CDMS classic documentation

new - [Molecules in Space]

mueller@undisclosed.example.com (mueller) — Wed, 29 Jul 2026 12:58:55 +0000

2026/07/29 11:46		current
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	[[archive#molecules_in_space\|Archive "Molecules in Space"]]		[[archive#molecules_in_space\|Archive "Molecules in Space"]]

-	* Jul. 2026: added OH documentation.	+	* Jul. 2026: added OH documentation; updated SiO and HC<sub>9</sub>N documentations.
	* Jun. 2026: added methyl carbamate; updated glycolamide documentation.		* Jun. 2026: added methyl carbamate; updated glycolamide documentation.
	* Apr. 2026: added 2,5-cyclohexadienthione with documentation, updated CH<sub>3</sub>OH and CH<sub>3</sub>CN documentations.		* Apr. 2026: added 2,5-cyclohexadienthione with documentation, updated CH<sub>3</sub>OH and CH<sub>3</sub>CN documentations.

hc9n

mueller@undisclosed.example.com (mueller) — Wed, 29 Jul 2026 12:58:17 +0000

2020/08/12 12:43		current
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	[[https://ui.adsabs.harvard.edu/abs/1978ApJ...223L.105B\|The Detection of HC<sub>9</sub>N in Interstellar Space]]\\		[[https://ui.adsabs.harvard.edu/abs/1978ApJ...223L.105B\|The Detection of HC<sub>9</sub>N in Interstellar Space]]\\
	//Astrophys. J.// 223, L105–L107 (1978)\\		//Astrophys. J.// 223, L105–L107 (1978)\\
-	reported the first detection of this cyanopolyyne in two transitions (//J// = 18 – 17 and 25 – 24 near 10.5 and 14.5 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory before the molecules was detected in the laboratory. The spectroscopic parameters were estimated from the smaller cyanopolyynes. Heile's Cloud 2 is better known as TMC-1.	+	reported the first detection of this cyanopolyyne in two transitions (//J// = 18 – 17 and 25 – 24 near 10.5 and 14.5 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory before the molecules was detected in the laboratory. The spectroscopic parameters were estimated from the smaller cyanopolyynes. Heile's Cloud 2 is better known as TMC-1.\\
		+	\\

	More recently, the molecule was also detected in six transitions in the circumstellar shell of the famous carbon star CW Leo:\\		More recently, the molecule was also detected in six transitions in the circumstellar shell of the famous carbon star CW Leo:\\
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	[[https://ui.adsabs.harvard.edu/abs/1992ApJ...400..551B\|The Excitation Temperature of HC<sub>9</sub>N in the Circumstellar Envelope of IRC +10216]]\\		[[https://ui.adsabs.harvard.edu/abs/1992ApJ...400..551B\|The Excitation Temperature of HC<sub>9</sub>N in the Circumstellar Envelope of IRC +10216]]\\
	//Astrophys. J.// 400, 551–555 (1992).\\		//Astrophys. J.// 400, 551–555 (1992).\\
		+	\\

	Truong-Bach, D. Graham, and Nguyen-Q-Rieu,\\		Truong-Bach, D. Graham, and Nguyen-Q-Rieu,\\
Line 15:		Line 17:
	//Astron. Astrophys.// 277, 133–138 (1993);\\		//Astron. Astrophys.// 277, 133–138 (1993);\\
	detected one additional higher-//J// transition toward the former source and the same transition in a protoplanetary nebula.\\		detected one additional higher-//J// transition toward the former source and the same transition in a protoplanetary nebula.\\
		+	\\

