molecules:ism:mecho

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molecules:ism:mecho [2023/03/06 12:48] – muellermolecules:ism:mecho [2023/03/06 13:09] (current) – mueller
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 **Detection of Acetaldehyde in Sagittarius**\\ **Detection of Acetaldehyde in Sagittarius**\\
 //Molecules in the Galactic Environment// eds. M. A. Gordon and L. E. Snyder, Wiley-Interscience, New York, 181–186 (1973).\\ //Molecules in the Galactic Environment// eds. M. A. Gordon and L. E. Snyder, Wiley-Interscience, New York, 181–186 (1973).\\
-The //a//-type //Q//-branch transition 1<sub>10</sub> – 1<sub>11</sub> near 1065 MHz was detected toward Sagittarius A and Sgr B2.+The //a//-type //Q//-branch transition 1<sub>10</sub> – 1<sub>11</sub> near 1065 MHz was detected toward Sagittarius A and Sgr B2.\\ 
 +\\
  
 Soon thereafter, the observation of the 2<sub>11</sub> – 2<sub>12</sub> transition near 3195 MHz toward Sgr B2 with the Parkes 64 m telescope was reported:\\ Soon thereafter, the observation of the 2<sub>11</sub> – 2<sub>12</sub> transition near 3195 MHz toward Sgr B2 with the Parkes 64 m telescope was reported:\\
 N. Fourikis, M. W. Sinclair, B. J. Robinson, P. D. Godfrey, and R. D. Brown,\\ N. Fourikis, M. W. Sinclair, B. J. Robinson, P. D. Godfrey, and R. D. Brown,\\
 **[[https://ui.adsabs.harvard.edu/abs/1974AuJPh..27..425F|Microwave Emission of the 2<sub>11</sub> → 2<sub>12</sub> Rotational Transition in Interstellar Acetaldehyde]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1974AuJPh..27..425F|Microwave Emission of the 2<sub>11</sub> → 2<sub>12</sub> Rotational Transition in Interstellar Acetaldehyde]]**\\
-//Aust. J. Phys.// **27**, 425–430 (1974).+//Aust. J. Phys.// **27**, 425–430 (1974).\\ 
 +\\
  
 Many more transitions were detected toward hot cores such as Sgr B2 or OMC-1. However, the rotational temperatures were usually quite low (50 K or even considerably lower) and suggest an extended distribution. A fairly recent mapping of the 1<sub>10</sub> – 1<sub>11</sub> transition toward Sgr B2 with the GRMT demonstrates this rather nicely:\\ Many more transitions were detected toward hot cores such as Sgr B2 or OMC-1. However, the rotational temperatures were usually quite low (50 K or even considerably lower) and suggest an extended distribution. A fairly recent mapping of the 1<sub>10</sub> – 1<sub>11</sub> transition toward Sgr B2 with the GRMT demonstrates this rather nicely:\\
 J. N. Chengalur and N. Kanekar,\\ J. N. Chengalur and N. Kanekar,\\
 **[[https://doi.org/10.1051/0004-6361:20030577|Widespread Acetaldehyde near the Galactic Centre]]**\\ **[[https://doi.org/10.1051/0004-6361:20030577|Widespread Acetaldehyde near the Galactic Centre]]**\\
-//Astron. Astrophys.// **403**, L43–L46 (2003).+//Astron. Astrophys.// **403**, L43–L46 (2003).\\ 
 +\\
  
 Ethanal has also been detected in cold clouds:\\ Ethanal has also been detected in cold clouds:\\
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 **[[https://doi.org/10.1086/163018|The Detection of Acetaldehyde in Cold Dust Clouds]]**\\ **[[https://doi.org/10.1086/163018|The Detection of Acetaldehyde in Cold Dust Clouds]]**\\
 //Astrophys. J.// **290**, 609–614 (1985).\\ //Astrophys. J.// **290**, 609–614 (1985).\\
-Both //A// and //E// internal rotation components of the 1<sub>01</sub> – 0<sub>00</sub> transition near 19264 MHz were detected with the NRAO 140-foot telescope toward TMC-1 and L134N.+Both //A// and //E// internal rotation components of the 1<sub>01</sub> – 0<sub>00</sub> transition near 19264 MHz were detected with the NRAO 140-foot telescope toward TMC-1 and L134N.\\ 
 +\\
  
