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| ===== Detections of Metal Isocyanides and Metal Cyanides in Circumstellar Envelopes ===== | ===== Detections of Metal Isocyanides and Metal Cyanides in Circumstellar Envelopes ===== |
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| **Magnesium isocyanide**, **MgNC**, is a linear radical which is lower in energy than its MgCN isomer. It was observed first as an unidentified species in the circumstellar envelope of the famous carbon star CW Leo, also known as IRC +10216, by\\ | ==== MgNC ==== |
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| | **Magnesium isocyanide** is a linear radical which is lower in energy than its MgCN isomer. It was observed first as an unidentified species in the circumstellar envelope of the famous carbon star CW Leo, also known as IRC +10216, by\\ |
| M. Guélin, J. Cernicharo, C. Kahane, E. González-Alfonso,\\ | M. Guélin, J. Cernicharo, C. Kahane, E. González-Alfonso,\\ |
| **[[http://adsabs.harvard.edu/abs/1986A%26A...157L..17G|A New Free Radical in IRC +10216]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1986A%26A...157L..17G|A New Free Radical in IRC +10216]]**\\ |
| //Astron. Astrophys.// **157**, L17–L20 (1986).\\ | //Astron. Astrophys.// **157**, L17–L20 (1986).\\ |
| The authors detected in the 3 mm region both strong fine structure components of the //N"// = 6, 7, and 8 transitions. The authors proposed as most likely carriers HSiCC, its isomer HCCSi, or HSCC. | The authors detected in the 3 mm region both strong fine structure components of the //N"// = 6, 7, and 8 transitions. The authors proposed as most likely carriers HSiCC, its isomer HCCSi, or HSCC. |
| The molecule was identified few years later as MgNC via masurement of its rotational spectrum by:\\ | The molecule was identified few years later as MgNC via masurement of its rotational spectrum by:\\ |
| K. Kawaguchi, E. Kagi, T. Hirano, S. Takano, S. Saito,\\ | K. Kawaguchi, E. Kagi, T. Hirano, S. Takano, S. Saito,\\ |
| **[[http://adsabs.harvard.edu/abs/1993ApJ...406L..39K|Laboratory Spectroscopy of MgNC – The First Radioastronomical Identification of Mg-bearing Molecule]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1993ApJ...406L..39K|Laboratory Spectroscopy of MgNC – The First Radioastronomical Identification of Mg-bearing Molecule]]**\\ |
| //Astrophys. J.// **406**, L39–L42 (1993). | //Astrophys. J.// **406**, L39–L42 (1993). |
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| Besides the main isotope of Mg with the mass number 24, there are two stable isotopes with mass numbers 25 and 26, respectively. The corresponding isotopologs have both been detected toward CW Leo by:\\ | Besides the main isotope of Mg with the mass number 24, there are two stable isotopes with mass numbers 25 and 26, respectively. The corresponding isotopologs have both been detected toward CW Leo by:\\ |
| M. Guélin, M. Forstini, P. Valiron, L. M. Ziurys, M. A. Anderson, J. Cernicharo, and C. Kahane,\\ | M. Guélin, M. Forstini, P. Valiron, L. M. Ziurys, M. A. Anderson, J. Cernicharo, and C. Kahane,\\ |
| **[[http://adsabs.harvard.edu/abs/1995A%26A...297..183G|Nucleosynthesis in AGB Stars: Observation of <sup>25</sup>Mg and <sup>26</sup>Mg in IRC +10216 and Possible Detection of <sup>26</sup>Al]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1995A%26A...297..183G|Nucleosynthesis in AGB Stars: Observation of <sup>25</sup>Mg and <sup>26</sup>Mg in IRC +10216 and Possible Detection of <sup>26</sup>Al]]**\\ |
| //Astron. Astrophys.// **297**, 183–196 (1995).\\ | //Astron. Astrophys.// **297**, 183–196 (1995).\\ |
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| More recently, MgNC was also detected toward the protoplanetary nebula (PPN) CRL 2688, the egg nebula:\\ | More recently, MgNC was also detected toward the protoplanetary nebula (PPN) CRL 2688, the egg nebula:\\ |
| J. L. Highberger, C. Savage, J. H. Bieging, L. M. Ziurys,\\ | J. L. Highberger, C. Savage, J. H. Bieging, L. M. Ziurys,\\ |
