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molecules:ism:hcno [2024/02/01 14:14] – [Fulminic acid] mueller | molecules:ism:hcno [2024/02/01 14:22] (current) – [Cyanic acid] mueller | ||
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//Astron. Astrophys.// | //Astron. Astrophys.// | ||
but also on the detection of vibrationally excited HNCO with the IRAM 30 m telescope in Gal 10.47+0.03, | but also on the detection of vibrationally excited HNCO with the IRAM 30 m telescope in Gal 10.47+0.03, | ||
+ | \\ | ||
+ | |||
+ | L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, | ||
+ | V. Bujarrabal, F. Herpin, K. M. Menten, and F. Wyrowski\\ | ||
+ | report on\\ | ||
+ | **[[https:// | ||
+ | //Astron. Astrophys.// | ||
+ | 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:// | ||
+ | A study of the isomers of HNCS and HNCO in TMC-1]]**\\ | ||
+ | //Astron. Astrophys.// | ||
+ | The authors detect H< | ||
+ | \\ | ||
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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:// | ||
+ | A study of the isomers of HNCS and HNCO in TMC-1]]**\\ | ||
+ | //Astron. Astrophys.// | ||
+ | The authors detect DCNO about a factor of 25 lower in abundance that the main isotopolog.\\ | ||
\\ | \\ | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | The transitions detected were the // | + | The transitions detected were the // |
+ | \\ | ||
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:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | 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 // | + | 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 // |
+ | \\ | ||
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:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | 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): | + | Contributor(s): |
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