Issue |
A&A
Volume 574, February 2015
|
|
---|---|---|
Article Number | A56 | |
Number of page(s) | 27 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/201424819 | |
Published online | 23 January 2015 |
Online material
Appendix A: Observed lines in this survey
![]() |
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. |
Open with DEXTER |
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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 |
Open with DEXTER |
![]() |
Fig. A.2
continued. |
Open with DEXTER |
![]() |
Fig. A.2
continued. |
Open with DEXTER |
Appendix B: Zoom-in plots of observed spectra
![]() |
Fig. B.1
Observed spectrum of IRC +10 216 from 17.8 to 26.3 GHz. |
Open with DEXTER |
![]() |
Fig. B.1
continued. |
Open with DEXTER |
![]() |
Fig. B.1
continued. |
Open with DEXTER |
![]() |
Fig. B.1
continued. |
Open with DEXTER |
![]() |
Fig. B.1
continued. |
Open with DEXTER |
![]() |
Fig. B.1
continued. |
Open with DEXTER |
![]() |
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. |
Open with DEXTER |
![]() |
Fig. B.2
continued. |
Open with DEXTER |
![]() |
Fig. B.2
continued. |
Open with DEXTER |
![]() |
Fig. B.2
continued. |
Open with DEXTER |
© ESO, 2015
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