molecules:ism:hcno

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molecules:ism:hcno [2024/02/01 14:14] – [Fulminic acid] muellermolecules:ism:hcno [2024/02/01 14:22] (current) – [Cyanic acid] mueller
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 //Astron. Astrophys.// **341**, 882–895 (1999);\\ //Astron. Astrophys.// **341**, 882–895 (1999);\\
 but also on the detection of vibrationally excited HNCO with the IRAM 30 m telescope in Gal 10.47+0.03, which is also known as W31C (or part of the same cloud complex). Several //J// = 5 – 4 and 7 – 6 transitions pertaining to the ground state and the three lowest excited vibrational states were detected near 110 and 154 GHz.\\ but also on the detection of vibrationally excited HNCO with the IRAM 30 m telescope in Gal 10.47+0.03, which is also known as W31C (or part of the same cloud complex). Several //J// = 5 – 4 and 7 – 6 transitions pertaining to the ground state and the three lowest excited vibrational states were detected near 110 and 154 GHz.\\
 +\\
 +
 +L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, J. Alcolea, 
 +V. Bujarrabal, F. Herpin, K. M. Menten, and F. Wyrowski\\
 +report on\\
 +**[[https://doi.org/10.1051/0004-6361/201424768|New N-bearing species towards OH 231.8+4.2 — HNCO, HNCS, HC3N, and NO]]**\\
 +//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.\\
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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.\\ 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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 **[[https://doi.org/10.1088/0004-637X/697/1/880|Laboratory Detection of HOCN and Tentative Identification in Sgr B2]]**\\ **[[https://doi.org/10.1088/0004-637X/697/1/880|Laboratory Detection of HOCN and Tentative Identification in Sgr B2]]**\\
 //Astrophys. J.// **697**, (2009), 880.\\ //Astrophys. J.// **697**, (2009), 880.\\
-The transitions detected were the //K<sub>a</sub>// = 0, //J// = 4 – 3 and 5 – 4; the 5 – 4 and 6 – 5; and the 7 – 6. The first two pairs of transitions have fairly similar intensities, the last, singly observed transition had not been calibrated. Even though the detection was deemed tentative, it is probably fairly secure.+The transitions detected were the //K<sub>a</sub>// = 0, //J// = 4 – 3 and 5 – 4; the 5 – 4 and 6 – 5; and the 7 – 6. The first two pairs of transitions have fairly similar intensities, the last, singly observed transition had not been calibrated. Even though the detection was deemed tentative, it is probably fairly secure.\\ 
 +\\
  
 More recently, the Sgr B2 region was studied more thoroughly by:\\ More recently, the Sgr B2 region was studied more thoroughly by:\\
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 **[[https://doi.org/10.1051/0004-6361/200912456|Interstellar HOCN in the Galactic Center Region]]**\\ **[[https://doi.org/10.1051/0004-6361/200912456|Interstellar HOCN in the Galactic Center Region]]**\\
 //Astron. Astrophys.// **516**, (2010), Art. No. A109.\\ //Astron. Astrophys.// **516**, (2010), Art. No. A109.\\
-Data from a line survey of Sgr B2(M) and (N) were supplemented by dedicated searches toward several other positions in the Sgr B2 region. Up to four //K<sub>a</sub>// = 0 transitions were detected with the IRAM 30 m telescope. The transitions had //J"// = 3, 4, 6, and 7 and extend from 83 to 168 GHz. Interestingly, they authours found a nearly contant HNCO/HOCN ratio of around 200. Moreover, the molecules were less abundant toward the hot and dense regions.+Data from a line survey of Sgr B2(M) and (N) were supplemented by dedicated searches toward several other positions in the Sgr B2 region. Up to four //K<sub>a</sub>// = 0 transitions were detected with the IRAM 30 m telescope. The transitions had //J"// = 3, 4, 6, and 7 and extend from 83 to 168 GHz. Interestingly, they authours found a nearly contant HNCO/HOCN ratio of around 200. Moreover, the molecules were less abundant toward the hot and dense regions.\\ 
 +\\
  
 N. Marcelino, M. Agúndez, J. Cernicharo, E. Roueff, and M. Tafalla\\ N. Marcelino, M. Agúndez, J. Cernicharo, E. Roueff, and M. Tafalla\\
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 **[[https://doi.org/10.1051/0004-6361/201833074|Discovery of the Elusive Radical NCO and Confirmation of H<sub>2</sub>NCO<sup>+</sup> in Space]]**\\ **[[https://doi.org/10.1051/0004-6361/201833074|Discovery of the Elusive Radical NCO and Confirmation of H<sub>2</sub>NCO<sup>+</sup> in Space]]**\\
 //Astron. Astrophys.// **612**, Art. No. L10 (2018).\\ //Astron. Astrophys.// **612**, Art. No. L10 (2018).\\
-They also observed HOCN along with HCNO and HNCO toward the dense core L483 in the course of a 3 mm line survey carried out with the IRAM 30 m telescope. +They also observed HOCN along with HCNO and HNCO toward the dense core L483 in the course of a 3 mm line survey carried out with the IRAM 30 m telescope.\\ 
 +\\
  
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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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