CDMS classic documentation

new - [Recent Catalog Entries]

mueller@undisclosed.example.com (mueller) — Fri, 04 Sep 2026 13:48:09 +0000

2026/08/20 15:20		current
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	[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]		[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]

		+	* Sep. 2026: Glycidol; H<sub>2</sub>COD<sup>+</sup>.
	* Aug. 2026: Z-2,3-//c//-CHDCHDO; E-2,3-//c//-CHDCHDO; HD, //v// = 0; CH<sub>2</sub>DSH, //v//<sub>t</sub> = 0.		* Aug. 2026: Z-2,3-//c//-CHDCHDO; E-2,3-//c//-CHDCHDO; HD, //v// = 0; CH<sub>2</sub>DSH, //v//<sub>t</sub> = 0.
	* Jul. 2026: //c//-C<sub>5</sub>H<sub>6</sub>O; CH<sub>3</sub>SSH; CH<sub>3</sub>SCN.		* Jul. 2026: //c//-C<sub>5</sub>H<sub>6</sub>O; CH<sub>3</sub>SSH; CH<sub>3</sub>SCN.

etoh

mueller@undisclosed.example.com (mueller) — Tue, 25 Aug 2026 09:52:23 +0000

molecules

mueller@undisclosed.example.com (mueller) — Tue, 25 Aug 2026 08:51:58 +0000

2026/07/29 14:48		current
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	We welcome comments on this list!		We welcome comments on this list!
-	===== Molecules in the Interstellar Medium or Circumstellar Shells (as of 07/2026) =====	+	===== Molecules in the Interstellar Medium or Circumstellar Shells (as of 08/2026) =====

