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| molecules:ism:fec [2023/11/24 13:31] – created mueller | molecules:ism:fec [2023/11/24 13:40] (current) – mueller |
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| **[[https://doi.org/10.3847/2041-8213/ad0899|Elusive Iron: Detection of the FeC Radical (X<sup>3</sup>Δ<sub>i</sub>) in the Envelope of IRC+10216]]**\\ | **[[https://doi.org/10.3847/2041-8213/ad0899|Elusive Iron: Detection of the FeC Radical (X<sup>3</sup>Δ<sub>i</sub>) in the Envelope of IRC+10216]]**\\ |
| //Astrophys. J. Lett.// **958**, Art. No. L6 (2023).\\ | //Astrophys. J. Lett.// **958**, Art. No. L6 (2023).\\ |
| Dedicated observations of CW Leonis with the ARO 12 m dish at Kitt Peak as well as observations (dedicated and from a line survey) with the ARO SMT in the regions of the <sup>2</sup>Π<sub>3/2</sub>, //J"// = 7.5, 12.5, 15.5, and 16.5 transitions of SiP. Only the //J"// = 12.5 and 15.5 transitions near 215.05 and 262.81 GHz appear to be unblended. While this is fine for a tentative detection, it is too little for us to qualify for a definitive detection. The authors derive peak abundances only slightly lower than CP and even slightly higher than PN, but somewhat closer to the star.\\ | Dedicated observations of CW Leonis with the ARO SMT as well as observations from a line survey at 2 mm with the ARO 12 m dish at Kitt Peak in the regions of the <sup>3</sup>Δ<sub>3</sub>, //J"// = 5, 4, and 3 transitions of FeC. The derived column density is nearly the same as for FeCN.\\ |
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