molecules:ism:sio

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molecules:ism:sio [2026/07/29 12:37] – muellermolecules:ism:sio [2026/08/25 10:17] (current) – mueller
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 L. E. Snyder and D. Buhl\\ L. E. Snyder and D. Buhl\\
 proposed the\\ proposed the\\
-**[[https://ui.adsabs.harvard.edu/abs/1974ApJ...189L..31S|Detection of Possible Maser Emission Near 3.48 Millimeters from an Unidentified Molecular Species in Orion]]**\\+**[[https://doi.org/10.1093/10.1086/181457|Detection of Possible Maser Emission Near 3.48 Millimeters from an Unidentified Molecular Species in Orion]]**\\
 //Astrophys. J.// **189**, L31–L33 (1974).\\ //Astrophys. J.// **189**, L31–L33 (1974).\\
 Orion A was observed with the 11 m Kitt Peak telescope. The frequency coincidence with the //J// = 2 – 1 transition of SiO in its first excited vibrational state was noted.\\ Orion A was observed with the 11 m Kitt Peak telescope. The frequency coincidence with the //J// = 2 – 1 transition of SiO in its first excited vibrational state was noted.\\
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 J. H. Davis, G. N. Blair, H. van Till, and P. Thaddeus,\\ J. H. Davis, G. N. Blair, H. van Till, and P. Thaddeus,\\
 who studied\\ who studied\\
-**[[https://ui.adsabs.harvard.edu/abs/1974ApJ...189L..31S|Vibrationally Excited Silicon Monoxide in the Orion Nebula]]**\\+**[[https://doi.org/10.1093/10.1086/181520|Vibrationally Excited Silicon Monoxide in the Orion Nebula]]**\\
 //Astrophys. J.// **190**, L117–L119 (1974).\\ //Astrophys. J.// **190**, L117–L119 (1974).\\
 They observed the //J// = 3 – 2 transition of SiO.\\ They observed the //J// = 3 – 2 transition of SiO.\\
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 **[[https://doi.org/10.1093/mnras/stag888|ATOMIUM: Inner Circumstellar Envelopes of Oxygen-Rich AGB Stars as Revealed by Highly Excited SiO Lines]]**\\ **[[https://doi.org/10.1093/mnras/stag888|ATOMIUM: Inner Circumstellar Envelopes of Oxygen-Rich AGB Stars as Revealed by Highly Excited SiO Lines]]**\\
 //Mon. Not. R. Astron. Soc.// **549**, Art. No. stag888 (2026).\\ //Mon. Not. R. Astron. Soc.// **549**, Art. No. stag888 (2026).\\
-and detected a //v// = 5 SiO maser.\\+SiO //v// = 8 //J// = 6 − 5 was detected possibly (meaning 3.0 ≲ S/N ≲ 5.0) in emission toward R Hya and in absorption toward S Pav and R Aql.\\ 
 +\\ 
 +---- 
 + 
 +Employing the NRAO 11 m dish,\\ 
 +F.J. Lovas, D.R. Johnson, D. Buhl, and L.E. Snyder\\ 
 +identified\\ 
 +**[[https://doi.org/10.1086/154774|Millimeter emission lines in Orion A]]**\\ 
 +//Astrophys. J.// **209**, 770–777 (1976).\\ 
 +Among them was the //J// = 2 − 1 transition of <sup>29</sup>SiO. The <sup>28</sup>Si/<sup>29</sup>Si ratio is 17.5 ± 5, consistent with the terrestrial ratio of 19.6.\\ 
 +\\ 
 + 
 +F.O. Clark and F.J. Lovas\\ 
 +detected similarly\\ 
 +**[[https://doi.org/10.1086/182536|<sup>30</sup>SiO in the interstellar medium]]**\\ 
 +//Astrophys. J.// **217**, L47–L48 (1977).\\ 
 +The isotopolog was detected toward Orion A and Sgr B2. The <sup>28</sup>Si/<sup>30</sup>Si ratio is 32 ± 8, concordant  with the terrestrial ratio of 29.8. The line of the SiO main species displayed a double peak, suggestive of opacity or foreground absorption, preventing an isotopic ratio to be determined.\\
 \\ \\
  
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 The low mass-loss star was R Dor, the high mass-loss star was IK Tau. The very sensitive data permitted detection of <sup>29</sup>Si<sup>18</sup>O and <sup>30</sup>Si<sup>18</sup>O.\\ The low mass-loss star was R Dor, the high mass-loss star was IK Tau. The very sensitive data permitted detection of <sup>29</sup>Si<sup>18</sup>O and <sup>30</sup>Si<sup>18</sup>O.\\
 \\ \\
 +
 +B. Pimpanuwat et al. (see above)\\
 +also report detections of <sup>30</sup>SiO //v// = 4 and 5 //J// = 6 − 5 toward R Hya and one or possibly toward three further sources, as well as possibly <sup>29</sup>SiO //v// = 6 //J// = 6 − 5 toward R Hya.\\
 +**[[https://doi.org/10.1093/mnras/stag888|ATOMIUM: Inner Circumstellar Envelopes of Oxygen-Rich AGB Stars as Revealed by Highly Excited SiO Lines]]**\\
 +//Mon. Not. R. Astron. Soc.// **549**, Art. No. stag888 (2026).\\
 +\\
 +
  
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-Contributor(s): H. S. P. Müller; 12, 2014; 10, 2018+Contributor(s): H. S. P. Müller; 12, 2014; 10, 2018; 07, 2026
  
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