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| molecules:ism:prcn [2019/04/24 12:25] – [On the Detection of n-Propyl Cyanide in Space] mueller | molecules:ism:prcn [2022/06/28 16:54] (current) – [On the Detection of n-Propyl Cyanide in Space] mueller |
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| **[[https://doi.org/10.1051/0004-6361/200811550|Increased Complexity in Interstellar Chemistry: Detection and Chemical Modeling of Ethyl Formate and //n//-Propyl Cyanide in Sagittarius B2(N)]]**\\ | **[[https://doi.org/10.1051/0004-6361/200811550|Increased Complexity in Interstellar Chemistry: Detection and Chemical Modeling of Ethyl Formate and //n//-Propyl Cyanide in Sagittarius B2(N)]]**\\ |
| //Astron. Astrophys.// **499**, (2009) 215–232.\\ | //Astron. Astrophys.// **499**, (2009) 215–232.\\ |
| See also the [[http://www.mpifr-bonn.mpg.de/pressreleases/2009/3|MPIfR press release]] (in English; German version also available).\\ | See also the **[[https://www.mpifr-bonn.mpg.de/pressreleases/2009/3|MPIfR press release]]** (in English; **[[https://www.mpifr-bonn.mpg.de/pressemeldungen/2009/3|German version]]** also available).\\ |
| In the group of the complex molecules detected by radio astronomical means, //n//-propyl cyanide, //n//-C<sub>3</sub>H<sub>7</sub>CN, and ethyl formate are among the largest. They have been detected in the famous massive star-forming region Sagittarius B2(N) in the course of a molecular line survey in the 3 mm wavelength domain with additional observations at 2 and 1 mm carried out with the IRAM 30 m radio telescope.\\ | In the group of the complex molecules detected by radio astronomical means, //n//-propyl cyanide, //n//-C<sub>3</sub>H<sub>7</sub>CN, and ethyl formate are among the largest. They have been detected in the famous massive star-forming region Sagittarius B2(N) in the course of a molecular line survey in the 3 mm wavelength domain with additional observations at 2 and 1 mm carried out with the IRAM 30 m radio telescope.\\ |
| [[https://cdms.astro.uni-koeln.de/classic/molecules:ism:prcn|Aminoacetonitrile]] was detected earlier in the course of this molecular line survey. At a rotational temperature of about 150 K, very many transitions of //n//-propyl cyanide have non-negligible intensities. However, many of them are blended severely with emissions or absorptions of other molecules. Nevertheless, a considerable number of transitions of the lower energy //anti//-conformer are not or only slightly blended. Its column density is about a factor of 100 lower in Sgr B2(N) than those of methyl and ethyl cyanide. | [[molecules:ism:aan|Aminoacetonitrile]] was detected earlier in the course of this molecular line survey. At a rotational temperature of about 150 K, very many transitions of //n//-propyl cyanide have non-negligible intensities. However, many of them are blended severely with emissions or absorptions of other molecules. Nevertheless, a considerable number of transitions of the lower energy //anti//-conformer are not or only slightly blended. Its column density is about a factor of 100 lower in Sgr B2(N) than those of methyl and ethyl cyanide. |
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| //n//-Propyl cyanide is the third alkyl cyanide to be detected in space after methyl cyanide, [[http://www.astro.uni-koeln.de/site/vorhersagen/molecules/ism/MeCN.html|CH<sub>3</sub>CN]], and ethyl cyanide, [[http://www.astro.uni-koeln.de/site/vorhersagen/molecules/ism/EtCN.html|C<sub>2</sub>H<sub>5</sub>CN]]. | //n//-Propyl cyanide is the third alkyl cyanide to be detected in space after methyl cyanide, **[[molecules:ism:mecn|CH<sub>3</sub>CN]]**, and ethyl cyanide, **[[molecules:ism:etcn|C<sub>2</sub>H<sub>5</sub>CN]]**. |
