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| molecules:ism:sip [2022/12/16 13:16] – mueller | molecules:ism:sip [2023/11/24 13:33] (current) – mueller |
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| L. A. Koelemay, M. A. Burton, A. P. Singh, P. M. Sheridan, J. J. Bernal, and L. M. Ziurys\\ | L. A. Koelemay, M. A. Burton, A. P. Singh, P. M. Sheridan, J. J. Bernal, and L. M. Ziurys\\ |
| described the\\ | described the\\ |
| **[[https://doi.org/10.3847/2041-8213/ac9d9b|Laboratory and Astronomical Detection of the SiP Radical (X<sup>2</sup>Π<sub>i</sub>): More Circumstellar | **[[https://doi.org/10.3847/2041-8213/ac9d9b|Laboratory and Astronomical Detection of the SiP Radical (X<sup>2</sup>Π<sub>i</sub>): More Circumstellar Phosphorus]]**\\ |
| Phosphorus]]**\\ | |
| //Astrophys. J. Lett.// **940**, Art. No. L11 (2022).\\ | //Astrophys. J. Lett.// **940**, Art. No. L11 (2022).\\ |
| 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 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.\\ |