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molecules:ism:c2_3s [2019/05/09 12:43] – [Additional information on C2S] mueller | molecules:ism:c2_3s [2021/12/20 12:47] – [Thioxoethenylidene, C2S, and Thioxopropadienylidene, C3S] 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.\\ |
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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.\\ |
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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. |
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). |
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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). |
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). |
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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). |
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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). |
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. 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.\\ |
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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.\\ |
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| 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.\\ |
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==== Information on C4S and larger species ==== | ==== Information on C4S ==== |
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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. |
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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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