	^2 atoms ^3 atoms ^4 atoms ^5 atoms ^6 atoms ^7 atoms ^8 atoms ^9 atoms ^10 atoms ^11 atoms ^12 atoms ^>12 atoms ^		^2 atoms ^3 atoms ^4 atoms ^5 atoms ^6 atoms ^7 atoms ^8 atoms ^9 atoms ^10 atoms ^11 atoms ^12 atoms ^>12 atoms ^
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	\| KCl \| [[molecules:ism:C3\|C]]<sub>3</sub>* \| [[molecules:ism:H2CN\|H]]<sub>2</sub>CN \| [[molecules:ism:Hydroxymethylium\|H]]<sub>2</sub>COH<sup>+</sup> \| [[molecules:ism:C5N-minus\|C]]<sub>5</sub>N<sup>−</sup> \| [[molecules:ism:H2C5\|l-H]]<sub>2</sub>C<sub>5</sub> \| [[molecules:ism:C4H4\|CH]]<sub>2</sub>CHCCH \| [[molecules:ism:hydroxypropenal\|HOCHCHCHO]] \| [[molecules:ism:Glykolamid\|HOCH]]<sub>2</sub>C(O)NH<sub>2</sub> \| \| \| [[molecules:ism:Cyanoacenaphtalin\|5-C]]<sub>12</sub>H<sub>7</sub>CN \|		\| KCl \| [[molecules:ism:C3\|C]]<sub>3</sub>* \| [[molecules:ism:H2CN\|H]]<sub>2</sub>CN \| [[molecules:ism:Hydroxymethylium\|H]]<sub>2</sub>COH<sup>+</sup> \| [[molecules:ism:C5N-minus\|C]]<sub>5</sub>N<sup>−</sup> \| [[molecules:ism:H2C5\|l-H]]<sub>2</sub>C<sub>5</sub> \| [[molecules:ism:C4H4\|CH]]<sub>2</sub>CHCCH \| [[molecules:ism:hydroxypropenal\|HOCHCHCHO]] \| [[molecules:ism:Glykolamid\|HOCH]]<sub>2</sub>C(O)NH<sub>2</sub> \| \| \| [[molecules:ism:Cyanoacenaphtalin\|5-C]]<sub>12</sub>H<sub>7</sub>CN \|
	\| AlCl \| CO<sub>2</sub>* \| [[molecules:ism:SiC3\|c-SiC]]<sub>3</sub> \| [[molecules:ism:C4H-minus\|C]]<sub>4</sub>H<sup>−</sup> \| [[molecules:ism:Cyanomethanimin\|HNCHCN]] \| [[molecules:ism:mgc3n\|MgC]]<sub>5</sub>N \| [[molecules:ism:mgc2_4h\|MgC]]<sub>6</sub>H \| [[molecules:ism:HCxN-plus\|HC]]<sub>7</sub>N<sup>+</sup> \| [[molecules:ism:Butin\|CH]]<sub>3</sub>CH<sub>2</sub>CCH \| \| \| [[molecules:ism:Cyanopyren\|1-C]]<sub>16</sub>H<sub>9</sub>CN \|		\| AlCl \| CO<sub>2</sub>* \| [[molecules:ism:SiC3\|c-SiC]]<sub>3</sub> \| [[molecules:ism:C4H-minus\|C]]<sub>4</sub>H<sup>−</sup> \| [[molecules:ism:Cyanomethanimin\|HNCHCN]] \| [[molecules:ism:mgc3n\|MgC]]<sub>5</sub>N \| [[molecules:ism:mgc2_4h\|MgC]]<sub>6</sub>H \| [[molecules:ism:HCxN-plus\|HC]]<sub>7</sub>N<sup>+</sup> \| [[molecules:ism:Butin\|CH]]<sub>3</sub>CH<sub>2</sub>CCH \| \| \| [[molecules:ism:Cyanopyren\|1-C]]<sub>16</sub>H<sub>9</sub>CN \|
-	\| AlF \| [[molecules:ism:CH2\|CH]]<sub>2</sub> \| CH<sub>3</sub>* \| [[molecules:ism:HCOCN\|HC(O)CN]] \| [[molecules:ism:SiH3CN\|SiH]]<sub>3</sub>CN \| [[molecules:ism:cyanopropargyl\|CH]]<sub>2</sub>C<sub>3</sub>N \| [[molecules:ism:VyNH2\|C]]<sub>2</sub>H<sub>3</sub>NH<sub>2</sub> \| [[molecules:ism:C5H4\|CH]]<sub>2</sub>(CCH)<sub>2</sub> \| [[molecules:ism:Methylcarbamat\|CH]]<sub>3</sub>OC(O)N<sub>2</sub> (2026) \| \| \| [[molecules:ism:Cyanopyren\|2-C]]<sub>16</sub>H<sub>9</sub>CN (2025) \|	+	\| AlF \| [[molecules:ism:CH2\|CH]]<sub>2</sub> \| CH<sub>3</sub>* \| [[molecules:ism:HCOCN\|HC(O)CN]] \| [[molecules:ism:SiH3CN\|SiH]]<sub>3</sub>CN \| [[molecules:ism:cyanopropargyl\|CH]]<sub>2</sub>C<sub>3</sub>N \| [[molecules:ism:VyNH2\|C]]<sub>2</sub>H<sub>3</sub>NH<sub>2</sub> \| [[molecules:ism:C5H4\|CH]]<sub>2</sub>(CCH)<sub>2</sub> \| [[molecules:ism:Methylcarbamat\|CH]]<sub>3</sub>OC(O)NH<sub>2</sub> (2026) \| \| \| [[molecules:ism:Cyanopyren\|2-C]]<sub>16</sub>H<sub>9</sub>CN (2025) \|
	\| [[molecules:ism:PN\|PN]] \| [[molecules:ism:c_no\|C]]<sub>2</sub>O \| [[molecules:ism:C3N-minus\|C]]<sub>3</sub>N<sup>−</sup>\|[[molecules:ism:HNCNH\|HNCNH]] \| [[molecules:ism:C2_3S#information_on_thioxopentatetraenylidene_c5s\|C]]<sub>5</sub>S \| [[molecules:ism:NC4NH-plus\|NC]]<sub>4</sub>NH<sup>+</sup> \| [[molecules:ism:Ethendiol\|(CHOH)]]<sub>2</sub> \| [[molecules:ism:DMS\|(CH]]<sub>3</sub>)<sub>2</sub>S (2025) \| \| \| \| [[molecules:ism:Cyanopyren\|4-C]]<sub>16</sub>H<sub>9</sub>CN (2025) \|		\| [[molecules:ism:PN\|PN]] \| [[molecules:ism:c_no\|C]]<sub>2</sub>O \| [[molecules:ism:C3N-minus\|C]]<sub>3</sub>N<sup>−</sup>\|[[molecules:ism:HNCNH\|HNCNH]] \| [[molecules:ism:C2_3S#information_on_thioxopentatetraenylidene_c5s\|C]]<sub>5</sub>S \| [[molecules:ism:NC4NH-plus\|NC]]<sub>4</sub>NH<sup>+</sup> \| [[molecules:ism:Ethendiol\|(CHOH)]]<sub>2</sub> \| [[molecules:ism:DMS\|(CH]]<sub>3</sub>)<sub>2</sub>S (2025) \| \| \| \| [[molecules:ism:Cyanopyren\|4-C]]<sub>16</sub>H<sub>9</sub>CN (2025) \|
	\| [[molecules:ism:SiC\|SiC]] \| [[molecules:ism:MNC_MCN#MgNC\|MgNC]] \| [[molecules:ism:PH3\|PH]]<sub>3</sub> \| [[molecules:ism:MeO\|CH]]<sub>3</sub>O\| [[molecules:ism:MgC2_4H\|MgC]]<sub>4</sub>H \| [[molecules:ism:MgC2nH-plus\|MgC]]<sub>5</sub>N<sup>+</sup> \| [[molecules:ism:other_C6H2\|HC]]<sub>2</sub>(H)C<sub>4</sub> \| \| \| \| \| [[molecules:ism:Cyanocoronen\|C]]<sub>24</sub>H<sub>11</sub>CN (2025) \|		\| [[molecules:ism:SiC\|SiC]] \| [[molecules:ism:MNC_MCN#MgNC\|MgNC]] \| [[molecules:ism:PH3\|PH]]<sub>3</sub> \| [[molecules:ism:MeO\|CH]]<sub>3</sub>O\| [[molecules:ism:MgC2_4H\|MgC]]<sub>4</sub>H \| [[molecules:ism:MgC2nH-plus\|MgC]]<sub>5</sub>N<sup>+</sup> \| [[molecules:ism:other_C6H2\|HC]]<sub>2</sub>(H)C<sub>4</sub> \| \| \| \| \| [[molecules:ism:Cyanocoronen\|C]]<sub>24</sub>H<sub>11</sub>CN (2025) \|

