molecules:ism:c2_3s

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molecules:ism:c2_3s [2019/05/09 12:43] – [Additional information on C2S] muellermolecules:ism:c2_3s [2021/12/20 12:48] (current) – [Information on thioxopentatetraenylidene, C5S] mueller
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 N. Kaifu, H. Suzuki, M. Ohishi, T. Miyaki, S.-I. Ishikawa, T. Kasuga, M. Morimoto, and S. Saito\\ N. Kaifu, H. Suzuki, M. Ohishi, T. Miyaki, S.-I. Ishikawa, T. Kasuga, M. Morimoto, and S. Saito\\
 reported on the\\ reported on the\\
-**[[http://cdsads.u-strasbg.fr/abs/1987ApJ...317L.111K|Detection of Intense Unidentified Lines in TMC-1]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1987ApJ...317L.111K|Detection of Intense Unidentified Lines in TMC-1]]**\\
 //Astrophys. J.// **317**, L111–L114 (1987);\\ //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\\ Laboratory spectroscopic investigations by\\
 S. Saito, K. Kawaguchi, S. Yamamoto, M. Ohishi, H. Suzuki, and N. Kaifu\\ S. Saito, K. Kawaguchi, S. Yamamoto, M. Ohishi, H. Suzuki, and N. Kaifu\\
 lead to the\\ lead to the\\
-**[[http://cdsads.u-strasbg.fr/abs/1987ApJ...317L.115S|Laboratory Detection and Astronomical Identification of a New Free Radical, CCS <sup>3</sup>Σ<sup>–</sup>]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1987ApJ...317L.115S|Laboratory Detection and Astronomical Identification of a New Free Radical, CCS <sup>3</sup>Σ<sup>–</sup>]]**\\
 //Astrophys. J.// **317**, L115–L118 (1987).\\ //Astrophys. J.// **317**, L115–L118 (1987).\\
 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.\\ 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.\\ 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\\ In addition, laboratory spectroscopic investigations by\\
 S. Yamamoto, S. Saito, K. Kawaguchi, N. Kaifu, and H. Suzuki\\ S. Yamamoto, S. Saito, K. Kawaguchi, N. Kaifu, and H. Suzuki\\
 lead to the\\ lead to the\\
-**[[http://cdsads.u-strasbg.fr/abs/1987ApJ...317L.119Y|Laboratory Detection of a New Carbon-chain Molecule C<sub>3</sub>S and its Astronomical Identification]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1987ApJ...317L.119Y|Laboratory Detection of a New Carbon-chain Molecule C<sub>3</sub>S and its Astronomical Identification]]**\\
 //Astrophys. J.// **317**, L119–L121 (1987).\\ //Astrophys. J.// **317**, L119–L121 (1987).\\
 The //J// = 4 – 3, 7 – 6, and 8 – 7 transitions were identified at 23123, 40465, and 46246 MHz, respectively. The //J// = 4 – 3, 7 – 6, and 8 – 7 transitions were identified at 23123, 40465, and 46246 MHz, respectively.
Line 29: Line 31:
 C<sub>2</sub>S, along with C<sub>3</sub>S, were also detected with the IRAM 30 m telescope in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216 in the course of a molecular line survey in the 3 and 2 mm regions by\\ C<sub>2</sub>S, along with C<sub>3</sub>S, were also detected with the IRAM 30 m telescope in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216 in the course of a molecular line survey in the 3 and 2 mm regions by\\
 J. Cernicharo, M. Guélin, H. Hein, and C. Kahane,\\ J. Cernicharo, M. Guélin, H. Hein, and C. Kahane,\\
-**[[http://cdsads.u-strasbg.fr/abs/1987A%26A...181L...9C|Sulfur in IRC +10216]]**\\ +**[[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\\ C<sub>2</sub>S was also seen toward several translucent clouds, albeit in only the lower energy transition of two by\\
 B. E. Turner, H.-H. Lee, and E. Herbst,\\ B. E. Turner, H.-H. Lee, and E. Herbst,\\
-**[[http://dx.doi.org/10.1086/313077|The Physics and Chemistry of Small Translucent Molecular Clouds.\\+**[[https://doi.org/10.1086/313077|The Physics and Chemistry of Small Translucent Molecular Clouds.\\
 IX. Acetylenic Chemistry]]**\\ 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\\ The two <sup>13</sup>C isotopomers were detected with the Nobeyama 45 m telescope toward TMC-1 by\\
Line 48: Line 52:
 C<sub>3</sub>S, along with C<sub>2</sub>S, were also detected with the IRAM 30 m telescope in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216 in the course of a molecular line survey in the 3 and 2 mm region by\\ C<sub>3</sub>S, along with C<sub>2</sub>S, were also detected with the IRAM 30 m telescope in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216 in the course of a molecular line survey in the 3 and 2 mm region by\\
 J. Cernicharo, M. Guélin, H. Hein, and C. Kahane,\\ J. Cernicharo, M. Guélin, H. Hein, and C. Kahane,\\
-**[[http://cdsads.u-strasbg.fr/abs/1987A%26A...181L...9C|Sulfur in IRC +10216]]**\\+**[[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).
  