	J. R. Pardo, C. Bermúdez, C. Cabezas, M. Agúndez, J. D. Gallego, J. P. Fonfría, L. Velilla-Prieto, G. Quintana-Lacaci, B. Tercero, M. Guélin, and J. Cernicharo\\		J. R. Pardo, C. Bermúdez, C. Cabezas, M. Agúndez, J. D. Gallego, J. P. Fonfría, L. Velilla-Prieto, G. Quintana-Lacaci, B. Tercero, M. Guélin, and J. Cernicharo\\
Line 21:		Line 24:
	//Astron. Astrophys.// 640, Art. No. L13 (2020).\\		//Astron. Astrophys.// 640, Art. No. L13 (2020).\\
	The authors carried out an unbiased molecular line survey with the Yebes 40 m dish between 31 and 50 GHz toward the circumstellar envelope of the famous C-rich AGB star CW Leonis. Numerous transitions of HC<sub>9</sub>N in its lowest excited state //v//<sub>19</sub> = 1 were detected despite the low rotational temperature. The lines could be assigned unambiguously although no laboratory data were available for this excited state. The derived HC<sub>5</sub>N to HC<sub>7</sub>N ratio is extremely low, roughly 2.4. The derived HC<sub>7</sub>N to HC<sub>9</sub>N ratio is still very low, roughly 7.7.\\		The authors carried out an unbiased molecular line survey with the Yebes 40 m dish between 31 and 50 GHz toward the circumstellar envelope of the famous C-rich AGB star CW Leonis. Numerous transitions of HC<sub>9</sub>N in its lowest excited state //v//<sub>19</sub> = 1 were detected despite the low rotational temperature. The lines could be assigned unambiguously although no laboratory data were available for this excited state. The derived HC<sub>5</sub>N to HC<sub>7</sub>N ratio is extremely low, roughly 2.4. The derived HC<sub>7</sub>N to HC<sub>9</sub>N ratio is still very low, roughly 7.7.\\
		+	\\

		+	J. R. Pardo, J. Cernicharo, J. P. Fonfría, C. Cabezas, M. Agúndez, B. Tercero, N. Marcelino, P. de Vicente, L. Velilla-Prieto and M. Guélin\\
		+	announced some time later the\\
		+	[[https://doi.org/10.1051/0004-6361/202659372\|Discovery of HC<sub>9</sub>N //v//<sub>19</sub> Overtones in IRC +10216]]\\
		+	//Astron. Astrophys.// 709, Art. No. L13 (2026).\\
		+	Deeper integration than in the previous entry permitted overtone states of HC<sub>9</sub>N to detect up to //v//<sub>19</sub> = 8.\\
		+	\\

	----		----

-	Contributor(s): H. S. P. Müller; 02, 2006; 06, 2009; 08, 2020.	+	Contributor(s): H. S. P. Müller; 02, 2006; 06, 2009; 08, 2020; 07, 2026.

	----		----

molecules - [Molecules in the Interstellar Medium or Circumstellar Shells (as of 06/2026)]

mueller@undisclosed.example.com (mueller) — Wed, 29 Jul 2026 12:48:50 +0000

2026/07/28 14:07		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 06/2026) =====	+	===== Molecules in the Interstellar Medium or Circumstellar Shells (as of 07/2026) =====