formamid

mueller@undisclosed.example.com (mueller) — Tue, 25 Aug 2026 08:41:06 +0000

etcn

mueller@undisclosed.example.com (mueller) — Tue, 25 Aug 2026 08:38:51 +0000

sio

mueller@undisclosed.example.com (mueller) — Tue, 25 Aug 2026 08:17:45 +0000

2026/07/29 13:32		current
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	L. E. Snyder and D. Buhl\\		L. E. Snyder and D. Buhl\\
	proposed the\\		proposed the\\
-	[[https://ui.adsabs.harvard.edu/abs/1974ApJ...189L..31S\|Detection of Possible Maser Emission Near 3.48 Millimeters from an Unidentified Molecular Species in Orion]]\\	+	[[https://doi.org/10.1093/10.1086/181457\|Detection of Possible Maser Emission Near 3.48 Millimeters from an Unidentified Molecular Species in Orion]]\\
	//Astrophys. J.// 189, L31–L33 (1974).\\		//Astrophys. J.// 189, L31–L33 (1974).\\
	Orion A was observed with the 11 m Kitt Peak telescope. The frequency coincidence with the //J// = 2 – 1 transition of SiO in its first excited vibrational state was noted.\\		Orion A was observed with the 11 m Kitt Peak telescope. The frequency coincidence with the //J// = 2 – 1 transition of SiO in its first excited vibrational state was noted.\\
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	J. H. Davis, G. N. Blair, H. van Till, and P. Thaddeus,\\		J. H. Davis, G. N. Blair, H. van Till, and P. Thaddeus,\\
	who studied\\		who studied\\
-	[[https://ui.adsabs.harvard.edu/abs/1974ApJ...189L..31S\|Vibrationally Excited Silicon Monoxide in the Orion Nebula]]\\	+	[[https://doi.org/10.1093/10.1086/181520\|Vibrationally Excited Silicon Monoxide in the Orion Nebula]]\\
	//Astrophys. J.// 190, L117–L119 (1974).\\		//Astrophys. J.// 190, L117–L119 (1974).\\
	They observed the //J// = 3 – 2 transition of SiO.\\		They observed the //J// = 3 – 2 transition of SiO.\\
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	[[https://doi.org/10.1086/154774\|Millimeter emission lines in Orion A]]\\		[[https://doi.org/10.1086/154774\|Millimeter emission lines in Orion A]]\\
	//Astrophys. J.// 209, 770–777 (1976).\\		//Astrophys. J.// 209, 770–777 (1976).\\
-	Among them was the //J// = 2 − 1 transition of <sup>29</sup>SiO. The <sup>28</sup>Si/<sup>29</sup>Si ratio is 17.5 ± 5, consistent with the terrestrial ratio of19.6.\\	+	Among them was the //J// = 2 − 1 transition of <sup>29</sup>SiO. The <sup>28</sup>Si/<sup>29</sup>Si ratio is 17.5 ± 5, consistent with the terrestrial ratio of 19.6.\\
		+	\\
		+
		+	F.O. Clark and F.J. Lovas\\
		+	detected similarly\\
		+	[[https://doi.org/10.1086/182536\|<sup>30</sup>SiO in the interstellar medium]]\\
		+	//Astrophys. J.// 217, L47–L48 (1977).\\
		+	The isotopolog was detected toward Orion A and Sgr B2. The <sup>28</sup>Si/<sup>30</sup>Si ratio is 32 ± 8, concordant with the terrestrial ratio of 29.8. The line of the SiO main species displayed a double peak, suggestive of opacity or foreground absorption, preventing an isotopic ratio to be determined.\\
	\\		\\

phcn

mueller@undisclosed.example.com (mueller) — Thu, 13 Aug 2026 10:32:16 +0000

2026/08/13 12:15		current
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	reported on the\\		reported on the\\
	[[https://doi.org/10.1038/s41550-020-01253-4\|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]\\		[[https://doi.org/10.1038/s41550-020-01253-4\|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]\\
-	//Science// **359, 202–205 (2018**).\\	+	//Nat. Astron.// 5, 181–187 (2021).\\
-	Benzonitrile was detected by the same method as in the first reference toward four additional dark clouds, Serpens 1A, 1B, 2, and L1521F. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratio was found to be around 5 for the first threre sources and ~17 for L1521F, compared with ~23 in TMC-1 derivewd from the previous entry.\\	+	Benzonitrile was detected by the same method as in the first reference toward four additional dark clouds, Serpens 1A, 1B, 2, and L1521F. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratio was found to be around 5 for the first threre sources and ~17 for L1521F. The last value is very similar to the one in TMC-1 derivewd from the previous entry.\\
	\\		\\

	V. M. Rivilla, D. San Andrés, M. Sanz-Novo, L. Colzi, I. Jiménez-Serra, A. López-Gallifa, A. Martínez-Henares, A. Megías, S. Martín, B. Tercero, S. Zeng, J. Loreau, M. Ben Khalifa, M. A. Requena-Torres and P. de Vicente \\		V. M. Rivilla, D. San Andrés, M. Sanz-Novo, L. Colzi, I. Jiménez-Serra, A. López-Gallifa, A. Martínez-Henares, A. Megías, S. Martín, B. Tercero, S. Zeng, J. Loreau, M. Ben Khalifa, M. A. Requena-Torres and P. de Vicente \\
	announced\\		announced\\
-	[[https://doi.org/10.1051/0004-6361/202660367\|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]\\	+	[[https://doi.org/10.1051/0004-6361/202660367\|Aromatic Rings in the Central Molecular Zone: Benzonitrile]]\\
	//Astron. Astrophys.// 712, Art. No. A128 (2026).\\		//Astron. Astrophys.// 712, Art. No. A128 (2026).\\
		+	The molecule was detected in two kinetically warmer, rotationally cold clouds G+0.693−0.027 and G+0.633−0.0604 close to the Galactic center in the course of molecular line surveys with the Yebes 40 m dish. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratios of ~2.15 and ~2.4 are even lower than the values reported earlier. Additional values of comparison are given from other publications, including a value of ~30 in Lupus-1A.\\
		+	\\

