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| molecules:ism:glycolaldehyd [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:glycolaldehyd [2019/10/24 09:40] – mueller |
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| There had been two initial reports in the literature on the detection of hydroxyethanal, aka glycolaldehyde, in Sgr B2(N):\\ | There had been two initial reports in the literature on the detection of hydroxyethanal, aka glycolaldehyde, in Sgr B2(N):\\ |
| J. M. Hollis, F. J. Lovas, and P. R. Jewell,\\ | J. M. Hollis, F. J. Lovas, and P. R. Jewell,\\ |
| **[[http://dx.doi.org/10.1086/312881|Interstellar Glycolaldehyde: The First Sugar]]**\\ | **[[https://doi.org/10.1086/312881|Interstellar Glycolaldehyde: The First Sugar]]**\\ |
| //Astrophys. J.// **540**, L107–L110 (2000); and\\ | //Astrophys. J.// **540**, L107–L110 (2000); and\\ |
| J. M. Hollis, S. N. Vogel, L. E. Snyder, P. R. Jewell, and F. J. Lovas,\\ | J. M. Hollis, S. N. Vogel, L. E. Snyder, P. R. Jewell, and F. J. Lovas,\\ |
| **[[http://dx.doi.org/10.1086/320930|The Spatial Scale of Glycolaldehyde in the Galactic Center]]**\\ | **[[https://doi.org/10.1086/320930|The Spatial Scale of Glycolaldehyde in the Galactic Center]]**\\ |
| //Astrophys. J.// **554**, L81–L85 (2001).\\ | //Astrophys. J.// **554**, L81–L85 (2001).\\ |
| 6 //b//-type rotational transitions in the 70 to 105 GHz region were searched for with the NRAO 12 m radio telescope in the former work. Two transitions were severely blended, the remaining four appeared to be free of contamination. No rotational temeperature was derived, but 200 K were assumed. Because of the small number of lines and possible line overlap this detection had to be viewed with some caution until further observations.\\ | 6 //b//-type rotational transitions in the 70 to 105 GHz region were searched for with the NRAO 12 m radio telescope in the former work. Two transitions were severely blended, the remaining four appeared to be free of contamination. No rotational temeperature was derived, but 200 K were assumed. Because of the small number of lines and possible line overlap this detection had to be viewed with some caution until further observations.\\ |
| Recent observations of the four lowest //<sup>r</sup>Q//<sub>0</sub> transitions in the microwave region toward Sgr B2(N) secure the glycolaldehyde detection:\\ | Recent observations of the four lowest //<sup>r</sup>Q//<sub>0</sub> transitions in the microwave region toward Sgr B2(N) secure the glycolaldehyde detection:\\ |
| J. M. Hollis, P. R. Jewell, F. J. Lovas, and A. Remijan,\\ | J. M. Hollis, P. R. Jewell, F. J. Lovas, and A. Remijan,\\ |
| **[[http://dx.doi.org/10.1086/424927|Green Bank Telescope Observations of Interstellar Glycolaldehyde: Low-Temperature Sugar]]**\\ | **[[https://doi.org/10.1086/424927|Green Bank Telescope Observations of Interstellar Glycolaldehyde: Low-Temperature Sugar]]**\\ |
| //Astrophys. J.// **613**, L45–L48 (2004).\\ | //Astrophys. J.// **613**, L45–L48 (2004).\\ |
| Interestingly, these transitions point at temperatures of around 8 K, whereas a reanalysis of the millimeter wave transitions, observed by the same group and mentioned above, were reinterpreted in terms of a temperature of about 50 K. | Interestingly, these transitions point at temperatures of around 8 K, whereas a reanalysis of the millimeter wave transitions, observed by the same group and mentioned above, were reinterpreted in terms of a temperature of about 50 K. |
| The observations from the Ziurys group have appeared eventually:\\ | The observations from the Ziurys group have appeared eventually:\\ |
| D. T. Halfen, A. J. Apponi, N. Woolf, R. Polt, and L. M. Ziurys,\\ | D. T. Halfen, A. J. Apponi, N. Woolf, R. Polt, and L. M. Ziurys,\\ |
| **[[http://dx.doi.org/10.1086/499225|A Systematic Study of Glycolaldehyde in Sagittarius B2(N) at 2 and 3 mm:\\ | **[[https://doi.org/10.1086/499225|A Systematic Study of Glycolaldehyde in Sagittarius B2(N) at 2 and 3 mm:\\ |
| Criteria for Detecting Large Interstellar Molecules]]**\\ | Criteria for Detecting Large Interstellar Molecules]]**\\ |
| //Astrophys. J.// **639**, 237–245 (2006).\\ | //Astrophys. J.// **639**, 237–245 (2006).\\ |