| **[[http://dx.doi.org/10.1086/323231|Heavy-Metal Chemistry in Proto-Planetary Nebulae:\\ | **[[https://doi.org/10.1086/323231|Heavy-Metal Chemistry in Proto-Planetary Nebulae:\\ |
| Detection of MgNC, NaCN, and AlF toward CRL 2688]]**\\ | Detection of MgNC, NaCN, and AlF toward CRL 2688]]**\\ |
| //Astrophys. J.// **562**, 790–798 (2001). | //Astrophys. J.// **562**, 790–798 (2001). |
| ---- | ---- |
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| **Sodium cyanide**, **NaCN**, is a nearly T-shaped molecule. It possesses a NaN bond that is slightly shorther than the NaC bond. Therefore, the molecule should be considered more appropriately as sodium **iso**cyanide, NaNC. It was observed first in the circumstellar envelope of CW Leo in four //K<sub>a</sub>// = 0 transitions by\\ | ==== NaCN ==== |
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| | **Sodium cyanide** is a nearly T-shaped molecule. It possesses a NaN bond that is slightly shorther than the NaC bond. Therefore, the molecule should be considered more appropriately as sodium **iso**cyanide, NaNC. It was observed first in the circumstellar envelope of CW Leo in four //K<sub>a</sub>// = 0 transitions by\\ |
| B. E. Turner, T. C. Steimle, and L. Meerts,\\ | B. E. Turner, T. C. Steimle, and L. Meerts,\\ |
| **[[http://adsabs.harvard.edu/abs/1994ApJ...426L..97T|Detection of Sodium Cyanide (NaCN) in IRC+10216]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1994ApJ...426L..97T|Detection of Sodium Cyanide (NaCN) in IRC+10216]]**\\ |
| //Astrophys. J.// **426**, 97–100 (1994).\\ | //Astrophys. J.// **426**, 97–100 (1994).\\ |
| The //J"// = 4, 5, and 6 transitions are in the 3 mm region, the one with //J"// = 8 is in the 2 mm region. **Note:** in that paper the assumed dipole moment was too low by a factor of about 2.5 because an //ab initio// dipole moment was taken as being in units of Debye whereas it actually was given in atomic units. 1 au equals 2.542 D. | The //J"// = 4, 5, and 6 transitions are in the 3 mm region, the one with //J"// = 8 is in the 2 mm region. **Note:** in that paper the assumed dipole moment was too low by a factor of about 2.5 because an //ab initio// dipole moment was taken as being in units of Debye whereas it actually was given in atomic units. 1 au equals 2.542 D. |
| NaCN too was detected toward the PPN CRL 2688:\\ | NaCN too was detected toward the PPN CRL 2688:\\ |
| J. L. Highberger, C. Savage, J. H. Bieging, L. M. Ziurys,\\ | J. L. Highberger, C. Savage, J. H. Bieging, L. M. Ziurys,\\ |
| **[[http://dx.doi.org/10.1086/323231|Heavy-Metal Chemistry in Proto-Planetary Nebulae:\\ | **[[https://doi.org/10.1086/323231|Heavy-Metal Chemistry in Proto-Planetary Nebulae:\\ |
| Detection of MgNC, NaCN, and AlF toward CRL 2688]]**\\ | Detection of MgNC, NaCN, and AlF toward CRL 2688]]**\\ |
| //Astrophys. J.// **562**, 790–798 (2001). | //Astrophys. J.// **562**, 790–798 (2001). |
| ---- | ---- |
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| The **magnesium cyanide** isomer, **MgCN**, was detected in three transitions with //N"// = 8, 9, and 10, all lying in the 3 mm region, by:\\ | ==== MgCN ==== |
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| | The **magnesium cyanide** isomer was detected in three transitions with //N"// = 8, 9, and 10, all lying in the 3 mm region, by:\\ |
| L. M. Ziurys, A. J. Apponi, M. Guélin, and J. Cernicharo,\\ | L. M. Ziurys, A. J. Apponi, M. Guélin, and J. Cernicharo,\\ |
| **[[http://adsabs.harvard.edu/abs/1995ApJ...445L..47Z|Detection of MgCN in IRC +10216: A New Metal-bearing Free Radical]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1995ApJ...445L..47Z|Detection of MgCN in IRC +10216: A New Metal-bearing Free Radical]]**\\ |
| //Astrophys. J.// **445**, L47–L50 (1995). | //Astrophys. J.// **445**, L47–L50 (1995). |
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| ---- | ---- |
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| **Aluminum isocyanide**, **AlNC**, is a linear molecule which is lower in energy than its AlCN isomer. It was observed in five transitions (//J"// = 10, 11, and 12 in the 2 mm region and //J"// = 17 and 20 in the 1 mm region) toward CW Leo by:\\ | ==== AlNC ==== |
