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molecules:ism:mecho [2023/03/06 12:48] – mueller | molecules:ism:mecho [2023/03/06 12:52] – 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.\\ |
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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).\\ |
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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).\\ |
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Ethanal has also been detected in cold clouds:\\ | Ethanal has also been detected in cold clouds:\\ |
**[[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.\\ |
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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).\\ |
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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\\ |
**[[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.\\ |
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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\\ |
//Astron. Astrophys.// **624**, Art. No. A70 (2019).\\ | //Astron. Astrophys.// **624**, Art. No. A70 (2019).\\ |
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| 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 (CHD2CHO) and First Detection towards IRAS 16293−2422]]**\\ |
| //Astron. Astrophys.// **670**, Art. No. A177 (2023).\\ |
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