 The detection of the <sup>34</sup>S isotopolog in the course of the Nobeyama 45 m line survey was mentioned first by\\ The detection of the <sup>34</sup>S isotopolog in the course of the Nobeyama 45 m line survey was mentioned first by\\
 M. Ohishi and N. Kaifu,\\ M. Ohishi and N. Kaifu,\\
-**[[http://dx.doi.org/10.1039/a801058g|Chemical and Physical Evolution of Dark Clouds. Molecular Spectral Line Survey toward TMC-1]]**\\+**[[https://doi.org/10.1039/a801058g|Chemical and Physical Evolution of Dark Clouds. Molecular Spectral Line Survey toward TMC-1]]**\\
 //Faraday Discuss.// **190**, 205–216 (1998). //Faraday Discuss.// **190**, 205–216 (1998).
  
 C<sub>3</sub>S was deteceted very recently in a warm cloud by\\ C<sub>3</sub>S was deteceted very recently in a warm cloud by\\
 B. Tercero, J. Cernicharo, J. R. Pardo, and J. R. Goicoechea,\\ B. Tercero, J. Cernicharo, J. R. Pardo, and J. R. Goicoechea,\\
-**[[http://dx.doi.org/10.1051/0004-6361/200913501|A line confusion limited millimeter survey of Orion KL\\+**[[https://doi.org/10.1051/0004-6361/200913501|A line confusion limited millimeter survey of Orion KL\\
 I. Sulfur carbon chains]]**\\ I. Sulfur carbon chains]]**\\
 //Astron. Astrophys.// **517**, Art. No. A96 (2010). //Astron. Astrophys.// **517**, Art. No. A96 (2010).
Line 71: Line 75:
 M. Agúndez, J. Cernicharo, and M. Guélin\\ M. Agúndez, J. Cernicharo, and M. Guélin\\
 reported on\\ reported on\\
-**[[http://dx.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]]**\\+**[[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).\\ //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. Thereforewe suggest to view the identification of C<sub>5</sub>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 moleculeshere C<sub>5</sub>and C<sub>3</sub>S, are very unusual, though not unprecedented.\\ 
 +\\
  
 M. B. Bell, L. W. Avery, and P. A. Feldman\\ M. B. Bell, L. W. Avery, and P. A. Feldman\\
 had reported on\\ had reported on\\
-**[[http://cdsads.u-strasbg.fr/abs/1993ApJ...417L..37B|C<sub>3</sub>S and C<sub>5</sub>S in IRC +10216]]**\\+**[[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).\\ //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>Sand larger molecules C<sub>n</sub>S, with n ≥ 6have not been detected in space thus far.+J. CernicharoC. 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 blendedone 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
  
  
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