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--- molecules:ism:hcno [2024/02/01 14:17] – [Isocyanic acid] mueller
+++ molecules:ism:hcno [2024/02/01 14:22] (current) – [Cyanic acid] mueller
@@ Line 54: / Line 54: @@
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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 H<sup>15</sup>NCO about a factor of 330 lower in abundance that the main isotopolog.\\
+\\
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 Obviously, the detection of three transitions would have been more convincing. However, there are several reasons why the detection probably can be viewed as quite secure: the number of lines is quite low in dark clouds, in particular that of U-lines; the rotational temperatures in the two sources, in which both transitions have been detected, is identical within error bars with that of HNCO; the HNCO/HCNO ratio in the sources in which HCNO line(s) have been detected, fall in a fairly narrow range of about 20 – 60.\\
+\\
+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 DCNO about a factor of 25 lower in abundance that the main isotopolog.\\
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-Contributor(s): H. S. P. Müller; 02, 2009; 05, 2009; 05, 2010; 03, 2012; 06, 2016; 05, 2018; 09, 2019
+Contributor(s): H. S. P. Müller; 02, 2009; 05, 2009; 05, 2010; 03, 2012; 06, 2016; 05, 2018; 09, 2019; 02, 2024
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