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| | **Aluminum isocyanide** is a linear molecule which is lower in energy than its AlCN isomer. It was observed in five transitions (//J"// = 10, 11, and 12 in the 2 mm region and //J"// = 17 and 20 in the 1 mm region) toward CW Leo by:\\ |
| L. M. Ziurys, C. Savage, J. L. Highberger, A. J. Apponi, M. Guélin, and J. Cernicharo,\\ | L. M. Ziurys, C. Savage, J. L. Highberger, A. J. Apponi, M. Guélin, and J. Cernicharo,\\ |
| **[[http://dx.doi.org/10.1086/338775|More Metal Cyanide Species: Detection of AlNC (X <sup>1</sup>Σ<sup>+</sup>) toward IRC +10216]]**\\ | **[[https://doi.org/10.1086/338775|More Metal Cyanide Species: Detection of AlNC (X <sup>1</sup>Σ<sup>+</sup>) toward IRC +10216]]**\\ |
| //Astrophys. J.// **564**, L45–L48 (2002). | //Astrophys. J.// **564**, L45–L48 (2002). |
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| ---- | ---- |
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| **Potassium cyanide**, **KCN**, is a nearly T-shaped molecule, just as NaCN. It too should be considered as an isocyanide rather than a cyanide. Several transitions in the 3, 2, and 1 mm region were detected toward CW Leo by:\\ | ==== KCN ==== |
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| | **Potassium cyanide** is a nearly T-shaped molecule, just as NaCN. It too should be considered as an isocyanide rather than a cyanide. Several transitions in the 3, 2, and 1 mm region were detected toward CW Leo by:\\ |
| R. L. Pulliam, C. Savage, M. Agúndez, J. Cernicharo, M. Guélin, and L. M. Ziurys,\\ | R. L. Pulliam, C. Savage, M. Agúndez, J. Cernicharo, M. Guélin, and L. M. Ziurys,\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/725/2/L181|Identification of KCN in IRC +10216: Evidence for Selective Cyanide Chemistry]]**\\ | **[[https://doi.org/10.1088/2041-8205/725/2/L181|Identification of KCN in IRC +10216: Evidence for Selective Cyanide Chemistry]]**\\ |
| //Astrophys. J.// **725**, L181–L185 (2010). | //Astrophys. J.// **725**, L181–L185 (2010). |
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| ---- | ---- |
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| **Iron cyanide**, **FeCN**, is a linear molecule. According to laboratory spectroscopic work, it actually is lowein in energy than iron isocyanide, FeNC. The molecule has a <sup>4</sup>Δ<sub>i</sub> ground state with considerable spin-orbit splitting. The Ω = 7/2 spin component is lowest in energy. Three apparently clean transitions with //J"// = 9.5, 11.5, and 12.5 as well as two partially overlapped transitions (10.5 and 15.5) were detected with the ARO 12 m radio-telescope toward CW Leo by:\\ | ==== FeCN ==== |
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| | **Iron cyanide** is a linear molecule. According to laboratory spectroscopic work, it actually is lowein in energy than iron isocyanide, FeNC. The molecule has a <sup>4</sup>Δ<sub>i</sub> ground state with considerable spin-orbit splitting. The Ω = 7/2 spin component is lowest in energy. Three apparently clean transitions with //J"// = 9.5, 11.5, and 12.5 as well as two partially overlapped transitions (10.5 and 15.5) were detected with the ARO 12 m radio-telescope toward CW Leo by:\\ |
| L. N. Zack, D. T. Halfen, and L. M. Ziurys,\\ | L. N. Zack, D. T. Halfen, and L. M. Ziurys,\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/733/2/L36|Detection of FeCN (//X// <sup>4</sup>Δ<sub>i</sub>) in IRC +10216: A New Interstellar Molecule]]**\\ | **[[https://doi.org/10.1088/2041-8205/733/2/L36|Detection of FeCN (//X// <sup>4</sup>Δ<sub>i</sub>) in IRC +10216: A New Interstellar Molecule]]**\\ |
| //Astrophys. J.// **733**, Art. No. L36 (2011). | //Astrophys. J.// **733**, Art. No. L36 (2011). |
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| Contributor(s): H. S. P. Müller; 09, 2005; 04, 2007; 04, 2011; 05, 2011 | Contributor(s): H. S. P. Müller; 09, 2005; 04, 2007; 04, 2011; 05, 2011 |
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