Differences

This shows you the differences between two versions of the page.

--- molecules:ism:c2_3s [2019/10/21 17:20] – mueller
+++ molecules:ism:c2_3s [2021/12/20 12:47] – [Additional information on C2S] mueller
@@ Line 7: / Line 7: @@
 **[[https://ui.adsabs.harvard.edu/abs/1987ApJ...317L.111K|Detection of Intense Unidentified Lines in TMC-1]]**\\
 //Astrophys. J.// **317**, L111–L114 (1987);\\
-obtained in the course of a molecular line survey carried out with the 45 m Nobeyama telescope which ultimately covered the 8 – 50 GHz range.
+obtained in the course of a molecular line survey carried out with the 45 m Nobeyama telescope which ultimately covered the 8 – 50 GHz range.\\
+\\
 Laboratory spectroscopic investigations by\\
@@ Line 16: / Line 17: @@
 Four lines from the line survey mentioned above were assigned to C<sub>2</sub>S. These were the //N<sub>J</sub>// = 1<sub>2</sub> – 2<sub>1</sub>, 3<sub>3</sub> – 2<sub>2</sub>, 4<sub>3</sub> – 3<sub>2</sub>, and 3<sub>4</sub> – 2<sub>3</sub> transitions at 22344, 38866, 43981, and 45379 MHz, respectively. Please note: the labeling of the 2<sub>1</sub> level follows that of the CDMS catalog entry. This level is labeled 0<sub>1</sub> in the original work.\\
 The authors also assigned several U-lines from two molecular line surveys of Sagittarius B2 in the 3 and 2 mm regions to C<sub>2</sub>S.\\
-Finally, the CC<sup>34</sup>S isotopolog was also detected toward TMC-1 by its 1<sub>2</sub> – 2<sub>1</sub> transition at 21930 MHz.
+Finally, the CC<sup>34</sup>S isotopolog was also detected toward TMC-1 by its 1<sub>2</sub> – 2<sub>1</sub> transition at 21930 MHz.\\
+\\
 In addition, laboratory spectroscopic investigations by\\
@@ Line 30: / Line 32: @@
 J. Cernicharo, M. Guélin, H. Hein, and C. Kahane,\\
 **[[https://ui.adsabs.harvard.edu/abs/1987A%26A...181L...9C|Sulfur in IRC +10216]]**\\
-//Astron. Astrophys.// **181**, L9–L12 (1987).
+//Astron. Astrophys.// **181**, L9–L12 (1987).\\
+\\
 C<sub>2</sub>S was also seen toward several translucent clouds, albeit in only the lower energy transition of two by\\
@@ Line 36: / Line 39: @@
 **[[https://doi.org/10.1086/313077|The Physics and Chemistry of Small Translucent Molecular Clouds.\\
 IX. Acetylenic Chemistry]]**\\
-//Astrophys. J. Suppl. Ser.// **115**, 91–118 (1998).
+//Astrophys. J. Suppl. Ser.// **115**, 91–118 (1998).\\
+\\
 The two <sup>13</sup>C isotopomers were detected with the Nobeyama 45 m telescope toward TMC-1 by\\
@@ Line 73: / Line 77: @@
 **[[https://doi.org/10.1051/0004-6361/201424542|New molecules in IRC +10216: confirmation of C<sub>5</sub>S and tentative identification of MgCCH, NCCP, and SiH<sub>3</sub>CN]]**\\
 //Astron. Astrophys.// **570**, Art. No. A45 (2014).\\
-The //J// + 1 – //J// transitions with //J// = 43, 44, and 45 of C<sub>5</sub>S were identified in the course of a 3 mm line survey with the IRAM 30 m telescope near 81.2, 83.0, and 84.9 GHz. The first transition is blended. The identification rests to a considerable amount on an earlier report detailed below that is deemed to be not secure. Therefore, we suggest to view the identification of C<sub>5</sub>S in space with some caution.