	----		----

phenalene

mueller@undisclosed.example.com (mueller) — Mon, 03 Aug 2026 10:20:53 +0000

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	//Astron. Astrophys.// 701, Art. No. L8 (2025).\\		//Astron. Astrophys.// 701, Art. No. L8 (2025).\\
	Phenalene was identified through several //a//-type rotational transitions, often series easier to detect because of oblate pairing of the transitions having the same //K<sub>c</sub>// close to //J// and then blended with weaker //b//-type transitions having equivalent quantum numbres. Some isolated //b//-type transitions were also assigned in the astronomical spectrum. The identifications were based on the QUIJOTE molecular line survey carried out with the Yebes 40 m radio telescope between 31.0 and 50.4 GHz, but phenalene assignments were made only up to 39.8 GHz. A rotational temperature of 8 K was derived. The column density of phenalene appears to be slightly larger than that of the lighter indene, albeit with considerable uncertainty.\\		Phenalene was identified through several //a//-type rotational transitions, often series easier to detect because of oblate pairing of the transitions having the same //K<sub>c</sub>// close to //J// and then blended with weaker //b//-type transitions having equivalent quantum numbres. Some isolated //b//-type transitions were also assigned in the astronomical spectrum. The identifications were based on the QUIJOTE molecular line survey carried out with the Yebes 40 m radio telescope between 31.0 and 50.4 GHz, but phenalene assignments were made only up to 39.8 GHz. A rotational temperature of 8 K was derived. The column density of phenalene appears to be slightly larger than that of the lighter indene, albeit with considerable uncertainty.\\
		+	\\
		+
		+	G. Wenzel, T. H. Speak, C. Xue, E. A. Bergin, A. M. Burkhardt, M. A. Cordiner, M. Duffy, Z. T. P. Fried, A. Lipnicky, C. N. Shingledecker, R. H. J. Willis, A. J. Remijan, M. C. McCarthy, B. A. McGuire, and I. R. Cooke\\
		+	reported on the\\
		+	**[[https://doi.org/10.3847/2041-8213/ae8757\|Detection of the Polycyclic Aromatic Hydrocarbon Phenalene (C13H10) in the Very
		+	Low-luminosity Object MC27/L1521F]]**\\
		+	//Astrophys. J. Lett.// 1006, Art. No. L38 (2026).\\
		+	The molecule was identified by line stacking of observations carried out with thw GBT 100 m dish. While the column density of phenalene is similar to the one in TMC-1 CP, but the phenalene/benzonitrile ratios differ. It is ~9 in TMC-1 CP, whereas it is ~40 in MC27/L1521F.\\
	\\		\\

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2019/04/25 13:38		current
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	===== On the Detection of Ethanol in Space =====		===== On the Detection of Ethanol in Space =====

-	Ethanol, C<sub>2</sub>H<sub>5</sub>OH, occurs in two conformers. The //anti// conformer is the lowest one. The heavy atoms occupy a //trans// configuration; for that matter, this conformer is frequently, but not quite correctly refered to as the //trans// conformer. The //gauche// conformers are higher in energy by 0.47 kJ/mol, 39.5 cm<sup>–1</sup>, or 56.8 K.	+	Ethanol, C<sub>2</sub>H<sub>5</sub>OH, occurs in two conformers. The //anti// conformer is the lowest one. The heavy atoms occupy a //trans// configuration; for that matter, this conformer is frequently, but not quite correctly refered to as the //trans// conformer. The //gauche// conformers are higher in energy by 0.47 kJ/mol, 39.5 cm<sup>–1</sup>, or 56.8 K.\\
		+	\\

	Ethanol in its lowest //anti// configuration was among the early molecules to be detected in space. Its first detection was reported by:\\		Ethanol in its lowest //anti// configuration was among the early molecules to be detected in space. Its first detection was reported by:\\
	B. Zuckerman, B. E. Turner, D. R. Johnson, F. O. Clark, F. J. Lovas, N. Fourikis, P. Palmer, M. Morris, A. E. Lilley, J. A. Ball, C. A. Gottlieb, and H. Penfield,\\		B. Zuckerman, B. E. Turner, D. R. Johnson, F. O. Clark, F. J. Lovas, N. Fourikis, P. Palmer, M. Morris, A. E. Lilley, J. A. Ball, C. A. Gottlieb, and H. Penfield,\\
-	[[http://cdsads.u-strasbg.fr/abs/1975ApJ...196L..99Z\|Detection of Interstellar //trans//-Ethyl Alcohol]]\\	+	[[https://ui.adsabs.harvard.edu/abs/1975ApJ...196L..99Z\|Detection of Interstellar //trans//-Ethyl Alcohol]]\\
	//Astrophys. J.// 196, L99–L102 (1975).\\		//Astrophys. J.// 196, L99–L102 (1975).\\
-	Three //b//-type transitions (6<sub>06</sub> – 5<sub>15</sub>, 4<sub>14</sub> – 3<sub>03</sub>, and 5<sub>15</sub> – 4<sub>04</sub>) were detected with the 36-foot NRAO telescope in the 3 mm region toward the massive star-forming region Sagittarius B2(OH). Since then, //anti//-ethanol was detected in many massive star-forming regions, including W51M, G34.3+0.15, and Orion KL as well as other molecular clouds with somewhat elevated temperatures (around 100 K).	+	Three //b//-type transitions (6<sub>06</sub> – 5<sub>15</sub>, 4<sub>14</sub> – 3<sub>03</sub>, and 5<sub>15</sub> – 4<sub>04</sub>) were detected with the 36-foot NRAO telescope in the 3 mm region toward the massive star-forming region Sagittarius B2(OH). Since then, //anti//-ethanol was detected in many massive star-forming regions, including W51M, G34.3+0.15, and Orion KL as well as other molecular clouds with somewhat elevated temperatures (around 100 K).\\
		+	\\

	The molecule was also detected in some of the investigated 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 or three transitions were detected with the IRAM 30 m telescope in the 3 mm range by\\		The molecule was also detected in some of the investigated 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 or three transitions were detected with the IRAM 30 m telescope in the 3 mm range by\\
	M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\		M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\
	[[https://doi.org/10.1051/0004-6361:20065190\|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]\\		[[https://doi.org/10.1051/0004-6361:20065190\|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]\\
-	//Astron. Astrophys.// 455, 971–985 (2006).	+	//Astron. Astrophys.// 455, 971–985 (2006).\\
		+	\\