	^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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	\| CH \| [[molecules:ism:HCO-plus\|HCO]]<sup>+</sup> \| [[molecules:ism:H2CO\|H]]<sub>2</sub>CO \| [[molecules:ism:Formic_Acid\|HCOOH]] \| [[molecules:ism:MeCN\|CH]]<sub>3</sub>CN \| [[molecules:ism:Propin\|CH]]<sub>3</sub>C<sub>2</sub>H \| [[molecules:ism:MeC3N\|CH]]<sub>3</sub>C<sub>3</sub>N \| [[molecules:ism:EtOH\|CH]]<sub>3</sub>CH<sub>2</sub>OH \| [[molecules:ism:glycol\|(CH]]<sub>2</sub>OH)<sub>2</sub> \| [[molecules:ism:ch3c6h\|CH]]<sub>3</sub>C<sub>6</sub>H\| [[molecules:ism:PrCN#on_the_detection_of_n-propyl_cyanide_in_space\|n-C]]<sub>3</sub>H<sub>7</sub>CN \| [[molecules:ism:Fullerene#C70\|C]]<sub>70</sub>*\|		\| CH \| [[molecules:ism:HCO-plus\|HCO]]<sup>+</sup> \| [[molecules:ism:H2CO\|H]]<sub>2</sub>CO \| [[molecules:ism:Formic_Acid\|HCOOH]] \| [[molecules:ism:MeCN\|CH]]<sub>3</sub>CN \| [[molecules:ism:Propin\|CH]]<sub>3</sub>C<sub>2</sub>H \| [[molecules:ism:MeC3N\|CH]]<sub>3</sub>C<sub>3</sub>N \| [[molecules:ism:EtOH\|CH]]<sub>3</sub>CH<sub>2</sub>OH \| [[molecules:ism:glycol\|(CH]]<sub>2</sub>OH)<sub>2</sub> \| [[molecules:ism:ch3c6h\|CH]]<sub>3</sub>C<sub>6</sub>H\| [[molecules:ism:PrCN#on_the_detection_of_n-propyl_cyanide_in_space\|n-C]]<sub>3</sub>H<sub>7</sub>CN \| [[molecules:ism:Fullerene#C70\|C]]<sub>70</sub>*\|
	\| CN \| [[molecules:ism:HCN\|HCN]] \| [[molecules:ism:HCNO\|HNCO]] \| [[molecules:ism:H2CNH\|H]]<sub>2</sub>CNH \| [[molecules:ism:Formamid\|NH]]<sub>2</sub>CHO \| [[molecules:ism:MeNH2\|CH]]<sub>3</sub>NH<sub>2</sub> \| [[molecules:ism:C7H\|C]]<sub>7</sub>H \| [[molecules:ism:EtCN\|CH]]<sub>3</sub>CH<sub>2</sub>CN \| [[molecules:ism:c3_aldehydes\|CH]]<sub>3</sub>CH<sub>2</sub>CHO \| [[molecules:ism:Ethylformiat\|C]]<sub>2</sub>H<sub>5</sub>OCHO \| [[molecules:ism:PrCN#on_the_detection_of_i-propyl_cyanide_in_space\|i-C]]<sub>3</sub>H<sub>7</sub>CN \| [[molecules:ism:C60-plus\|C]]<sub>60</sub><sup>+</sup>* \|		\| CN \| [[molecules:ism:HCN\|HCN]] \| [[molecules:ism:HCNO\|HNCO]] \| [[molecules:ism:H2CNH\|H]]<sub>2</sub>CNH \| [[molecules:ism:Formamid\|NH]]<sub>2</sub>CHO \| [[molecules:ism:MeNH2\|CH]]<sub>3</sub>NH<sub>2</sub> \| [[molecules:ism:C7H\|C]]<sub>7</sub>H \| [[molecules:ism:EtCN\|CH]]<sub>3</sub>CH<sub>2</sub>CN \| [[molecules:ism:c3_aldehydes\|CH]]<sub>3</sub>CH<sub>2</sub>CHO \| [[molecules:ism:Ethylformiat\|C]]<sub>2</sub>H<sub>5</sub>OCHO \| [[molecules:ism:PrCN#on_the_detection_of_i-propyl_cyanide_in_space\|i-C]]<sub>3</sub>H<sub>7</sub>CN \| [[molecules:ism:C60-plus\|C]]<sub>60</sub><sup>+</sup>* \|
