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. Author manuscript; available in PMC: 2017 Nov 13.
Published in final edited form as: Astron Astrophys. 2017 Oct 9;606:L5. doi: 10.1051/0004-6361/201731672

Fig. 1.

Fig. 1

Observed rotational lines of methyl silane, CH3SiH3, towards IRC+10216 in antenna temperature (in K). The spectral resolution is 1 MHz for lines below 200 GHz, and 2 MHz above that frequency. Rest frequencies are indicated for an assumed LS R velocity of the source of −26.5 km s−1. The arrows indicate the position of the K = 0, 1, 2, and 3 components of each J → (J – 1) rotational transition. In most cases the K = 0 and 1 components appear superposed. The identification of other features found in the spectra is indicated. Some of the CH3SiH3 lines are partially blended, but their red or blue parts are still clearly visible in the spectra. Green lines correspond to the emerging line profiles calculated with the model discussed in the text.