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molecules:ism:glycol [2019/02/25 22:38] – external edit 127.0.0.1 | molecules: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/ | + | **[[https:// |
// | // | ||
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 ?]]**,\\ | + | **{{ : |
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), | The molecule was also detected in three Galactic center molecular clouds which have low dust temperatures (10–20 K), | ||
M. A. Requena-Torres, | M. A. Requena-Torres, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
The column density relative to methanol is reasonable. Considering also the low rotational temperature, | The column density relative to methanol is reasonable. Considering also the low rotational temperature, | ||
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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/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
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/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
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, | N. Brouillet, D. Despois, X.-H. Lu, A. Baudry, J. Cernicharo, D. Bockelée-Morvan, | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
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, | 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, | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
The authors detect ethanediol unambiguously in this source and the higher energy // | The authors detect ethanediol unambiguously in this source and the higher energy // | ||
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Contributor(s): | Contributor(s): | ||
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