molecules:ism:sio

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revision Previous revision
Next revision		 Previous revision
molecules:ism:sio [2019/10/18 12:56] – muellermolecules:ism:sio [2026/08/25 10:17] (current) – mueller
Line 11: Line 11:
 **[[https://ui.adsabs.harvard.edu/abs/1972ApJ...175L..43D|Detection of Silicon Monoxide at 87 GHz]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1972ApJ...175L..43D|Detection of Silicon Monoxide at 87 GHz]]**\\
 //Astrophys. J.// **175**, L43–L100 (1972).\\ //Astrophys. J.// **175**, L43–L100 (1972).\\
-The 11 m Kitt Peak telescope was used to detect the line toward Sgr B2(OH) and Orion A.+The 11 m Kitt Peak telescope was used to detect the line toward Sgr B2(OH) and Orion A.\\ 
 +\\
  
 P. Schilke, G. Pineau des Forêts, C. M. Walmsley, and J. Martín-Pintado\\ P. Schilke, G. Pineau des Forêts, C. M. Walmsley, and J. Martín-Pintado\\
Line 17: Line 18:
 **[[https://doi.org/10.1051/0004-6361:20010470|Observations of SiO towards Photon Dominated Regions]]**\\ **[[https://doi.org/10.1051/0004-6361:20010470|Observations of SiO towards Photon Dominated Regions]]**\\
 //Astron. Astrophys.// **372**, 291–301 (2001).\\ //Astron. Astrophys.// **372**, 291–301 (2001).\\
-The IRAM 30 m telecope was used to detect several SiO transitions toward the Orion Bar and S 140.+The IRAM 30 m telecope was used to detect several SiO transitions toward the Orion Bar and S 140.\\ 
 +\\
  
 S. Yamamoto, H. Mikami, S. Saito, N. Kaifu, M. Ohishi, and K. Kawaguchi\\ S. Yamamoto, H. Mikami, S. Saito, N. Kaifu, M. Ohishi, and K. Kawaguchi\\
Line 23: Line 25:
 **[[https://ui.adsabs.harvard.edu/abs/1992PASJ...44..459Y|SiO in Barnard 1]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1992PASJ...44..459Y|SiO in Barnard 1]]**\\
 //Publs. Astron. Soc. Japan// **167**, L97–L100 (1971),\\ //Publs. Astron. Soc. Japan// **167**, L97–L100 (1971),\\
-a low-mass star-forming region.+a low-mass star-forming region.\\ 
 +\\
  
 The molecule is conspicuously absent in cold, quiescent molecular clouds, as reported by\\ The molecule is conspicuously absent in cold, quiescent molecular clouds, as reported by\\
Line 33: Line 36:
 view\\ view\\
 **[[https://ui.adsabs.harvard.edu/abs/1992A%26A...254..315M|SiO Emission as a Tracer of Shocked Gas in Molecular Outflows]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1992A%26A...254..315M|SiO Emission as a Tracer of Shocked Gas in Molecular Outflows]]**\\
-//Astron. Astrophys.// **254**, 315–326 (1992).+//Astron. Astrophys.// **254**, 315–326 (1992).\\ 
 +\\
  
 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.\\
Line 43: Line 47:
 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.\\ 
 +\\
  
 D. Buhl, L. E. Snyder, F. J. Lovas, and D. R. Johnson\\ D. Buhl, L. E. Snyder, F. J. Lovas, and D. R. Johnson\\
Line 51: Line 56:
 **[[https://ui.adsabs.harvard.edu/abs/1974ApJ...192L..97B|Silicon Monoxide: Detection of Maser Emission from the Second Vibrationally Excited State]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1974ApJ...192L..97B|Silicon Monoxide: Detection of Maser Emission from the Second Vibrationally Excited State]]**\\
 //Astrophys. J.// **192**, L97–L100 (1974).\\ //Astrophys. J.// **192**, L97–L100 (1974).\\
-Half of the authors are laboratory spectroscopists, thus highlighting the crucial importance for radio astronomical observations.+Half of the authors are laboratory spectroscopists, thus highlighting the crucial importance for radio astronomical observations.\\ 
 +\\
  
 T. Kaminski, C. A. Gottlieb, K. H. Young, K. M. Menten, and N. A. Patel\\ T. Kaminski, C. A. Gottlieb, K. H. Young, K. M. Menten, and N. A. Patel\\
Line 57: Line 63:
 **[[https://doi.org/10.1088/0067-0049/209/2/38|An Interferometric Spectral Line and Imaging Survey of VY Canis Majoris in the 345 GHz Band]]**\\ **[[https://doi.org/10.1088/0067-0049/209/2/38|An Interferometric Spectral Line and Imaging Survey of VY Canis Majoris in the 345 GHz Band]]**\\
 //Astrophys. J. Suppl. Ser.// **209**, Art. No. 38 (2013),\\ //Astrophys. J. Suppl. Ser.// **209**, Art. No. 38 (2013),\\
-and detected a //v// = 5 SiO maser.+and detected a //v// = 5 SiO maser.\\ 
 +\\ 
 + 
 +B. Pimpanuwat, S. Etoka, M. D. Gray, A. M. S. Richards, A. Baudry, F. Herpin, T. Danilovich, L. Decin, M. O. Lewis, I. El Mellah, C. A. Gottlieb, Y. Mori, H. S. P. Müller, R. Sahai, K. T. Wong, J. A. Yates, and A. Zijlstra\\ 
 +published on\\ 
 +**[[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).\\ 
 +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.\\ 
 +\\
  
