CDMS classic documentation

new - [Recent Catalog Entries]

mueller@undisclosed.example.com (mueller) — Fri, 06 Nov 2026 10:46:29 +0000

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	[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]		[[archive#less_recent_catalog_entries\|Earlier Catalog Entries]]

		+	* Nov. 2026: H<sub>2</sub>CSO.
	* Oct. 2026: FeS, //v// = 0, Ω = 4; FeS, //v// = 0, Ω = 3; FeS, //v// = 1, Ω = 4; FeS, //v// = 1, Ω = 3; ClCH<sub>2</sub>CH<sub>2</sub>OH; <sup>37</sup>ClCH<sub>2</sub>CH<sub>2</sub>OH.		* Oct. 2026: FeS, //v// = 0, Ω = 4; FeS, //v// = 0, Ω = 3; FeS, //v// = 1, Ω = 4; FeS, //v// = 1, Ω = 3; ClCH<sub>2</sub>CH<sub>2</sub>OH; <sup>37</sup>ClCH<sub>2</sub>CH<sub>2</sub>OH.
	* Sep. 2026: Glycidol; H<sub>2</sub>COD<sup>+</sup>; NS<sup>+</sup>; <sup>15</sup>NS<sup>+</sup>; erythrulose.		* Sep. 2026: Glycidol; H<sub>2</sub>COD<sup>+</sup>; NS<sup>+</sup>; <sup>15</sup>NS<sup>+</sup>; erythrulose.
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	[[archive#molecules_in_space\|Archive "Molecules in Space"]]		[[archive#molecules_in_space\|Archive "Molecules in Space"]]

		+	* Nov. 2026: updated TiO documentation.
	* Oct. 2026: added C<sub>2</sub>H<sup>+</sup> with documentation, updated CH<sub>3</sub>OH documentation.		* Oct. 2026: added C<sub>2</sub>H<sup>+</sup> with documentation, updated CH<sub>3</sub>OH documentation.
	* Sep. 2026: added erythrulose with documentation.		* Sep. 2026: added erythrulose with documentation.

ti-oxide - [Titanium Dioxide]

mueller@undisclosed.example.com (mueller) — Mon, 02 Nov 2026 11:16:32 +0000

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	[[https://doi.org/10.3847/2041-8213/aeacbe\|Dust-seeding Molecules in a Massive Protostar—Detection of TiO in Orion Source I]]\\		[[https://doi.org/10.3847/2041-8213/aeacbe\|Dust-seeding Molecules in a Massive Protostar—Detection of TiO in Orion Source I]]\\
	//Astrophys. J. Lett.// 1011, Art. No. L13 (2026).\\		//Astrophys. J. Lett.// 1011, Art. No. L13 (2026).\\
		+	Archival ALMA data were inspected. Three Ω = 1 transitions with //J//" = 10, 20, 26 near 348.2, 664.3, and 853.8 GHz were observed with good to very good S/N. Its abundance is only a factor of ~78 lower than that of SiO. Thus, it is about a factor of ~5 more abundant than in CI chondrites, which may be reconciled by the fact that a substantial fraction of Si in Orion Source I is present in SiS.\\
		+	\\

	Finally, the detection of rotational transitions in the circumstellar envelope of VY CMa (and others) will be described in the TiO<sub>2</sub> section.\\		Finally, the detection of rotational transitions in the circumstellar envelope of VY CMa (and others) will be described in the TiO<sub>2</sub> section.\\
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	----		----

-	Contributor(s): H. S. P. Müller; 03, 2013; 03, 2017; 12, 2020	+	Contributor(s): H. S. P. Müller; 03, 2013; 03, 2017; 12, 2020; 11, 2026

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ch3oh

mueller@undisclosed.example.com (mueller) — Tue, 13 Oct 2026 08:55:52 +0000

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	CD<sub>3</sub>OD, along with many other methanol isotopologs, was detected toward IRAS4A2 in the NGC 1333 molecular cloud in the course of the molecular line survey mentioned in the title and carried with ALMA between 279.0 and 311.7 GHz. Deuteration is very high in the methyl group with the abundance of CHD<sub>2</sub>OH being only slightly smaller than that of CH<sub>2</sub>DOH and CD<sub>3</sub>OH only slightly less than half of CHD<sub>2</sub>OH. Deuteration is less pronounced in the hydroxyl group, as commonly observed, the abundance of CH<sub>3</sub>OD is about a factor of 1.5 lower than that of CD<sub>3</sub>OH, and the ratio between CD<sub>3</sub>OH and CD<sub>3</sub>OD is ~22.5. CH<sub>3</sub><sup>17</sup>OH was also detected clearly a factor of 4 less than CH<sub>3</sub><sup>18</sup>OH. The detection of numerous isotopologs in their excited torsional states is unsurprising because of a rotational temperature of ~200 K. The lack of laboratory data accounts for CH<sub>2</sub>DOH and CHD<sub>2</sub>OH being not detected in torsionally excited states.\\		CD<sub>3</sub>OD, along with many other methanol isotopologs, was detected toward IRAS4A2 in the NGC 1333 molecular cloud in the course of the molecular line survey mentioned in the title and carried with ALMA between 279.0 and 311.7 GHz. Deuteration is very high in the methyl group with the abundance of CHD<sub>2</sub>OH being only slightly smaller than that of CH<sub>2</sub>DOH and CD<sub>3</sub>OH only slightly less than half of CHD<sub>2</sub>OH. Deuteration is less pronounced in the hydroxyl group, as commonly observed, the abundance of CH<sub>3</sub>OD is about a factor of 1.5 lower than that of CD<sub>3</sub>OH, and the ratio between CD<sub>3</sub>OH and CD<sub>3</sub>OD is ~22.5. CH<sub>3</sub><sup>17</sup>OH was also detected clearly a factor of 4 less than CH<sub>3</sub><sup>18</sup>OH. The detection of numerous isotopologs in their excited torsional states is unsurprising because of a rotational temperature of ~200 K. The lack of laboratory data accounts for CH<sub>2</sub>DOH and CHD<sub>2</sub>OH being not detected in torsionally excited states.\\
	\\		\\
-	MPIfR issued press releases [[https://www.mpifr-bonn.mpg.de/pressemeldungen/2026/erster-nachweis-von-schwerem-methanol-im-weltraum?c=8727\|in German]] and in [[https://www.mpifr-bonn.mpg.de/pressemeldungen/2026/erster-nachweis-von-schwerem-methanol-im-weltraum?c=8727\|in English]]. Press releases were also issued by other participating institutions.	+	MPIfR issued press releases [[https://www.mpifr-bonn.mpg.de/pressemeldungen/2026/erster-nachweis-von-schwerem-methanol-im-weltraum?c=8727\|in German]] and in [[https://www.mpifr-bonn.mpg.de/pressreleases/2026/first-detection-of-heavy-methanol-in-space\|in English]]. Press releases were also issued by other participating institutions.\\
	\\		\\
	\\		\\

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