molecules:ism:vyoh

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molecules:ism:vyoh [2022/08/04 11:35] – muellermolecules:ism:vyoh [2022/08/04 12:45] (current) – mueller
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 Several //b//-type transitions //J//+1<sub>1,//J//+1</sub> – //J//<sub>0,//J//</sub> between 71 and 155 GHz were searched for with the Kitt Peak 12 m telescope toward the famous massive star-forming region Sagittarius B2(N) near the Galactic Center. Transitions with //J// = 0 to 4 have been detected for the energetically higher lying //anti//-conformer, whereas only //J// = 1 and 2 were found for the //syn//-conformer because of the less favorable dipole moment component.\\ Several //b//-type transitions //J//+1<sub>1,//J//+1</sub> – //J//<sub>0,//J//</sub> between 71 and 155 GHz were searched for with the Kitt Peak 12 m telescope toward the famous massive star-forming region Sagittarius B2(N) near the Galactic Center. Transitions with //J// = 0 to 4 have been detected for the energetically higher lying //anti//-conformer, whereas only //J// = 1 and 2 were found for the //syn//-conformer because of the less favorable dipole moment component.\\
 The low rotational temperature of 11.6 K (with a possible range from 6.9 to 25.1 K because of uncertainty) together with the large beam sizes of the telecope point to an occurance in cold and less dense regions of the source which are known to be far away from local thermodynamic equilibrium.\\ The low rotational temperature of 11.6 K (with a possible range from 6.9 to 25.1 K because of uncertainty) together with the large beam sizes of the telecope point to an occurance in cold and less dense regions of the source which are known to be far away from local thermodynamic equilibrium.\\
-There are very many lines of similar or larger intensity even in the proximity of the observed lines. Therefore, the number of transitions appears to be somewhat small to view the detection as fully secure, even more so as several transitions are (at least) partially blended. Moreover, the derived column density has been found to be basically identical to that of ethanal, which appears to be rather peculiar, though is maybe not impossible. All in all, it is recommended **to view the detection with some caution**.\\+There are very many lines of similar or larger intensity even in the proximity of the observed lines. Therefore, the number of transitions appears to be somewhat small to view the detection as fully secure, even more so as several transitions are (at least) partially blended. Moreover, the derived column density has been found to be basically identical to that of ethanal, which appears to be rather peculiar, though is maybe not impossible. All in all, it is recommended **to view this report with some caution**.\\
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 **[[https://doi.org/10.1051/0004-6361/202142699|Precursors of Fatty Alcohols in the ISM: Discovery of //n//-Propanol]]**\\ **[[https://doi.org/10.1051/0004-6361/202142699|Precursors of Fatty Alcohols in the ISM: Discovery of //n//-Propanol]]**\\
 //Astron. Astrophys.// **663** (2022), Art. No. A181.\\ //Astron. Astrophys.// **663** (2022), Art. No. A181.\\
 +Using data from line surveys  of the quiescent giant molecular cloud G+0.693−0.027, about 1' north-east of Sagittarius (Sgr) B2(N) carried out with the Yebes 40 m dish at 7 mm and with the IRAM 30 m dish at 3, 2, and 1 mm, the authors also identified //syn//- and //anti//-ethenol in a column density ratio of about 10 : 1. Interestingly, ethanol and ethanal are only about a factor of 5 and 4, respectively, more abundant than ethenol.\\
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