity (26.0 km s-1) of IRC +10216.

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thumbnail Fig. A.2

Rotational diagrams for the observed molecules in IRC +10216. For lines with hfs, all observed components have been taken into account. The circles with error bars are from our Effelsberg-100 m observations, where in addition to uncertainties in the fit to the integrated line intensities, a calibration error of 20% has also been included. Filled and open symbols indicate signal-to-noise ratios that are larger than or less than five, respectively. The triangles without error bars are obtained from Kawaguchi et al. (1995). The pentagrams with error bars for C8H are obtained from Remijan et al. (2007), and the squares for C3N are from He et al. (2008). Their values have been corrected for beam dilution. The molecules and their corresponding rotational temperatures, obtained from unweighted linear fits, are given in the upper right corner of each panel. Black dashed lines represent linear least-squares fit to the rotational diagram accounting for data presented by filled symbols, and the black dot-dashed lines represent the fit when the open circles are included. The red and blue dashed lines represent fits for the para and ortho states of NH3 and c-C3H2 and the and state of l-C5H and C6H, respectively. Specifically for NH3, the red dashed line shows the fit to the (J,K) = (1, 1) and (2, 2) para-lines, the blue dashed line uses the resulting excitation temperature (39.1 K) and the ortho-(3, 3) line, the dotted red line represents a fit to the para-(1, 1), (2, 2), and (4, 4) transitions and the blue dotted line fits the ortho-(3, 3) and (6, 6) transitions.

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Appendix B: Zoom-in plots of observed spectra

thumbnail Fig. B.1

Observed spectrum of IRC +10 216 from 17.8 to 26.3 GHz.

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thumbnail Fig. B.2

Zoom in all detected and tentative lines. The rest frequency in MHz and the assigned molecule of each line are shown in the upper right of each panel. Weak lines have been smoothed to have a channel width of ~3.3 km s-1, and they are marked with “smoothed” in the upper left of the corresponding panels. Otherwise, the channel width is ~0.8 km s-1 (see Sect. 3.1). The blue dashed line traces the systemic LSR velocity (26.0 km s-1) of IRC +10216. In the C6H 23 565.2 MHz panel, the other blue dashed line near 50 km s-1 refers to the C6H’s hfs component at 23567.2 MHz.

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© ESO, 2015

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