molecules:ism:hcno

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revision Previous revision
Next revision		 Previous revision
molecules:ism:hcno [2024/02/01 14:14] – [Cyanic acid] muellermolecules:ism:hcno [2024/02/01 14:22] (current) – [Cyanic acid] mueller
Line 30: Line 30:
 //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.\\
 \\ \\
  
Line 46: Line 54:
 \\ \\
  
 +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.\\
 +\\
  
 ---- ----
Line 58: Line 73:
  
 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.\\
 \\ \\
  
Line 87: Line 110:
 ---- ----
  
-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
  
 ---- ----
  
  
  • molecules/ism/hcno.1706793295.txt.gz
  • Last modified: 2024/02/01 14:14
  • by mueller