-	\| [[molecules:ism:OH\|OH]] \| OCS \| [[molecules:ism:H2CS\|H]]<sub>2</sub>CS \| [[molecules:ism:Cyanamid\|H]]<sub>2</sub>NCN \| [[molecules:ism:MeSH\|CH]]<sub>3</sub>SH \| [[molecules:ism:VCN\|CH]]<sub>2</sub>CHCN \| [[molecules:ism:HAc\|CH]]<sub>3</sub>COOH \| [[molecules:ism:HC7N\|HC]]<sub>7</sub>N \| [[molecules:ism:MeC5N\|CH]]<sub>3</sub>C<sub>5</sub>N \| [[molecules:ism:MeAc\|CH]]<sub>3</sub>OC(O)CH<sub>3</sub> \| [[molecules:ism:EME\|C]]<sub>2</sub>H<sub>5</sub>OCH<sub>3</sub> \|[[molecules:ism:PhCN\|c-C]]<sub>6</sub>H<sub>5</sub>CN \|	+	\| [[molecules:ism:OH\|OH]] \| OCS \| [[molecules:ism:H2CS\|H]]<sub>2</sub>CS \| [[molecules:ism:Cyanamid\|H]]<sub>2</sub>NCN \| [[molecules:ism:MeSH\|CH]]<sub>3</sub>SH \| [[molecules:ism:VCN\|CH]]<sub>2</sub>CHCN \| [[molecules:ism:HAc\|CH]]<sub>3</sub>COOH \| [[molecules:ism:HC7N\|HC]]<sub>7</sub>N \| [[molecules:ism:MeC5N\|CH]]<sub>3</sub>C<sub>5</sub>N \| [[molecules:ism:MeAc\|CH]]<sub>3</sub>OC(O)CH<sub>3</sub> \| [[molecules:ism:EME\|C]]<sub>2</sub>H<sub>5</sub>OCH<sub>3</sub> \|[[molecules:ism:PhCN\|c-C]]<sub>6</sub>H<sub>5</sub>CN \|
	\| CO \| [[molecules:ism:HNC\|HNC]] \| [[molecules:ism:HC2nH#HC2H\|C]]<sub>2</sub>H<sub>2</sub>* \| [[molecules:ism:H2CCO\|H]]<sub>2</sub>C<sub>2</sub>O \| [[molecules:ism:C2H4\|C]]<sub>2</sub>H<sub>4</sub>* \| [[molecules:ism:HC5N\|HC]]<sub>5</sub>N \| [[molecules:ism:C6H2\|C]]<sub>6</sub>H<sub>2</sub> \| [[molecules:ism:ch3c4h\|CH]]<sub>3</sub>C<sub>4</sub>H \| [[molecules:ism:Methyloxiran\|CH]]<sub>3</sub>CHCH<sub>2</sub>O \| [[molecules:ism:Hydroxyaceton\|CH]]<sub>3</sub>C(O)CH<sub>2</sub>OH \| [[molecules:ism:Cyanocyclopentadien\|1-c-C]]<sub>5</sub>H<sub>5</sub>CN \| [[molecules:ism:HC11N\|HC]]<sub>11</sub>N \|		\| CO \| [[molecules:ism:HNC\|HNC]] \| [[molecules:ism:HC2nH#HC2H\|C]]<sub>2</sub>H<sub>2</sub>* \| [[molecules:ism:H2CCO\|H]]<sub>2</sub>C<sub>2</sub>O \| [[molecules:ism:C2H4\|C]]<sub>2</sub>H<sub>4</sub>* \| [[molecules:ism:HC5N\|HC]]<sub>5</sub>N \| [[molecules:ism:C6H2\|C]]<sub>6</sub>H<sub>2</sub> \| [[molecules:ism:ch3c4h\|CH]]<sub>3</sub>C<sub>4</sub>H \| [[molecules:ism:Methyloxiran\|CH]]<sub>3</sub>CHCH<sub>2</sub>O \| [[molecules:ism:Hydroxyaceton\|CH]]<sub>3</sub>C(O)CH<sub>2</sub>OH \| [[molecules:ism:Cyanocyclopentadien\|1-c-C]]<sub>5</sub>H<sub>5</sub>CN \| [[molecules:ism:HC11N\|HC]]<sub>11</sub>N \|
	\| H<sub>2</sub> \| [[molecules:ism:H2S\|H]]<sub>2</sub>S \| C<sub>3</sub>N \| [[molecules:ism:C4H\|C]]<sub>4</sub>H \| [[molecules:ism:C5H\|C]]<sub>5</sub>H \| [[molecules:ism:C6H\|C]]<sub>6</sub>H \| [[molecules:ism:glycolaldehyd\|CH]]<sub>2</sub>OHCHO \| [[molecules:ism:C8H\|C]]<sub>8</sub>H \| [[molecules:ism:Methoxymethanol\|CH]]<sub>3</sub>OCH<sub>2</sub>OH \| [[molecules:ism:Cyclopentadien\|c-C]]<sub>5</sub>H<sub>6</sub> \| [[molecules:ism:Cyanocyclopentadien\|2-c-C]]<sub>5</sub>H<sub>5</sub>CN \| [[molecules:ism:Cyanonaphtalin\|1-C]]<sub>10</sub>H<sub>7</sub>CN \|		\| H<sub>2</sub> \| [[molecules:ism:H2S\|H]]<sub>2</sub>S \| C<sub>3</sub>N \| [[molecules:ism:C4H\|C]]<sub>4</sub>H \| [[molecules:ism:C5H\|C]]<sub>5</sub>H \| [[molecules:ism:C6H\|C]]<sub>6</sub>H \| [[molecules:ism:glycolaldehyd\|CH]]<sub>2</sub>OHCHO \| [[molecules:ism:C8H\|C]]<sub>8</sub>H \| [[molecules:ism:Methoxymethanol\|CH]]<sub>3</sub>OCH<sub>2</sub>OH \| [[molecules:ism:Cyclopentadien\|c-C]]<sub>5</sub>H<sub>6</sub> \| [[molecules:ism:Cyanocyclopentadien\|2-c-C]]<sub>5</sub>H<sub>5</sub>CN \| [[molecules:ism:Cyanonaphtalin\|1-C]]<sub>10</sub>H<sub>7</sub>CN \|

