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| The first member of this group, not really qualifying for "poly", acetylene, HC<sub>2</sub>H, itself, was detected in absorption at Kitt Peak toward the circumstellar shell of CW Leo, aka IRC +10216. The unresolved //Q//-branch of the ν<sub>4</sub> + ν<sub>5</sub> band was detected at 4091.0 cm<sup>–1</sup> by:\\ | The first member of this group, not really qualifying for "poly", acetylene, HC<sub>2</sub>H, itself, was detected in absorption at Kitt Peak toward the circumstellar shell of CW Leo, aka IRC +10216. The unresolved //Q//-branch of the ν<sub>4</sub> + ν<sub>5</sub> band was detected at 4091.0 cm<sup>–1</sup> by:\\ |
| S. T. Ridgway, D. N. B. Hall, R. S. Wojslaw, S. G. Kleinmann, and D. A. Weinberger,\\ | S. T. Ridgway, D. N. B. Hall, R. S. Wojslaw, S. G. Kleinmann, and D. A. Weinberger,\\ |
| **[[http://dx.doi.org/10.1038/264345a0|Circumstellar Acetylene in the Infrared Spectrum of IRC +10<sup>o</sup>216]]**\\ | **[[https://doi.org/10.1038/264345a0|Circumstellar Acetylene in the Infrared Spectrum of IRC +10<sup>o</sup>216]]**\\ |
| //Nature// **264**, 345–346 (1976). | //Nature// **264**, 345–346 (1976). |
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| A brief account on the observation of the ν<sub>5</sub> band with an origin at 730.3 cm<sup>–1</sup> (or 13.7 μm) was given by:\\ | A brief account on the observation of the ν<sub>5</sub> band with an origin at 730.3 cm<sup>–1</sup> (or 13.7 μm) was given by:\\ |
| T. Kostiuk, F. Espenak, D. Deming, M. J. Mumma, D. Zipoy, and J. Keady,\\ | T. Kostiuk, F. Espenak, D. Deming, M. J. Mumma, D. Zipoy, and J. Keady,\\ |
| **[[http://adsabs.harvard.edu/abs/1985BAAS...17..570K|Study of Velocity Structure in IRC +10216 Using Acetylene Line Profiles]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1985BAAS...17..570K|Study of Velocity Structure in IRC +10216 Using Acetylene Line Profiles]]**\\ |
| //Bull. Am. Astron. Soc.// **17**, 570 (1985). | //Bull. Am. Astron. Soc.// **17**, 570 (1985). |
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| Hot band transitions associated with ν<sub>5</sub> band, i.e. ν<sub>4</sub> + ν<sub>5</sub> – ν<sub>4</sub> and 2ν<sub>5</sub> – ν<sub>5</sub>, were reported by:\\ | Hot band transitions associated with ν<sub>5</sub> band, i.e. ν<sub>4</sub> + ν<sub>5</sub> – ν<sub>4</sub> and 2ν<sub>5</sub> – ν<sub>5</sub>, were reported by:\\ |
| J. J. Keady and S. T. Ridgway,\\ | J. J. Keady and S. T. Ridgway,\\ |
| **[[http://adsabs.harvard.edu/abs/1993ApJ...406..199K|The IRC +10216 Circumstellar Envelope. III – Infrared Molecular Line Profiles]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1993ApJ...406..199K|The IRC +10216 Circumstellar Envelope. III – Infrared Molecular Line Profiles]]**\\ |
| //Astrophys. J.// **406**, 199–214 (1993). | //Astrophys. J.// **406**, 199–214 (1993). |
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| The molecule was also detected toward three IR sources embedded in molecular clouds with the NASA IRTF 3 m telescope. Two or three of the //R//(5), //R//(10), or the unresolved //Q//-branch of the ν<sub>5</sub> band were detected toward GL 2591, W3 IRS 5, and OMC-1 IRc2 by\\ | The molecule was also detected toward three IR sources embedded in molecular clouds with the NASA IRTF 3 m telescope. Two or three of the //R//(5), //R//(10), or the unresolved //Q//-branch of the ν<sub>5</sub> band were detected toward GL 2591, W3 IRS 5, and OMC-1 IRc2 by\\ |
