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| //Astrophys. J.// **197**, L29–L31 (1975).\\ | //Astrophys. J.// **197**, L29–L31 (1975).\\ |
| The //A// component of the 1<sub>10</sub> – 1<sub>11</sub> near 1610 GHz was clearly seen with the Parkes 64 m telescope, and there was evidence for the //E// component close by.\\ | The //A// component of the 1<sub>10</sub> – 1<sub>11</sub> near 1610 GHz was clearly seen with the Parkes 64 m telescope, and there was evidence for the //E// component close by.\\ |
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| **[[https://doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\ | **[[https://doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\ |
| //Astrophys. J.// **593**, L51–L55 (2003).\\ | //Astrophys. J.// **593**, L51–L55 (2003).\\ |
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| //Astrophys. J.// **657**, L17–L19 (2007).\\ | //Astrophys. J.// **657**, L17–L19 (2007).\\ |
| 20 U-lines from four different line surveys in the frequency range 97 to 160 GHz were assigned.\\ | 20 U-lines from four different line surveys in the frequency range 97 to 160 GHz were assigned.\\ |
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| **[[https://doi.org/10.1051/0004-6361/200811456|Rotational Spectrum of <sup>13</sup>C<sub>2</sub>-Methyl Formate (HCOO<sup>13</sup>CH<sub>3</sub>) and Detection of the Two <sup>13</sup>C-Methyl Formate in Orion]]**\\ | **[[https://doi.org/10.1051/0004-6361/200811456|Rotational Spectrum of <sup>13</sup>C<sub>2</sub>-Methyl Formate (HCOO<sup>13</sup>CH<sub>3</sub>) and Detection of the Two <sup>13</sup>C-Methyl Formate in Orion]]**\\ |
| //Astron. Astrophys.// **500**, 1109–1118 (2009).\\ | //Astron. Astrophys.// **500**, 1109–1118 (2009).\\ |
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| //Astrophys. J.// **714**, 1120–1132 (2010).\\ | //Astrophys. J.// **714**, 1120–1132 (2010).\\ |
| Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used to search for the acid-deuterated isotopolog. The tentative D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual.\\ | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used to search for the acid-deuterated isotopolog. The tentative D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual.\\ |
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| //Astron. Astrophys.// **517**, Art. No. A17 (2010).\\ | //Astron. Astrophys.// **517**, Art. No. A17 (2010).\\ |
| The degree of deuteration is similar in both sub-sources A and B, about 0.06.\\ | The degree of deuteration is similar in both sub-sources A and B, about 0.06.\\ |
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| //Astron. Astrophys.// **538**, Art. No. A119 (2012).\\ | //Astron. Astrophys.// **538**, Art. No. A119 (2012).\\ |
| Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the <sup>18</sup>O isotopomers. The <sup>13</sup>C to <sup>18</sup>O of about 13 is rather reasonable. The <sup>12</sup>C to <sup>13</sup>C and <sup>16</sup>O to <sup>18</sup>O appear to be too small by a factor of about two, likely because of neglect of opacity.\\ | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the <sup>18</sup>O isotopomers. The <sup>13</sup>C to <sup>18</sup>O of about 13 is rather reasonable. The <sup>12</sup>C to <sup>13</sup>C and <sup>16</sup>O to <sup>18</sup>O appear to be too small by a factor of about two, likely because of neglect of opacity.\\ |
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| //Astrophys. J.// **779**, Art. No. 119 (2013).\\ | //Astrophys. J.// **779**, Art. No. 119 (2013).\\ |
| Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used once more to search for the methyl-deuterated isotopolog. The D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual, but is three times lower per H atom than the tentatively derived value for the acid-deuterated isotopolog.\\ | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used once more to search for the methyl-deuterated isotopolog. The D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual, but is three times lower per H atom than the tentatively derived value for the acid-deuterated isotopolog.\\ |
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| //Astrophys. J.// **755**, Art. No. 153 (2012).\\ | //Astrophys. J.// **755**, Art. No. 153 (2012).\\ |
| The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with //J"// = 0 to 2 were detected for both //A// and //E// internal rotation components. In addition, one //K// = 1 was detected for the //A// component. Two additional //K// = 1 transitions each were barely recognizable in the noise, the intensities being compatible with the model. The detection is probably not far from a definitive one.\\ | The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with //J"// = 0 to 2 were detected for both //A// and //E// internal rotation components. In addition, one //K// = 1 was detected for the //A// component. Two additional //K// = 1 transitions each were barely recognizable in the noise, the intensities being compatible with the model. The detection is probably not far from a definitive one.\\ |
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| | M. Sanz-Novo, G. Molpeceres, V. M. Rivilla, and I. Jimenez-Serra\\ |
| | reinvestigated the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202554686|Conformational Isomerism of Methyl Formate: New Detections of the Higher-energy //trans// Conformer and Theoretical Insights]]**\\ |
| | //Astron. Astrophys.// **698**, Art. No. A36 (2025).\\ |
| | The conformer was identified in G+0.693−0.027, close to the Galactic center, and in L1157−B1. Both are cold and shocked sources, the latter one is considered to be a prototypical shock region. The //syn// to //anti// ("//cis//" to "//trans//") ratios are about 72 and 34, respectively, about factors of 7 and 3 higher than in the Sagittarius B2(N) envelope mentioned above.\\ |
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| Contributor(s): H. S. P. Müller; 02, 2007; 04, 2011; 07, 2012; 08, 2012; 11, 2016; 03, 2019 | Contributor(s): H. S. P. Müller; 02, 2007; 04, 2011; 07, 2012; 08, 2012; 11, 2016; 03, 2019; 07, 2025 |
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