	S. E. Bisschop, J. K. Jørgensen, T. L. Bourke, S. Bottinelli, and E. F. van Dishoeck,\\		S. E. Bisschop, J. K. Jørgensen, T. L. Bourke, S. Bottinelli, and E. F. van Dishoeck,\\
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	[[https://doi.org/10.1051/0004-6361:200809673\|An interferometric study of the low-mass protostar IRAS 16293-2422: small scale organic chemistry]]\\		[[https://doi.org/10.1051/0004-6361:200809673\|An interferometric study of the low-mass protostar IRAS 16293-2422: small scale organic chemistry]]\\
	//Astron. Astrophys.// 488, 959–968 (2008).\\		//Astron. Astrophys.// 488, 959–968 (2008).\\
-	They found evidence for the presence of ethanol in this low mass protostellar object.	+	They found evidence for the presence of ethanol in this low mass protostellar object.\\
		+	\\

	J. C. Pearson, K. V. L. N. Sastry, E. Herbst, and F. C. De Lucia,\\		J. C. Pearson, K. V. L. N. Sastry, E. Herbst, and F. C. De Lucia,\\
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	[[https://doi.org/10.1086/303967\|//gauche// Ethyl Alcohol: Laboratory Assignments and Interstellar Identification]]\\		[[https://doi.org/10.1086/303967\|//gauche// Ethyl Alcohol: Laboratory Assignments and Interstellar Identification]]\\
	//Astrophys. J.// 480, 420–L102 (1997).\\		//Astrophys. J.// 480, 420–L102 (1997).\\
-	All these lines are //c//-type //Q//-branch transitions with //K<sub>a</sub>// = 1 ↔ 0 and //J// between 17 and 31; they occur between 97.5 and 98.0 GHz. Only one line appeared to be blended with a line different from //gauche//-ethanol. Additional U-lines in the 3 mm region were also assigned to this conformer.	+	All these lines are //c//-type //Q//-branch transitions with //K<sub>a</sub>// = 1 ↔ 0 and //J// between 17 and 31; they occur between 97.5 and 98.0 GHz. Only one line appeared to be blended with a line different from //gauche//-ethanol. Additional U-lines in the 3 mm region were also assigned to this conformer.\\
		+	\\

	H. S. P. Müller, A. Belloche, L.-H. Xu, R. M. Lees, R. T. Garrod, A. Walters, J. van Wijngaarden, F. Lewen, S. Schlemmer, and K. M. Menten,\\		H. S. P. Müller, A. Belloche, L.-H. Xu, R. M. Lees, R. T. Garrod, A. Walters, J. van Wijngaarden, F. Lewen, S. Schlemmer, and K. M. Menten,\\
Line 30:		Line 35:
	[[https://doi.org/10.1051/0004-6361/201527470\|Exploring molecular complexity with ALMA (EMoCA): Alkanethiols and alkanols in Sagittarius B2(N2)]]\\		[[https://doi.org/10.1051/0004-6361/201527470\|Exploring molecular complexity with ALMA (EMoCA): Alkanethiols and alkanols in Sagittarius B2(N2)]]\\
	//Astron. Astrophys.// 587, Art. No. A92 (2016).\\		//Astron. Astrophys.// 587, Art. No. A92 (2016).\\
-	A line survey of Sgr B2(N) was carried out with ALMA at 3 mm. Both <sup>13</sup>C isotopomers were detected with a <sup>12</sup>C/<sup>13</sup>C ratio of 25, which is usual in the Galactic Center.	+	A line survey of Sgr B2(N) was carried out with ALMA at 3 mm. Both <sup>13</sup>C isotopomers were detected with a <sup>12</sup>C/<sup>13</sup>C ratio of 25, which is usual in the Galactic Center.\\
		+	\\

	J. K. Jørgensen, H. S. P. Müller, H. Calcutt, A. Coutens, M. N. Drozdovskaya, K. I. Öberg, M. V. Persson, V. Taquet, E. F. van Dishoeck, and S. F. Wampfler\\		J. K. Jørgensen, H. S. P. Müller, H. Calcutt, A. Coutens, M. N. Drozdovskaya, K. I. Öberg, M. V. Persson, V. Taquet, E. F. van Dishoeck, and S. F. Wampfler\\
Line 36:		Line 42:
	[[https://doi.org/10.1051/0004-6361/201731667\|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]\\		[[https://doi.org/10.1051/0004-6361/201731667\|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]\\
	//Astron. Astrophys.// 620, Art. No. A170 (2018).\\		//Astron. Astrophys.// 620, Art. No. A170 (2018).\\
-	The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time the mono-deuterated isotopomers (three different ones; in addition, CH<sub>2</sub>DCH<sub>2</sub>OH has two conformers). The D/H ratio per H atom is about 0.05 to about 0.06. Lines of the two <sup>13</sup>C isotopomers were also detected, albeit not enough for a clear detection. The <sup>12</sup>C/<sup>13</sup>C ratio appears to be about 25, much lower than the local ISM value of 68. A confirmation of this value is desirable. Ethanol is among the molecules with warmer rotational temperatures of around 300 K in that hot corino.	+	The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time the mono-deuterated isotopomers (three different ones; in addition, CH<sub>2</sub>DCH<sub>2</sub>OH has two conformers). The D/H ratio per H atom is about 0.05 to about 0.06. Lines of the two <sup>13</sup>C isotopomers were also detected, albeit not enough for a clear detection. The <sup>12</sup>C/<sup>13</sup>C ratio appears to be about 25, much lower than the local ISM value of 68. A confirmation of this value is desirable. Ethanol is among the molecules with warmer rotational temperatures of around 300 K in that hot corino.\\
		+	\\