sio

mueller@undisclosed.example.com (mueller) — Wed, 29 Jul 2026 11:44:19 +0000

2026/07/29 13:27		current
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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. \\	+	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.\\
	\\		\\

oh

mueller@undisclosed.example.com (mueller) — Wed, 29 Jul 2026 09:43:33 +0000

2026/07/29 11:28		current
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	\\		\\

		+	B. Parise, F. Du, F.-C. Liu, A. Belloche, H. Wiesemeyer, R. Güsten, K. M. Menten, H.-W. Hübers, and B. Klein\\
		+	announced the\\
		+	[[https://doi.org/10.1051/0004-6361/201218784\|Detection of OD towards the Low-Mass Protostar IRAS 16293−2422]]\\
		+	//Astron. Astrophys.// 542, Art. No. L5 (2012).\\
		+	The GREAT receiver on board SOFIA was employed for the observations. A relatively high ratio of OD to HDO was found.\\
		+	\\

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ch-plus

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2021/07/14 10:46		current
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	//Astrophys. J.// 93, 11–23 (1941);\\		//Astrophys. J.// 93, 11–23 (1941);\\
	He reportedly also observed the third line.\\		He reportedly also observed the third line.\\
		+	\\

	The detection of its pure rotational spectrum toward in the planetary nebula NGC 7027 was reported by\\		The detection of its pure rotational spectrum toward in the planetary nebula NGC 7027 was reported by\\
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	[[https://doi.org/10.1086/310729\|Discovery of Far-Infrared Pure Rotational Transitions of CH<sup>+</sup> in NGC 7027]]\\		[[https://doi.org/10.1086/310729\|Discovery of Far-Infrared Pure Rotational Transitions of CH<sup>+</sup> in NGC 7027]]\\
	//Astrophys. J.// 483, L65–L68 (1997).\\		//Astrophys. J.// 483, L65–L68 (1997).\\
		+	\\

