molecules:ism:glycol

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molecules:ism:glycol [2019/04/24 16:22] – muellermolecules:ism:glycol [2019/10/24 09:53] (current) – mueller
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 There is a report in the literature on detection of ethanediol, aka ethylene glycol, or briefly glycol, in Sgr B2(N-LMH):\\ There is a report in the literature on detection of ethanediol, aka ethylene glycol, or briefly glycol, in Sgr B2(N-LMH):\\
 J. M. Hollis, F. J. Lovas, P. R. Jewell, and L. H. Coudert,\\ J. M. Hollis, F. J. Lovas, P. R. Jewell, and L. H. Coudert,\\
-**[[http://dx.doi.org/10.1086/341148|Interstellar Antifreeze: Ethylene Glycol]]**\\+**[[https://doi.org/10.1086/341148|Interstellar Antifreeze: Ethylene Glycol]]**\\
 //Astrophys. J.// **571**, L59–L62 (2002).\\ //Astrophys. J.// **571**, L59–L62 (2002).\\
 Because of the small number of lines and possible line overlap the detection should be viewed with some caution by itself. Because of the small number of lines and possible line overlap the detection should be viewed with some caution by itself.
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 More recently, two transition with complex velocity components have been detected in the centimeter range toward Sgr B2(N-LMH) employing the GBT:\\ More recently, two transition with complex velocity components have been detected in the centimeter range toward Sgr B2(N-LMH) employing the GBT:\\
 J. M. Hollis,\\ J. M. Hollis,\\
-**[[hollis_asilomar.pdf|Complex Molecules and the GBT: Is Isomerism the Key ?]]**,\\+**{{ :pdfs:hollis_asilomar.pdf |Complex Molecules and the GBT: Is Isomerism the Key ?}}**, 
 Contribution at the IAU Symposium 231, Astrochemistry throughout the Universe, Asilomar, CA.\\ Contribution at the IAU Symposium 231, Astrochemistry throughout the Universe, Asilomar, CA.\\
 While it is hard to say that the detection is beyond doubt, these two lines render the detection quite secure – mainly because the line density at these lower frequencies is fairly small. While it is hard to say that the detection is beyond doubt, these two lines render the detection quite secure – mainly because the line density at these lower frequencies is fairly small.
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 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). Two 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). Two 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).\\
 The column density relative to methanol is reasonable. Considering also the low rotational temperature, the detection is probably fairly secure even though only two transitions were detected. The column density relative to methanol is reasonable. Considering also the low rotational temperature, the detection is probably fairly secure even though only two transitions were detected.
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 A. J. Maury, A. Belloche, Ph. André, S. Maret, F. Gueth, C. Codella, S. Cabrit, L. Testi, and S. Bontemps\\ A. J. Maury, A. Belloche, Ph. André, S. Maret, F. Gueth, C. Codella, S. Cabrit, L. Testi, and S. Bontemps\\
 reported on\\ reported on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201323033|First results from the CALYPSO IRAM-PdBI survey. II. Resolving the hot corino in the Class 0 protostar NGC 1333-IRAS2A]]**\\+**[[https://doi.org/10.1051/0004-6361/201323033|First results from the CALYPSO IRAM-PdBI survey. II. Resolving the hot corino in the Class 0 protostar NGC 1333-IRAS2A]]**\\
 //Astron. Astrophys.// **563**, L2 (2014).\\ //Astron. Astrophys.// **563**, L2 (2014).\\
 Ethanediol was among the molecules identified unambiguously in several transitions between 216.8 and 220.5 GHz. Ethanediol was among the molecules identified unambiguously in several transitions between 216.8 and 220.5 GHz.
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 A. Fuente, J. Cernicharo, P. Caselli, C. McCoey, D. Johnstone, M. Fich, T. van Kempen, Aina Palau, U.A. Yildiz, B. Tercero, and A. López\\ A. Fuente, J. Cernicharo, P. Caselli, C. McCoey, D. Johnstone, M. Fich, T. van Kempen, Aina Palau, U.A. Yildiz, B. Tercero, and A. López\\
 reported on\\ reported on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201323074|The hot core towards the intermediate mass protostar NGC7129 FIRS 2: Chemical similarities with Orion KL]]**\\+**[[https://doi.org/10.1051/0004-6361/201323074|The hot core towards the intermediate mass protostar NGC7129 FIRS 2: Chemical similarities with Orion KL]]**\\
 //Astron. Astrophys.// **568**, A65 (2014).\\ //Astron. Astrophys.// **568**, A65 (2014).\\
 Several transitions of ethanediol were detected in a line survey with PdBI covering 218.2 to 221.8 GHz. Several transitions of ethanediol were detected in a line survey with PdBI covering 218.2 to 221.8 GHz.
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 N. Brouillet, D. Despois, X.-H. Lu, A. Baudry, J. Cernicharo, D. Bockelée-Morvan, J. Crovisier, and N. Biver\\ N. Brouillet, D. Despois, X.-H. Lu, A. Baudry, J. Cernicharo, D. Bockelée-Morvan, J. Crovisier, and N. Biver\\
 reported on\\ reported on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201424588|Antifreeze in the hot core of Orion – First detection of ethylene glycol in Orion-KL]]**\\+**[[https://doi.org/10.1051/0004-6361/201424588|Antifreeze in the hot core of Orion – First detection of ethylene glycol in Orion-KL]]**\\
 //Astron. Astrophys.// **576**, A129 (2015).\\ //Astron. Astrophys.// **576**, A129 (2015).\\
 A large number of unblended or slightly blended transitions of ethanediol were detected in an ALMA-SV line survey coverning 213.715 to 246.627 GHz. A large number of unblended or slightly blended transitions of ethanediol were detected in an ALMA-SV line survey coverning 213.715 to 246.627 GHz.
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 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).\\
 The authors detect ethanediol unambiguously in this source and the higher energy //gGg'// conformer for the first time unambiguously in the ISM. There were tentative reports in both instances. The authors detect ethanediol unambiguously in this source and the higher energy //gGg'// conformer for the first time unambiguously in the ISM. There were tentative reports in both instances.
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 Contributor(s): H. S. P. Müller; 12, 2005; 07, 2012; 04, 2015; 11, 2016 Contributor(s): H. S. P. Müller; 12, 2005; 07, 2012; 04, 2015; 11, 2016
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