molecules:ism:formamid

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molecules:ism:formamid [2019/05/09 12:38] – muellermolecules:ism:formamid [2019/10/23 22:03] (current) – mueller
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 Formamide, HC(O)NH<sub>2</sub>, is a fairly typical hot core molecule that is quite abundant. The first transition of this molecule was detected toward Sgr B2 and likely toward Sgr A by\\ Formamide, HC(O)NH<sub>2</sub>, is a fairly typical hot core molecule that is quite abundant. The first transition of this molecule was detected toward Sgr B2 and likely toward Sgr A by\\
 R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\ R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\
-**[[http://cdsads.u-strasbg.fr/abs/1971ApJ...169L..39R|Microwave Detection of Interstellar Formamide]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1971ApJ...169L..39R|Microwave Detection of Interstellar Formamide]]**\\
 //Astrophys. J.// **169**, L39–L43 (1971).\\ //Astrophys. J.// **169**, L39–L43 (1971).\\
 They detected all three Δ//F// = 0 hyperfine components of the //K<sub>a</sub>// = 1, //J// =  2 – 2 transition near 4619 MHz. Only the strongest component, overlapped in part with the H112α transition, was tentatively detected toward Sgr A.\\ They detected all three Δ//F// = 0 hyperfine components of the //K<sub>a</sub>// = 1, //J// =  2 – 2 transition near 4619 MHz. Only the strongest component, overlapped in part with the H112α transition, was tentatively detected toward Sgr A.\\
 The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\ The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\
 C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\ C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\
-**[[http://cdsads.u-strasbg.fr/abs/1973ApJ...182..699G|Studies of Interstellar Formamide]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1973ApJ...182..699G|Studies of Interstellar Formamide]]**\\
 //Astrophys. J.// **182**, 699–710 (1973). //Astrophys. J.// **182**, 699–710 (1973).
  
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 //Astron. Astrophys.// **590**, Art. No. L6 (2016).\\ //Astron. Astrophys.// **590**, Art. No. L6 (2016).\\
 Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a <sup>12</sup>C/<sup>13</sup>C ratio of 68 because lines of the main isotopolog are frequently affected by optical depth effects. Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a <sup>12</sup>C/<sup>13</sup>C ratio of 68 because lines of the main isotopolog are frequently affected by optical depth effects.
 +
 +A. Belloche, R. T. Garrod, H. S. P. Müller, K. M. Menten, I. Medvedev, J. Thomas, and Z. Kisiel\\
 +reported on\\
 +**[[https://doi.org/10.1051/0004-6361/201935428|Re-exploring Molecular Complexity with ALMA (ReMoCA): Interstellar Detection of Urea]]**\\
 +//Astron. Astrophys.// **628**, Art. No. A10 (2019).\\
 +In the course of a new unbiased line survey toward the high-mass star-forming region Sagittarius (Sgr) B2(N) close to the Galactic center, HC(<sup>18</sup>O)NH<sub>2</sub> and HC(O)<sup>15</sup>NH<sub>2</sub> were detected. The <sup>16</sup>O/<sup>18</sup>O ratio of 140 is in the range of values found in the Galactic center, the <sup>14</sup>N/<sup>15</sup>N ratio is about 300.
  
 The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, G34_3+0.15, and NGC 6334(I). The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, G34_3+0.15, and NGC 6334(I).
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 Contributor(s): H. S. P. Müller; 05, 2009; 08, 2012; 02, 2013; 06, 2016; 10, 2017; 01, 2019 Contributor(s): H. S. P. Müller; 05, 2009; 08, 2012; 02, 2013; 06, 2016; 10, 2017; 01, 2019
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