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| molecules:ism:hcns [2024/02/01 13:48] – [Thiofulminic acid] mueller | molecules:ism:hcns [2024/04/17 12:50] (current) – [Isothiocyanic acid] mueller |
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| //Astron. Astrophys.// **575**, (2015), Art. No. A84.\\ | //Astron. Astrophys.// **575**, (2015), Art. No. A84.\\ |
| The molecules were identified in the course of a line survey of the circumstellar envelope of this O-rich AGB star, aka QX Pup, with the IRAM 30 m dish at 3 to 1 mm.\\ | The molecules were identified in the course of a line survey of the circumstellar envelope of this O-rich AGB star, aka QX Pup, with the IRAM 30 m dish at 3 to 1 mm.\\ |
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| | M. Sanz-Novo, V. M. Rivilla, I. Jiménez-Serra, J. Martín-Pintado, L. Colzi, S. Zeng, A. Megías, Á. López-Gallifa, A. Martínez-Henares, S. Massalkhi, B. Tercero, P. de Vicente, D. San Andrés, S. Martín, and M. A. Requena-Torres\\ |
| | announced the\\ |
| | **[[https://doi.org/10.3847/1538-4357/ad2c01|Interstellar Detection of O-protonated Carbonyl Sulfide, HOCS<sup>+</sup>]]**\\ |
| | //Astrophys. J.// **965**, Art. No. 149 (2024).\\ |
| | The results were obtained in the course of a molecular line survey of the Galactic Center molecular cloud G+0.693–0.027 employing the Yebes 40 m and IRAM 30 m radio telecopes. The //K<sub>a</sub>// = 0 lines of HOCS<sup>+</sup> were blended with those of HNC<sup>34</sup>S because of nearly identical values of //B + C//. The transitions cover 34 to 161 GHz with //J"// = 2, 3, 6 − 13. The contribution of HNC<sup>34</sup>S could be accounted for accurately through lines of HNCS, OCS, and OC<sup>34</sup>S and turned out to be less than that of HOCS<sup>+</sup>. Several lines are slightly or more severely blended in addition, but this is in most cases also well accounted.\\ |
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| Contributor(s): H. S. P. Müller; 09, 2009; 02, 2024 | Contributor(s): H. S. P. Müller; 09, 2009; 02, 2024; 04, 2024 |
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| //Astrophys. J.// **702**, (2009), L124.\\ | //Astrophys. J.// **702**, (2009), L124.\\ |
| The Arizona Radio Observatory 12 m telescope has been employed to detect the //K<sub>a</sub>// = 0, //J// = 6 – 5 to 12 – 11 transitions; the next two transitions were also sought for, but were too weak to be detected, indicating again fairly low rotational temperatures. Observations have been made toward the Galactic center source Sgr B2(N). Though more than 3000 K higher in energy than HNCS, it is only lower in abundance by a factor of three. HNCS was also detected in this source.\\ | The Arizona Radio Observatory 12 m telescope has been employed to detect the //K<sub>a</sub>// = 0, //J// = 6 – 5 to 12 – 11 transitions; the next two transitions were also sought for, but were too weak to be detected, indicating again fairly low rotational temperatures. Observations have been made toward the Galactic center source Sgr B2(N). Though more than 3000 K higher in energy than HNCS, it is only lower in abundance by a factor of three. HNCS was also detected in this source.\\ |
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| | J. Cernicharo, M. Agúndez, C. Cabezas, B. Tercero, R. Fuentetaja, N. Marcelino, and P. de Vicente \\ |
| | announced the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202349105|Discovery of thiofulminic acid with the QUIJOTE line survey: |
| | A study of the isomers of HNCS and HNCO in TMC-1]]**\\ |
| | //Astron. Astrophys.// **682**, (2024), Art. No. L4.\\ |
| | The authors detect DSCN and H<sup>34</sup>SCN, which are about a factor of 40 lower in abundance that the main isotopolog.\\ |
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| Contributor(s): H. S. P. Müller; 09, 2009 | Contributor(s): H. S. P. Müller; 09, 2009; 02, 2024 |
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