	----		----

	Contributor(s): H. S. P. Müller; 11, 2009; 07, 2012; 11, 2016; 01, 2019		Contributor(s): H. S. P. Müller; 11, 2009; 07, 2012; 11, 2016; 01, 2019
-

	----		----

2019/07/26 18:56		current
Line 3:		Line 3:
	Formamide, HC(O)NH<sub>2</sub>, is a fairly typical hot core molecule that is quite abundant. The first transition of this molecule was detected toward Sgr B2 and likely toward Sgr A by\\		Formamide, HC(O)NH<sub>2</sub>, is a fairly typical hot core molecule that is quite abundant. The first transition of this molecule was detected toward Sgr B2 and likely toward Sgr A by\\
	R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\		R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\
-	[[http://cdsads.u-strasbg.fr/abs/1971ApJ...169L..39R\|Microwave Detection of Interstellar Formamide]]\\	+	[[https://ui.adsabs.harvard.edu/abs/1971ApJ...169L..39R\|Microwave Detection of Interstellar Formamide]]\\
	//Astrophys. J.// 169, L39–L43 (1971).\\		//Astrophys. J.// 169, L39–L43 (1971).\\
	They detected all three Δ//F// = 0 hyperfine components of the //K<sub>a</sub>// = 1, //J// = 2 – 2 transition near 4619 MHz. Only the strongest component, overlapped in part with the H112α transition, was tentatively detected toward Sgr A.\\		They detected all three Δ//F// = 0 hyperfine components of the //K<sub>a</sub>// = 1, //J// = 2 – 2 transition near 4619 MHz. Only the strongest component, overlapped in part with the H112α transition, was tentatively detected toward Sgr A.\\
	The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\		The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\
	C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\		C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\
-	[[http://cdsads.u-strasbg.fr/abs/1973ApJ...182..699G\|Studies of Interstellar Formamide]]\\	+	[[https://ui.adsabs.harvard.edu/abs/1973ApJ...182..699G\|Studies of Interstellar Formamide]]\\
-	//Astrophys. J.// 182, 699–710 (1973).	+	//Astrophys. J.// 182, 699–710 (1973).\\
		+	\\

	[[http://cdsads.u-strasbg.fr/abs/1978A%26A....70L..77L\|Detection of the <sup>13</sup>C Isotope of Formamide in the Galactic Center]]\\		[[http://cdsads.u-strasbg.fr/abs/1978A%26A....70L..77L\|Detection of the <sup>13</sup>C Isotope of Formamide in the Galactic Center]]\\
Line 15:		Line 16:
	B. Lazareff, R. Lucas, and P. Encrenaz,\\		B. Lazareff, R. Lucas, and P. Encrenaz,\\
	//Astron. Astrophys.// 70, L77–L78 (1978).\\		//Astron. Astrophys.// 70, L77–L78 (1978).\\
-	The //F// = 2 – 2 HFS component of the //J// = 1 – 1 transitions was observed near 1571 GHz toward Sgr B2.	+	The //F// = 2 – 2 HFS component of the //J// = 1 – 1 transitions was observed near 1571 GHz toward Sgr B2.\\
		+	\\

	A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, N. F. W. Ligterink, K. I. Öberg, M. V. Persson, E. F. van Dishoeck, and S. F. Wampfler\\		A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, C. Favre, E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, N. F. W. Ligterink, K. I. Öberg, M. V. Persson, E. F. van Dishoeck, and S. F. Wampfler\\
Line 21:		Line 23:
	[[https://doi.org/10.1051/0004-6361/201628612\|The ALMA-PILS Survey: First Detections of Deuterated Formamide and Deuterated Isocyanic Acid in the Interstellar Medium]]\\		[[https://doi.org/10.1051/0004-6361/201628612\|The ALMA-PILS Survey: First Detections of Deuterated Formamide and Deuterated Isocyanic Acid in the Interstellar Medium]]\\
	//Astron. Astrophys.// 590, Art. No. L6 (2016).\\		//Astron. Astrophys.// 590, Art. No. L6 (2016).\\
-	Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a <sup>12</sup>C/<sup>13</sup>C ratio of 68 because lines of the main isotopolog are frequently affected by optical depth effects.	+	Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a <sup>12</sup>C/<sup>13</sup>C ratio of 68 because lines of the main isotopolog are frequently affected by optical depth effects.\\
		+	\\

	A. Belloche, R. T. Garrod, H. S. P. Müller, K. M. Menten, I. Medvedev, J. Thomas, and Z. Kisiel\\		A. Belloche, R. T. Garrod, H. S. P. Müller, K. M. Menten, I. Medvedev, J. Thomas, and Z. Kisiel\\
Line 27:		Line 30:
	[[https://doi.org/10.1051/0004-6361/201935428\|Re-exploring Molecular Complexity with ALMA (ReMoCA): Interstellar Detection of Urea]]\\		[[https://doi.org/10.1051/0004-6361/201935428\|Re-exploring Molecular Complexity with ALMA (ReMoCA): Interstellar Detection of Urea]]\\
	//Astron. Astrophys.// 628, Art. No. A10 (2019).\\		//Astron. Astrophys.// 628, Art. No. A10 (2019).\\
-	In the course of a new unbiased line survey toward the high-mass star-forming region Sagittarius (Sgr) B2(N) close to the Galactic center, HC(<sup>18</sup>O)NH<sub>2</sub> and HC(O)<sup>15</sup>NH<sub>2</sub> were detected. The <sup>16</sup>O/<sup>18</sup>O ratio of 140 is in the range of values found in the Galactic center, the <sup>14</sup>N/<sup>15</sup>N ratio is about 300.	+	In the course of a new unbiased line survey toward the high-mass star-forming region Sagittarius (Sgr) B2(N) close to the Galactic center, HC(<sup>18</sup>O)NH<sub>2</sub> and HC(O)<sup>15</sup>NH<sub>2</sub> were detected. The <sup>16</sup>O/<sup>18</sup>O ratio of 140 is in the range of values found in the Galactic center, the <sup>14</sup>N/<sup>15</sup>N ratio is about 300.\\
		+	\\

