This shows you the differences between two versions of the page.
Both sides previous revision Previous revision | Last revisionBoth sides next revision |
molecules:ism:sip [2022/12/16 13:11] – mueller | molecules:ism:sip [2022/12/16 13:16] – mueller |
---|
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. | 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.\\ |
| \\ |
| |
---- | ---- |