CDMS classic documentation

new - [Recent Catalog Entries]

mueller@undisclosed.example.com (mueller) — Thu, 20 Aug 2026 13:20:14 +0000

2026/08/14 12:45		current
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	[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]		[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]

-	* Aug. 2026: Z-2,3-//c//-CHDCHDO; E-2,3-//c//-CHDCHDO; HD, //v// = 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.
	* Jun. 2026: 1-Cyanocyclopentene; MgC<sub>4</sub>H; MgC<sub>3</sub>N; CaC<sub>4</sub>H; CaC<sub>3</sub>N.		* Jun. 2026: 1-Cyanocyclopentene; MgC<sub>4</sub>H; MgC<sub>3</sub>N; CaC<sub>4</sub>H; CaC<sub>3</sub>N.

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.\\
		+	\\

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phenalene

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

2026/08/03 12:10		current
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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.\\
	\\		\\

molecules - [Molecules in the Interstellar Medium or Circumstellar Shells (as of 07/2026)]

mueller@undisclosed.example.com (mueller) — Mon, 03 Aug 2026 10:09:27 +0000

2026/07/28 14:08		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 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 ^

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:\\
Line 10:		Line 11:
	[[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,\\
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	//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\\
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	//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.

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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.\\
	\\		\\

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