-	The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, G34_3+0.15, and NGC 6334(I).	+	The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, G34_3+0.15, and NGC 6334(I).\\
		+	\\

	In addition,\\		In addition,\\
Line 36:		Line 41:
	[[https://doi.org/10.1088/2041-8205/763/2/L38\|Detection of Formamide, the Simplest but Crucial Amide, in a Solar-type Protostar]]\\		[[https://doi.org/10.1088/2041-8205/763/2/L38\|Detection of Formamide, the Simplest but Crucial Amide, in a Solar-type Protostar]]\\
	//Astrophys. J.// 763, Art. No. L38 (2013).\\		//Astrophys. J.// 763, Art. No. L38 (2013).\\
-	The protostar is the usual suspect, IRAS 16293–2422.	+	The protostar is the usual suspect, IRAS 16293–2422.\\
		+	\\

	V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\		V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\
Line 47:		Line 53:
	[[https://doi.org/10.1051/0004-6361/201834467\|Small-scale Physical and Chemical Structure of Diffuse and Translucent Molecular Clouds along the Line of Sight to Sgr B2]]\\		[[https://doi.org/10.1051/0004-6361/201834467\|Small-scale Physical and Chemical Structure of Diffuse and Translucent Molecular Clouds along the Line of Sight to Sgr B2]]\\
	//Astron. Astrophys.// 623 Art. No. A68 (2019).\\		//Astron. Astrophys.// 623 Art. No. A68 (2019).\\
-	Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds.	+	Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds.\\
		+	\\

	R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\		R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\
	described the\\		described the\\
	[[https://doi.org/10.1051/0004-6361/201220033\|Rotational Spectrum of Formamide up to 1 THz and First ISM Detection of its //v//<sub>12</sub> Vibrational State]]\\		[[https://doi.org/10.1051/0004-6361/201220033\|Rotational Spectrum of Formamide up to 1 THz and First ISM Detection of its //v//<sub>12</sub> Vibrational State]]\\
-	//Astron. Astrophys.// 548, Art. No. A71 (2012).	+	//Astron. Astrophys.// 548, Art. No. A71 (2012).\\
		+	\\

	----		----

	Contributor(s): H. S. P. Müller; 05, 2009; 08, 2012; 02, 2013; 06, 2016; 10, 2017; 01, 2019		Contributor(s): H. S. P. Müller; 05, 2009; 08, 2012; 02, 2013; 06, 2016; 10, 2017; 01, 2019
-

	----		----

2019/10/24 09:45		current
Line 4:		Line 4:
	D. R. Johnson, F. J. Lovas, C. A. Gottlieb, E. W. Gottlieb, M. M. Litvak, P. Thaddeus, and M. Guélin,\\		D. R. Johnson, F. J. Lovas, C. A. Gottlieb, E. W. Gottlieb, M. M. Litvak, P. Thaddeus, and M. Guélin,\\
	[[https://ui.adsabs.harvard.edu/abs/1977ApJ...218..370J\|Detection of Interstellar Ethyl Cyanide]]\\		[[https://ui.adsabs.harvard.edu/abs/1977ApJ...218..370J\|Detection of Interstellar Ethyl Cyanide]]\\
-	//Astrophys. J.// 218, L370–L376 (1977).	+	//Astrophys. J.// 218, L370–L376 (1977).\\
		+	\\

	More recently, however, it has also been detected toward a low-mass star-forming region:\\		More recently, however, it has also been detected toward a low-mass star-forming region:\\
Line 10:		Line 11:
	[[https://doi.org/10.1086/378038\|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]\\		[[https://doi.org/10.1086/378038\|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]\\
	//Astrophys. J.// 593, L51–L55 (2003).\\		//Astrophys. J.// 593, L51–L55 (2003).\\
		+	\\

	Ethyl cyanide in its two lowest vibrational states //v//<sub>13</sub> ≡ //v//<sub>b</sub> = 1 (in plane CCN bend; ca. 206.5 cm<sup>–1</sup>) and //v//<sub>21</sub> ≡ //v//<sub>t</sub> = 1 (torsion; ca. 212.7 cm<sup>–1</sup>) has been detected in a 3, 2, and 1 mm line survey carried out with SEST:\\		Ethyl cyanide in its two lowest vibrational states //v//<sub>13</sub> ≡ //v//<sub>b</sub> = 1 (in plane CCN bend; ca. 206.5 cm<sup>–1</sup>) and //v//<sub>21</sub> ≡ //v//<sub>t</sub> = 1 (torsion; ca. 212.7 cm<sup>–1</sup>) has been detected in a 3, 2, and 1 mm line survey carried out with SEST:\\
Line 19:		Line 20:
	D. M. Mehringer, J. C. Pearson, J. Keene, and T. G. Philips,\\		D. M. Mehringer, J. C. Pearson, J. Keene, and T. G. Philips,\\
	[[https://doi.org/10.1086/386357\|Detection of Vibrationally Excited Ethyl Cyanide in the Interstellar Medium]]\\		[[https://doi.org/10.1086/386357\|Detection of Vibrationally Excited Ethyl Cyanide in the Interstellar Medium]]\\
-	//Astrophys. J.// 608, 306–313 (2004).	+	//Astrophys. J.// 608, 306–313 (2004).\\
		+	\\