+The //J// + 1 → //J// transitions with //J// = 43, 44, and 45 of C<sub>5</sub>S were identified in the course of a 3 mm line survey with the IRAM 30 m telescope near 81.2, 83.0, and 84.9 GHz. The first transition is blended. The almost similar column densities between two carbon chain molecules, here C<sub>5</sub>S and C<sub>3</sub>S, are very unusual, though not unprecedented.\\
 M. B. Bell, L. W. Avery, and P. A. Feldman\\
@@ Line 79: / Line 83: @@
 **[[https://ui.adsabs.harvard.edu/abs/1993ApJ...417L..37B|C<sub>3</sub>S and C<sub>5</sub>S in IRC +10216]]**\\
 //Astrophys. J.// **417**, L37–L40 (1993).\\
-A line observed with the NRAO 43 m telecope near 24.0 GHz in the course of a molecular line survey was assigned to the //J// = 13 – 12 transition of C<sub>5</sub>S. The authors state in the abstract: "Assuming the observed feature is due to C<sub>5</sub>S, we find that //N//(C<sub>5</sub>S)///N//(C<sub></sub>S) ≈ 0.5." Confirmation of this finding or identification of further transitions at shorter wavelengths will be useful.
+A line observed with the NRAO 43 m telecope near 24.0 GHz in the course of a molecular line survey was assigned to the //J// = 13 – 12 transition of C<sub>5</sub>S. The authors state in the abstract: "Assuming the observed feature is due to C<sub>5</sub>S, we find that //N//(C<sub>5</sub>S)///N//(C<sub>3</sub>S) ≈ 0.5." Confirmation of this finding or identification of further transitions at shorter wavelengths will be useful.\\
+The molecule was recently also identified in TMC-1 by\\
+J. Cernicharo, C. Cabezas, M. Agúndez, B. Tercero, J. R. Pardo, N. Marcelino, J. D. Gallego, F. Tercero, J. A. López-Pérez, and P. de Vicente\\
+**[[https://doi.org/10.1051/0004-6361/202140642|TMC-1, the starless core sulfur factory: Discovery of NCS, HCCS, H<sub>2</sub>CCS, H<sub>2</sub>CCCS, and C<sub>4</sub>S and detection of C<sub>5</sub>S]]**\\
+//Astron. Astrophys.// **648**, Art. No. L3 (2021).\\
+C<sub>5</sub>S was identified through 5 rotational transitions with //J"// = 16 to 20 and with modest to good signal-to-noise ratio (one slightly blended, one severely blended) in the course of a molecular line survey of the prototypical cold dark molecular cloud TMC-1 carried out with the Yebes 40 m radio telescope between 32.8 and 49.2 GHz. See below for statements on the column densities.\\
 ----
-==== Information on C4S and larger species ====
+==== Information on C4S ====
-Thioxobutatrienylidene, C<sub>4</sub>S, and larger molecules C<sub>n</sub>S, with n ≥ 6, have not been detected in space thus far.
+J. Cernicharo, C. Cabezas, M. Agúndez, B. Tercero, J. R. Pardo, N. Marcelino, J. D. Gallego, F. Tercero, J. A. López-Pérez, and P. de Vicente\\
+reported on\\
+**[[https://doi.org/10.1051/0004-6361/202140642|TMC-1, the starless core sulfur factory: Discovery of NCS, HCCS, H<sub>2</sub>CCS, H<sub>2</sub>CCCS, and C<sub>4</sub>S and detection of C<sub>5</sub>S]]**\\
+//Astron. Astrophys.// **648**, Art. No. L3 (2021).\\
+C<sub>4</sub>S was identified through for fine structure transitions with //N"// = 9 to 12 and //J// = //N// + 1 and with moderate to good signal-to-noise ratio (one slightly blended, one severely blended) in the course of a molecular line survey of the prototypical cold dark molecular cloud TMC-1 carried out with the Yebes 40 m radio telescope between 32.8 and 49.2 GHz. The column density of C<sub>4</sub>S is slightly lower than that of C<sub>5</sub>S, and about factors of 340 and 1350 lower than those of C<sub>3</sub>S and C<sub>2</sub>S, respectively.
 ----
-Contributor(s): H. S. P. Müller; 09, 2012; 07, 2018
+Contributor(s): H. S. P. Müller; 09, 2012; 07, 2018; 09, 2020; 04, 2021