| The molecule was also detected in three Galactic center molecular clouds which have low dust temperatures (10–20 K), even lower rotational temperatures (around 10 K), which are moderately dense (a few tenthousand molecules per cubic centimeter), but which are kinetically moderately warm (about 100 K or more). Three or four transitions were detected with the 100 m GBT telescope between 13 and 23 GHz by\\ | The molecule was also detected in three Galactic center molecular clouds which have low dust temperatures (10–20 K), even lower rotational temperatures (around 10 K), which are moderately dense (a few tenthousand molecules per cubic centimeter), but which are kinetically moderately warm (about 100 K or more). Three or four transitions were detected with the 100 m GBT telescope between 13 and 23 GHz by\\ |
| M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris,\\ | M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris,\\ |
| **[[http://dx.doi.org/10.1086/523627|The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository]]**\\ | **[[https://doi.org/10.1086/523627|The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository]]**\\ |
| //Astrophys. J.// **672**, 352–360 (2008). | //Astrophys. J.// **672**, 352–360 (2008). |
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| A report on the\\ | A report on the\\ |
| **[[http://dx.doi.org/10.1088/0004-637X/690/2/L93|First Detection of Glycolaldehyde Outside the Galactic Center]]**\\ | **[[https://doi.org/10.1088/0004-637X/690/2/L93|First Detection of Glycolaldehyde Outside the Galactic Center]]**\\ |
| by M. T. Beltrán, C. Codella, S. Viti, R. Neri, and R. Cesaroni,\\ | by M. T. Beltrán, C. Codella, S. Viti, R. Neri, and R. Cesaroni,\\ |
| //Astrophys. J.// **690**, L93–L96 (2009),\\ | //Astrophys. J.// **690**, L93–L96 (2009),\\ |
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| The situation is more favorable in\\ | The situation is more favorable in\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/757/1/L4|Detection of the Simplest Sugar, Glycolaldehyde, in a Solar-type Protostar with ALMA]]**\\ | **[[https://doi.org/10.1088/2041-8205/757/1/L4|Detection of the Simplest Sugar, Glycolaldehyde, in a Solar-type Protostar with ALMA]]**\\ |
| by J. K. Jørgensen, C. Favre, S. E. Bisschop, T. L. Bourke, E. F. van Dishoeck, and Markus Schmalzl,\\ | by J. K. Jørgensen, C. Favre, S. E. Bisschop, T. L. Bourke, E. F. van Dishoeck, and Markus Schmalzl,\\ |
| //Astrophys. J.// **757**, Art. No. L4 (2012).\\ | //Astrophys. J.// **757**, Art. No. L4 (2012).\\ |
| J. K. Jørgensen, M. H. D. van der Wiel, A. Coutens, J. M. Lykke, H. S. P. Müller, E. F. van Dishoeck, H. Calcutt, P. Bjerkeli, T. L. Bourke, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, K. I. Öberg, M. V. Persson, and S. F. Wampfler\\ | J. K. Jørgensen, M. H. D. van der Wiel, A. Coutens, J. M. Lykke, H. S. P. Müller, E. F. van Dishoeck, H. Calcutt, P. Bjerkeli, T. L. Bourke, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, K. I. Öberg, M. V. Persson, and S. F. Wampfler\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201628648|The ALMA Protostellar Interferometric Line Survey (PILS): First Results from an Unbiased Submillimeter Wavelength Line Survey of the Class 0 Protostellar Binary IRAS 16293–2422 with ALMA]]**,\\ | **[[https://doi.org/10.1051/0004-6361/201628648|The ALMA Protostellar Interferometric Line Survey (PILS): First Results from an Unbiased Submillimeter Wavelength Line Survey of the Class 0 Protostellar Binary IRAS 16293–2422 with ALMA]]**,\\ |
| //Astron. Astrophys.// **595**, Art. No. A117 (2016).\\ | //Astron. Astrophys.// **595**, Art. No. A117 (2016).\\ |
| Emission of deuterated isotopologs was detected as well as that of <sup>13</sup>C species. The D to H ratio was about 0.05 per H atom, irrespective of the functional group. The <sup>12</sup>C to <sup>13</sup>C ratio was about 30 for each C atom, lower than the canonical value of 67 expected for the local ISM. | Emission of deuterated isotopologs was detected as well as that of <sup>13</sup>C species. The D to H ratio was about 0.05 per H atom, irrespective of the functional group. The <sup>12</sup>C to <sup>13</sup>C ratio was about 30 for each C atom, lower than the canonical value of 67 expected for the local ISM. |
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| Contributor(s): H. S. P. Müller; 09, 2003; 09, 2004; 02, 2006; 04, 2012; 07, 2012; 09, 2012; 11, 2016 | Contributor(s): H. S. P. Müller; 09, 2003; 09, 2004; 02, 2006; 04, 2012; 07, 2012; 09, 2012; 11, 2016 |
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