 E. Gonzalez-Alfonso, J. Alcolea, and J. Cernicharo\\ E. Gonzalez-Alfonso, J. Alcolea, and J. Cernicharo\\
 reported on the\\ reported on the\\
 **[[https://ui.adsabs.harvard.edu/abs/1996A%26A...313L..13G|Detection of <sup>29</sup>SiO //v// = 3 //J// = 8 → 7 Maser Emission: a new IR SiO Overlap]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1996A%26A...313L..13G|Detection of <sup>29</sup>SiO //v// = 3 //J// = 8 → 7 Maser Emission: a new IR SiO Overlap]]**\\
-//Astron. Astrophys.// **313**, L13–L16 (1996).+//Astron. Astrophys.// **313**, L13–L16 (1996).\\ 
 +\\
  
 S.-H. Cho, H.-G. Kim, Y.-S. Park, C.-H. Choi, and N. Ukita\\ S.-H. Cho, H.-G. Kim, Y.-S. Park, C.-H. Choi, and N. Ukita\\
 reported on the\\ reported on the\\
 **[[https://doi.org/10.1086/426585|First Detection of <sup>28</sup>Si<sup>18</sup>O Maser and Thermal Emission from Orion KL]]**\\ **[[https://doi.org/10.1086/426585|First Detection of <sup>28</sup>Si<sup>18</sup>O Maser and Thermal Emission from Orion KL]]**\\
-//Astrophys. J.// **622**, 390–392 (2005).+//Astrophys. J.// **622**, 390–392 (2005).\\ 
 +\\
  
 L. Decin, J. Cernicharo, M. J. Barlow, et al.\\ L. Decin, J. Cernicharo, M. J. Barlow, et al.\\
Line 73: Line 105:
 **[[https://doi.org/10.1051/0004-6361/201014562|Silicon in the Dust Formation Zone of IRC +10216]]**\\ **[[https://doi.org/10.1051/0004-6361/201014562|Silicon in the Dust Formation Zone of IRC +10216]]**\\
 //Astron. Astrophys.// **518**, Art. No. L143 (2010).\\ //Astron. Astrophys.// **518**, Art. No. L143 (2010).\\
-Using the PACS low-resolution spectrometer on board of the //Herschel// satellite, they identified unblended SiO rotational transitions beyond 3 THz.+Using the PACS low-resolution spectrometer on board of the //Herschel// satellite, they identified unblended SiO rotational transitions beyond 3 THz.\\ 
 +\\
  
 The observation of <sup>28</sup>Si<sup>17</sup>O was reported by\\ The observation of <sup>28</sup>Si<sup>17</sup>O was reported by\\
Line 79: Line 112:
 in the course of\\ in the course of\\
 **[[https://doi.org/10.1051/0004-6361/201628776|The Millimeter IRAM-30m Line Survey toward IK Tauri]]**\\ **[[https://doi.org/10.1051/0004-6361/201628776|The Millimeter IRAM-30m Line Survey toward IK Tauri]]**\\
-//Astron. Astrophys.// **597**, Art. No. A25 (2017).+//Astron. Astrophys.// **597**, Art. No. A25 (2017).\\ 
 +\\
  
 L. Decin, A. M. S. Richards, T. Danilovich, W. Homan, and J. A. Nuth\\ L. Decin, A. M. S. Richards, T. Danilovich, W. Homan, and J. A. Nuth\\
Line 85: Line 119:
 **[[https://doi.org/10.1051/0004-6361/201732216|ALMA Spectral Line and Imaging Survey of a Low and a High Mass-loss Rate AGB Star between 335 and 362 GHz]]**\\ **[[https://doi.org/10.1051/0004-6361/201732216|ALMA Spectral Line and Imaging Survey of a Low and a High Mass-loss Rate AGB Star between 335 and 362 GHz]]**\\
 //Astron. Astrophys.// **615**, Art. No. A28 (2018).\\ //Astron. Astrophys.// **615**, Art. No. A28 (2018).\\
-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).\\
 +\\
  
----- 
  
-Contributor(s): H. S. P. Müller; 12, 2014; 10, 2018+----
  
 +Contributor(s): H. S. P. Müller; 12, 2014; 10, 2018; 07, 2026
  
 ---- ----
  
  
  • molecules/ism/sio.1571396215.txt.gz
  • Last modified: 2019/10/18 12:56
  • by mueller