	More recently, interstellar methylidynium has been observed for the first time in high resolution and in absorption towards the star-forming region G10.6-0.4. Actually, as observation of the //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> is hampered by a terrestrial O<sub>2</sub> line, <sup>13</sup>CH<sup>+</sup> was observed instead:\\		More recently, interstellar methylidynium has been observed for the first time in high resolution and in absorption towards the star-forming region G10.6-0.4. Actually, as observation of the //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> is hampered by a terrestrial O<sub>2</sub> line, <sup>13</sup>CH<sup>+</sup> was observed instead:\\
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	//Astrophys. J.// 634, L149–L152 (2005).\\		//Astrophys. J.// 634, L149–L152 (2005).\\
	Please note that the inferred rest-frequency is incorrect. Two alternative rest frequencies were proposed of which the higher one is quite appropriate.\\		Please note that the inferred rest-frequency is incorrect. Two alternative rest frequencies were proposed of which the higher one is quite appropriate.\\
		+	\\

	The //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> has been detected with the //Herschel// satellite in emission toward the Orion Bar by\\		The //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> has been detected with the //Herschel// satellite in emission toward the Orion Bar by\\
Line 39:		Line 42:
	//Astron. Astrophys.// 518, Art. No. L118 (2010).\\		//Astron. Astrophys.// 518, Art. No. L118 (2010).\\
	These authors were the first to use the correct rest frequency of 835137.5 MHz.\\		These authors were the first to use the correct rest frequency of 835137.5 MHz.\\
		+	\\

	Higher-//J// transitions of CH<sup>+</sup> were also detected with the PACS instrument on board of the //Herschel// satellite in the disc around a Herbig Be star by:\\		Higher-//J// transitions of CH<sup>+</sup> were also detected with the PACS instrument on board of the //Herschel// satellite in the disc around a Herbig Be star by:\\
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	[[https://doi.org/10.1051/0004-6361/201116678\|Detection of CH<sup>+</sup> Emission from the Disc around HD 100546]]\\		[[https://doi.org/10.1051/0004-6361/201116678\|Detection of CH<sup>+</sup> Emission from the Disc around HD 100546]]\\
	//Astron. Astrophys.// 530, Art. No. L2 (2011).\\		//Astron. Astrophys.// 530, Art. No. L2 (2011).\\
		+	\\

	D. A. Neufeld, M. Goto, T. R. Geballe, R. Güsten, K. M. Menten, and H. Wiesemeyer\\		D. A. Neufeld, M. Goto, T. R. Geballe, R. Güsten, K. M. Menten, and H. Wiesemeyer\\
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	//Astrophys. J.// 894, Art. No. 37 (2020).\\		//Astrophys. J.// 894, Art. No. 37 (2020).\\
	They detected in addition the //v// = 1 − 0, //P//(6) to //R//(3) transitions of CH<sup>+</sup> around 3.5 μm using the iSHELL spectrograph at the Infrared Telescope Facility on Mauna Kea. The //P//(6) line, however, is severely blended with a hydrogen recombination line. A separate account is planned on this subject.\\		They detected in addition the //v// = 1 − 0, //P//(6) to //R//(3) transitions of CH<sup>+</sup> around 3.5 μm using the iSHELL spectrograph at the Infrared Telescope Facility on Mauna Kea. The //P//(6) line, however, is severely blended with a hydrogen recombination line. A separate account is planned on this subject.\\
		+	\\

	T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, A. Schwörer, and C. Comito\\		T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, A. Schwörer, and C. Comito\\
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	//Astron. Astrophys.// 651, Art. No. A9 (2021).\\		//Astron. Astrophys.// 651, Art. No. A9 (2021).\\
	They observed clearly the //J// = 2 − 1 transition of CD<sup>+</sup> near 906.8 GHz mostly in absorption. The //J// = 4 − 2 transition near 1811.2 GHz is seen weakly in absorption.\\		They observed clearly the //J// = 2 − 1 transition of CD<sup>+</sup> near 906.8 GHz mostly in absorption. The //J// = 4 − 2 transition near 1811.2 GHz is seen weakly in absorption.\\
		+	\\

	----		----

-	Contributor(s): H. S. P. Müller; 2003; 02, 2006; 03, 2007; 04, 2011; 05, 2020; 07, 2021	+	Contributor(s): H. S. P. Müller; 2003; 02, 2006; 03, 2007; 04, 2011; 05, 2020; 07, 2021.

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