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| Transitions of the lower energy //g//-//n//-propyl cyanide were detected unambiguously in the course of a line survey of the same region carried out with ALMA which lead to the detection of //i//-propyl cyanide as described in the paragraphs further below.\\ | Transitions of the lower energy //g//-//n//-propyl cyanide were detected unambiguously in the course of a line survey of the same region carried out with ALMA which lead to the detection of //i//-propyl cyanide as described in the paragraphs further below.\\ |
| H. S. P. Müller, A. Walters, N. Wehres, A. Belloche, O. H. Wilkins, D. Liu, R. Vicente, R. T. Garrod, K. M. Menten, F. Lewen, and S. Schlemmer\\ | H. S. P. Müller, A. Walters, N. Wehres, A. Belloche, O. H. Wilkins, D. Liu, R. Vicente, R. T. Garrod, K. M. Menten, F. Lewen, and S. Schlemmer\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201629309|Laboratory Spectroscopic Study and Astronomical Detection of Vibrationally Excited //n//-Propyl Cyanide]]**\\ | **[[https://doi.org/10.1051/0004-6361/201629309|Laboratory Spectroscopic Study and Astronomical Detection of Vibrationally Excited //n//-Propyl Cyanide]]**\\ |
| //Astron. Astrophys.// **595**, (2016) Art. No. A87.\\ | //Astron. Astrophys.// **595**, (2016) Art. No. A87.\\ |
| The four lowest vibrational states of each conformer, //gauche// and //anti//, were detected in the ALMA line survery described below. The intensities of all vibrational states are compatible with the earlier determined rotational temperature of 150 K. | The four lowest vibrational states of each conformer, //gauche// and //anti//, were detected in the ALMA line survery described below. The intensities of all vibrational states are compatible with the earlier determined rotational temperature of 150 K. |
| A. Belloche, R. T. Garrod, H. S. P. Müller, and K. M. Menten\\ | A. Belloche, R. T. Garrod, H. S. P. Müller, and K. M. Menten\\ |
| carried out a molecular line survey of Sagittarius B2(N) at 3 mm (between 84 and 111 GHz) with the Atacama Large Millimeter Array (ALMA) and reported on the\\ | carried out a molecular line survey of Sagittarius B2(N) at 3 mm (between 84 and 111 GHz) with the Atacama Large Millimeter Array (ALMA) and reported on the\\ |
| **[[http://dx.doi.org/10.1126/science.1256678|Detection of a Branched Alkyl Molecule in the Interstellar Medium: //iso//-Propyl Cyanide]]**\\ | **[[https://doi.org/10.1126/science.1256678|Detection of a Branched Alkyl Molecule in the Interstellar Medium: //iso//-Propyl Cyanide]]**\\ |
| //Science// **345**, (2014) 1584–1587.\\ | //Science// **345**, (2014) 1584–1587.\\ |
| See also the [[http://www.mpifr-bonn.mpg.de/pressreleases/2014/10|MPIfR press release]] (in English; German version also available) or the [[https://www.portal.uni-koeln.de/9015.html?&tx_news_pi1%5Bnews%5D=2543&tx_news_pi1%5Bcontroller%5D=News&tx_news_pi1%5Baction%5D=detail&cHash=7d0d470b18ca899e3116a7d35f57f0dc|Universität zu Köln press release]] (in German). | See also the **[[https://www.mpifr-bonn.mpg.de/pressreleases/2014/10|MPIfR press release]]** (in English; **[[https://www.mpifr-bonn.mpg.de/pressemeldungen/2014/10|German version]]** also available) or the **[[https://portal.uni-koeln.de/universitaet/aktuell/presseinformationen/detail/interstellare-molekuele-verzweigen-sich|Universität zu Köln press release]]** (in German). |
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| The molecule is the first one found in the interstellar medium with a branched carbon backbone. It is a first step towards confirming earlier assumptions that branched molecules are abundant in space. This is a particularly important finding for the search for amino acids and other biogenic molecules in space. The molecule is also the fourth alkyl cyanide found in space. | The molecule is the first one found in the interstellar medium with a branched carbon backbone. It is a first step towards confirming earlier assumptions that branched molecules are abundant in space. This is a particularly important finding for the search for amino acids and other biogenic molecules in space. The molecule is also the fourth alkyl cyanide found in space. |