 It was also found in one of three translucent clouds (CB 17):\\ It was also found in one of three translucent clouds (CB 17):\\
 B. E. Turner, R. Terzieva, and E. Herbst,\\ B. E. Turner, R. Terzieva, and E. Herbst,\\
 **[[https://doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\ **[[https://doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\
-//Astrophys. J.// **518**, 699–732 (1999).+//Astrophys. J.// **518**, 699–732 (1999).\\ 
 +\\
  
 A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\ A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\
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 **[[https://doi.org/10.1051/0004-6361/201731667|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]**\\ **[[https://doi.org/10.1051/0004-6361/201731667|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]**\\
 //Astron. Astrophys.// **620**, Art. No. A170 (2018).\\ //Astron. Astrophys.// **620**, Art. No. A170 (2018).\\
-The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time both <sup>13</sup>C isotopomers as well as the CH<sub>3</sub>CDO species. The D/H ratio per H atom is about 0.08. The <sup>12</sup>C/<sup>13</sup>C ratio is compatible with the local ISM ratio. Ethanal is among the molecules with colder rotational temperatures of around 125 K in that hot corino.+The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time both <sup>13</sup>C isotopomers as well as the CH<sub>3</sub>CDO species. The D/H ratio per H atom is about 0.08. The <sup>12</sup>C/<sup>13</sup>C ratio is compatible with the local ISM ratio. Ethanal is among the molecules with colder rotational temperatures of around 125 K in that hot corino.\\ 
 +\\
  
 L. H. Coudert, L. Margulès, C. Vastel, R. Motiyenko, E. Caux, and J.-C. Guillemin\\ L. H. Coudert, L. Margulès, C. Vastel, R. Motiyenko, E. Caux, and J.-C. Guillemin\\
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 species of acetaldehyde CH<sub>2</sub>DCOH and CH<sub>3</sub>COD]]**\\ species of acetaldehyde CH<sub>2</sub>DCOH and CH<sub>3</sub>COD]]**\\
 //Astron. Astrophys.// **624**, Art. No. A70 (2019).\\ //Astron. Astrophys.// **624**, Art. No. A70 (2019).\\
 +The observations are based on PILS.\\
 +\\
 +
 +J. Ferrer Asensio, S. Spezzano, L. H. Coudert, V. Lattanzi, C. P. Endres, J. K. Jørgensen, and P. Caselli\\
 +described the\\
 +**[[https://doi.org/10.1051/0004-6361/202245442|Millimetre and Sub-millimetre Spectroscopy of Doubly Deuterated Acetaldehyde (CHD<sub>2</sub>CHO) and First Detection towards IRAS 16293−2422]]**\\
 +//Astron. Astrophys.// **670**, Art. No. A177 (2023).\\
 +The observations are based on PILS. The authors determine a CHD<sub>2</sub>CHO to CH<sub>2</sub>DCOH ratio of ~0.21. It is also worthwhile to compare the column densities with that of the main isotopic species. This translates to a deueration degree of ~0.017 per H atom for CH<sub>2</sub>DCOH and ~0.060 for CHD<sub>2</sub>CHO. Such enhancement in the degree of deueration in doubly or higher deuterated isotopologs compared with sinly deuterated variants has been found commonly.\\
 \\ \\
  
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-Contributor(s): H. S. P. Müller; 11, 2009; 03, 2012; 01, 2014; 10, 2017; 01, 2019; 04, 2019+Contributor(s): H. S. P. Müller; 11, 2009; 03, 2012; 01, 2014; 10, 2017; 01, 2019; 04, 2019; 03, 2023.
  
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