molecules:ism:formamid

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molecules:ism:formamid [2019/03/14 15:57] – 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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 A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, N. F. W. Ligterink, K. I. Öberg, M. V. Persson, E. F. van Dishoeck, and S. F. Wampfler\\ A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, N. F. W. Ligterink, K. I. Öberg, M. V. Persson, E. F. van Dishoeck, and S. F. Wampfler\\
 reported on\\ reported on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201628612|The ALMA-PILS Survey: First Detections of Deuterated Formamide and Deuterated Isocyanic Acid in the Interstellar Medium]]**\\+**[[https://doi.org/10.1051/0004-6361/201628612|The ALMA-PILS Survey: First Detections of Deuterated Formamide and Deuterated Isocyanic Acid in the Interstellar Medium]]**\\
 //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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 C. Kahane, C. Ceccarelli, A. Faure, and E. Caux\\ C. Kahane, C. Ceccarelli, A. Faure, and E. Caux\\
 gave an account on the\\ gave an account on the\\
-**[[http://dx.doi.org/10.1088/2041-8205/763/2/L38|Detection of Formamide, the Simplest but Crucial Amide, in a Solar-type Protostar]]**\\+**[[https://doi.org/10.1088/2041-8205/763/2/L38|Detection of Formamide, the Simplest but Crucial Amide, in a Solar-type Protostar]]**\\
 //Astrophys. J.// **763**, Art. No. L38 (2013).\\ //Astrophys. J.// **763**, Art. No. L38 (2013).\\
 The protostar is the usual suspect, IRAS 16293–2422. The protostar is the usual suspect, IRAS 16293–2422.
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 V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\ V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\
 reported on\\ reported on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201731495|Complex Organic Molecules in Diffuse Clouds along the Line of Sight to Sgr B2]]**\\+**[[https://doi.org/10.1051/0004-6361/201731495|Complex Organic Molecules in Diffuse Clouds along the Line of Sight to Sgr B2]]**\\
 //Astron. Astrophys.// **605** (2017), Art. No. L6.\\ //Astron. Astrophys.// **605** (2017), Art. No. L6.\\
 Four low-//J// //a//-type transitions of formamide were detected with ALMA between 84.5 and 105.5 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\ Four low-//J// //a//-type transitions of formamide were detected with ALMA between 84.5 and 105.5 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\
 V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\ V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\
 continued their investigation of\\ continued their investigation of\\
-**[[http://dx.doi.org/10.1051/0004-6361/201834467|Small-scale Physical and Chemical Structure of Diffuse and Translucent Molecular Clouds along the Line of Sight to Sgr B2]]**\\+**[[https://doi.org/10.1051/0004-6361/201834467|Small-scale Physical and Chemical Structure of Diffuse and Translucent Molecular Clouds along the Line of Sight to Sgr B2]]**\\
 //Astron. Astrophys.// **623** Art. No. A68 (2019).\\ //Astron. Astrophys.// **623** Art. No. A68 (2019).\\
 Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds. Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds.
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 R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\ R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\
 described the\\ described the\\
-**[[http://dx.doi.org/10.1051/0004-6361/201220033|Rotational Spectrum of Formamide up to 1 THz and First ISM Detection of its //v//<sub>12</sub> Vibrational State]]**\\+**[[https://doi.org/10.1051/0004-6361/201220033|Rotational Spectrum of Formamide up to 1 THz and First ISM Detection of its //v//<sub>12</sub> Vibrational State]]**\\
 //Astron. Astrophys.// **548**, Art. No. A71 (2012). //Astron. Astrophys.// **548**, Art. No. A71 (2012).
  
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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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