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molecules:ism:aceton [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:aceton [2019/10/24 09:52] (current) – mueller | ||
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F. Combes, M. Gerin, A. Wooten, G. Wlodarczak, F. Clausset, and P. J. Encrenaz,\\ | F. Combes, M. Gerin, A. Wooten, G. Wlodarczak, F. Clausset, and P. J. Encrenaz,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
detected propanone, aka acetone, for the first time in the interstellar medium. Observations were made with the IRAM 30m, Greenbank 43m, and Kitt Peak 12m telescopes toward Sgr B2. The column density of 5 × 10< | detected propanone, aka acetone, for the first time in the interstellar medium. Observations were made with the IRAM 30m, Greenbank 43m, and Kitt Peak 12m telescopes toward Sgr B2. The column density of 5 × 10< | ||
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15 years later, this detection was confirmed: | 15 years later, this detection was confirmed: | ||
L. E. Snyder, F. J. Lovas, D. M. Mehringer, N. Y. Miao, Y.-J. Kuan, J. M. Hollis, and P. R. Jewell,\\ | L. E. Snyder, F. J. Lovas, D. M. Mehringer, N. Y. Miao, Y.-J. Kuan, J. M. Hollis, and P. R. Jewell,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
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More recently, propanone was detected towards the high-mass star-forming region Orion KL: | More recently, propanone was detected towards the high-mass star-forming region Orion KL: | ||
D. N. Friedel, L. E. Snyder, A. J. Remijan, and B. E. Turner,\\ | D. N. Friedel, L. E. Snyder, A. J. Remijan, and B. E. Turner,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
Besides a very large number of transitions in its ground vibrational state, a few lines of the first excited torsional state were reported. Even though the number of vibrationally excited lines is small, the consistent global modeling ensures this aspect of the detection. | Besides a very large number of transitions in its ground vibrational state, a few lines of the first excited torsional state were reported. Even though the number of vibrationally excited lines is small, the consistent global modeling ensures this aspect of the detection. | ||
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J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
This report is the first one on the detection of acetone around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 186 lines were assigned to acetone. | This report is the first one on the detection of acetone around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 186 lines were assigned to acetone. | ||
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Contributor(s): | Contributor(s): | ||
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