| J. H. Lacy, N. J. Evans II, J. M. Achtermann, D. E. Bruce, J. F. Arens, and J. S. Carr,\\ | J. H. Lacy, N. J. Evans II, J. M. Achtermann, D. E. Bruce, J. F. Arens, and J. S. Carr,\\ |
| **[[http://adsabs.harvard.edu/abs/1989ApJ...342L..43L|Discovery of Interstellar Acetylene]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1989ApJ...342L..43L|Discovery of Interstellar Acetylene]]**\\ |
| //Astrophys. J.// **383**, 674–692 (1991). | //Astrophys. J.// **383**, 674–692 (1991). |
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| The observations were extended to more line of this band, to the same band of H<sup>13</sup>CCH, and to the ν<sub>4</sub> + ν<sub>5</sub> band at 7.6 μm toward OMC-1 using the same facility:\\ | The observations were extended to more line of this band, to the same band of H<sup>13</sup>CCH, and to the ν<sub>4</sub> + ν<sub>5</sub> band at 7.6 μm toward OMC-1 using the same facility:\\ |
| N. J. Evans II, J. H. Lacy, and J. S. Carr,\\ | N. J. Evans II, J. H. Lacy, and J. S. Carr,\\ |
| **[[http://adsabs.harvard.edu/abs/1991ApJ...383..674E|Infrared Molecular Spectroscopy toward the Orion IRc2 and IRc7 Sources – A new Probe of Physical Conditions and Abundances in Molecular Clouds]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1991ApJ...383..674E|Infrared Molecular Spectroscopy toward the Orion IRc2 and IRc7 Sources – A new Probe of Physical Conditions and Abundances in Molecular Clouds]]**\\ |
| //Astrophys. J.// **342**, L43–L46 (1989). | //Astrophys. J.// **342**, L43–L46 (1989). |
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| J. Cernicharo, A. M. Heras, A. G. G. M. Tielens, J. R. Pardo, F. Herpin, M. Guélin, and L. B. F. M. Waters,\\ | J. Cernicharo, A. M. Heras, A. G. G. M. Tielens, J. R. Pardo, F. Herpin, M. Guélin, and L. B. F. M. Waters,\\ |
| **[[http://dx.doi.org/10.1086/318871|//Infrared Space Observatory's// Discovery of C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>2</sub>, and Benzene in CRL 618]]**\\ | **[[https://doi.org/10.1086/318871|//Infrared Space Observatory's// Discovery of C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>2</sub>, and Benzene in CRL 618]]**\\ |
| //Astrophys. J.// **546**, L123–L126 (2001);\\ | //Astrophys. J.// **546**, L123–L126 (2001);\\ |
| report the detection of butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, employing mid-infrared absorption spectroscopy. The unresolved //Q//-branches of the cold ν<sub>8</sub> band of butadiyne along with hot bands were detected at 15.9 μm. Close by, at 16.1 μm, the //Q//-branch of ν<sub>11</sub> band of hexatriyne is seen. | report the detection of butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, employing mid-infrared absorption spectroscopy. The unresolved //Q//-branches of the cold ν<sub>8</sub> band of butadiyne along with hot bands were detected at 15.9 μm. Close by, at 16.1 μm, the //Q//-branch of ν<sub>11</sub> band of hexatriyne is seen. |
| A separate report;\\ | A separate report;\\ |
| J. Cernicharo, A. M. Heras, J. R. Pardo, A. G. G. M. Tielens, M. Guélin, E. Dartois, R. Neri, and L. B. F. M. Waters;\\ | J. Cernicharo, A. M. Heras, J. R. Pardo, A. G. G. M. Tielens, M. Guélin, E. Dartois, R. Neri, and L. B. F. M. Waters;\\ |
| **[[http://dx.doi.org/10.1086/318872|Methylpolyynes and Small Hydrocarbons in CRL 618]]**\\ | **[[https://doi.org/10.1086/318872|Methylpolyynes and Small Hydrocarbons in CRL 618]]**\\ |