	These states as well as higher vibrational states up to v<sub>12</sub> = 1 at 770 K were detected toward Orion KL by\\		These states as well as higher vibrational states up to v<sub>12</sub> = 1 at 770 K were detected toward Orion KL by\\
Line 28:		Line 30:
	A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito:\\		A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito:\\
	[[https://doi.org/10.1051/0004-6361/201321096\|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]\\		[[https://doi.org/10.1051/0004-6361/201321096\|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]\\
-	//Astron. Astrophys.// 559, Art. No. A47 (2013).	+	//Astron. Astrophys.// 559, Art. No. A47 (2013).\\
		+	\\

	The three <sup>13</sup>C isotopic species have been reported first in observations toward Orion IRc2 by\\		The three <sup>13</sup>C isotopic species have been reported first in observations toward Orion IRc2 by\\
Line 38:		Line 41:
	H. S. P. Müller, A. Belloche, K. M. Menten, C. Comito, and P. Schilke,\\		H. S. P. Müller, A. Belloche, K. M. Menten, C. Comito, and P. Schilke,\\
	[[https://doi.org/10.1016/j.jms.2008.03.016\|Rotational Spectroscopy of Isotopic Vinyl Cyanide, H<sub>2</sub>C=CH–C≡N, in the Laboratory and in Space]],\\		[[https://doi.org/10.1016/j.jms.2008.03.016\|Rotational Spectroscopy of Isotopic Vinyl Cyanide, H<sub>2</sub>C=CH–C≡N, in the Laboratory and in Space]],\\
-	//J. Mol. Spectrosc.// 250, 319–325 (2008).	+	//J. Mol. Spectrosc.// 250, 319–325 (2008).\\
		+	\\

	The detection of the <sup>15</sup>N isotopolog (in Orion KL) was reported first by\\		The detection of the <sup>15</sup>N isotopolog (in Orion KL) was reported first by\\
	L. Margulès, R. Motiyenko, K. Demyk, B. Tercero, J. Cernicharo, M. Sheng, M. Weidmann, J. Gripp, H. Mäder, and J. Demaison,\\		L. Margulès, R. Motiyenko, K. Demyk, B. Tercero, J. Cernicharo, M. Sheng, M. Weidmann, J. Gripp, H. Mäder, and J. Demaison,\\
	[[https://doi.org/10.1051/0004-6361:200810889\|Rotational Spectrum of Deuterated and <sup>15</sup>N Ethyl Cyanides: CH<sub>3</sub>CHDCN and CH<sub>2</sub>DCH<sub>2</sub>CN and of CH<sub>3</sub>CH<sub>2</sub>C<sup>15</sup>N]]\\		[[https://doi.org/10.1051/0004-6361:200810889\|Rotational Spectrum of Deuterated and <sup>15</sup>N Ethyl Cyanides: CH<sub>3</sub>CHDCN and CH<sub>2</sub>DCH<sub>2</sub>CN and of CH<sub>3</sub>CH<sub>2</sub>C<sup>15</sup>N]]\\
-	//Astron. Astrophys.// **559, Art. No. A47 (2013**).\\	+	//Astron. Astrophys.// **493, 565 (2009**).\\
	The isotopolog was also detected in Sagittarius B2(N2), the northern, secondary hot-core of Sgr B2(N), by\\		The isotopolog was also detected in Sagittarius B2(N2), the northern, secondary hot-core of Sgr B2(N), by\\
	A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten,\\		A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten,\\
	[[https://doi.org/10.1051/0004-6361/201527268\|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]\\		[[https://doi.org/10.1051/0004-6361/201527268\|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]\\
-	//Astron. Astrophys.// 587, Art. No. A91 (2016).	+	//Astron. Astrophys.// 587, Art. No. A91 (2016).\\
		+	\\

	A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\		A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\
Line 53:		Line 58:
	[[https://doi.org/10.1051/0004-6361/201527268\|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]\\		[[https://doi.org/10.1051/0004-6361/201527268\|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]\\
	//Astron. Astrophys.// 587, Art. No. A91 (2016).\\		//Astron. Astrophys.// 587, Art. No. A91 (2016).\\
-	They report the tentative detection of deuterated ethyl cyanide in the course of their 3 mm line survey with ALMA. Their ratios of the normal species to the one deuterated at the out-of-plane methyl group position and at the methylene group are about 2000, the upper limit to the one deuterate at the in-plane methyl group position is 4000, consistent with the other positions which occur twice each. The number of clean lines was so small that the authors refrained from claiming a firm detection.	+	They report the tentative detection of deuterated ethyl cyanide in the course of their 3 mm line survey with ALMA. Their ratios of the normal species to the one deuterated at the out-of-plane methyl group position and at the methylene group are about 2000, the upper limit to the one deuterate at the in-plane methyl group position is 4000, consistent with the other positions which occur twice each. The number of clean lines was so small that the authors refrained from claiming a firm detection.\\
		+	\\

	L. Margulès, A. Belloche, H. S. P. Müller, R. A. Motiyenko, J.-C. Guillemin, R. T. Garrod, and K. M. Menten,\\		L. Margulès, A. Belloche, H. S. P. Müller, R. A. Motiyenko, J.-C. Guillemin, R. T. Garrod, and K. M. Menten,\\
Line 59:		Line 65:
	[[https://doi.org/10.1051/0004-6361/201628309\|Spectroscopic Study and Astronomical Detection of Doubly <sup>13</sup>C-Substituted Ethyl Cyanide]]\\		[[https://doi.org/10.1051/0004-6361/201628309\|Spectroscopic Study and Astronomical Detection of Doubly <sup>13</sup>C-Substituted Ethyl Cyanide]]\\
	//Astron. Astrophys.// 590, Art. No. A93 (2016).\\		//Astron. Astrophys.// 590, Art. No. A93 (2016).\\
-	The astronomical detection was made in Sagittarius B2(N2) in the course of their 3 mm line survey with ALMA.	+	The astronomical detection was made in Sagittarius B2(N2) in the course of their 3 mm line survey with ALMA.\\
		+	\\

	----		----