| //Astrophys. J.// **546**, L127–L130 (2001);\\ | //Astrophys. J.// **546**, L127–L130 (2001);\\ |
| identifies one combination band each for butadiyne and hexatriyne. The spectrum around 8 μm is rather complex as is the model which contains many species. Inspection of laboratory spectroscopic literature is useful. A complex feature at almost exactly 8 μm is largely attributable to the strong, unresolved //R//-branch of ν<sub>6</sub> + ν<sub>8</sub> band of butadiyne. Features at 8.08 and 8.14 μm can be attributed to the unresolved //R//- and //P//-branches of the respective strong ν<sub>8</sub> + ν<sub>11</sub> band of hexatriyne, both overlapping the //P//-branch of the butadiyne band. | identifies one combination band each for butadiyne and hexatriyne. The spectrum around 8 μm is rather complex as is the model which contains many species. Inspection of laboratory spectroscopic literature is useful. A complex feature at almost exactly 8 μm is largely attributable to the strong, unresolved //R//-branch of ν<sub>6</sub> + ν<sub>8</sub> band of butadiyne. Features at 8.08 and 8.14 μm can be attributed to the unresolved //R//- and //P//-branches of the respective strong ν<sub>8</sub> + ν<sub>11</sub> band of hexatriyne, both overlapping the //P//-branch of the butadiyne band. |
| The spectral same region was also studied under high resolution by:\\ | The spectral same region was also studied under high resolution by:\\ |
| J. P. Fonfría, J. Cernicharo, M. J. Richter, J. H. Lacy,\\ | J. P. Fonfría, J. Cernicharo, M. J. Richter, J. H. Lacy,\\ |
| **[[http://dx.doi.org/10.1088/0004-637X/728/1/43|The Abundances of Polyacetylenes towards CRL618]]**\\ | **[[https://doi.org/10.1088/0004-637X/728/1/43|The Abundances of Polyacetylenes towards CRL618]]**\\ |
| //Astrophys. J.// **728**, Art. No. 43 (2011),\\ | //Astrophys. J.// **728**, Art. No. 43 (2011),\\ |
| revealing clear evidence for several hot bands associated with these rather strong combination bands.\\ | revealing clear evidence for several hot bands associated with these rather strong combination bands.\\ |
| Earlier, the two fundamental vibrations ν<sub>8</sub> of butadiyne at 15.9 μm and of ν<sub>11</sub> of hexatriyne at 16.1 μm, see also above, were observed toward a Nova like star by\\ | Earlier, the two fundamental vibrations ν<sub>8</sub> of butadiyne at 15.9 μm and of ν<sub>11</sub> of hexatriyne at 16.1 μm, see also above, were observed toward a Nova like star by\\ |
| A. Evans, V. H. Tyne, J. Th. van Loon, B. Smalley, T. R. Geballe, R. D. Gehrz, C. E. Woodward, A. A. Zijlstra, E. Polomski, M. T. Rushton, S. P. S. Eyres, S. G. Starrfield, J. Krautter, and R. M. Wagner,\\ | A. Evans, V. H. Tyne, J. Th. van Loon, B. Smalley, T. R. Geballe, R. D. Gehrz, C. E. Woodward, A. A. Zijlstra, E. Polomski, M. T. Rushton, S. P. S. Eyres, S. G. Starrfield, J. Krautter, and R. M. Wagner,\\ |
| **[[http://dx.doi.org/10.1111/j.1745-3933.2006.00246.x|The //Spitzer// Infrared Spectrometer View of V4334 Sgr (Sakurai’s Object)]]**\\ | **[[https://doi.org/10.1111/j.1745-3933.2006.00246.x|The //Spitzer// Infrared Spectrometer View of V4334 Sgr (Sakurai’s Object)]]**\\ |
| //Mon. Not. R. Astron. Soc.// **373**, L75–L79 (2006). | //Mon. Not. R. Astron. Soc.// **373**, L75–L79 (2006). |
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| Contributor(s): H. S. P. Müller; 10, 2003; 01, 2011; 06, 2011 | Contributor(s): H. S. P. Müller; 10, 2003; 01, 2011; 06, 2011 |
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