molecules:ism:sio

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molecules:ism:sio [2019/02/25 22:38] – external edit 127.0.0.1molecules:ism:sio [2019/10/18 12:56] (current) – mueller
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 R. W. Wilson, A. A. Penzias, K. B. Jefferts, M. Kutner, and P. Thaddeus\\ R. W. Wilson, A. A. Penzias, K. B. Jefferts, M. Kutner, and P. Thaddeus\\
 reported on the\\ reported on the\\
-**[[http://cdsads.u-strasbg.fr/abs/1971ApJ...167L..97W|Discovery of Interstellar Silicon Monoxide]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1971ApJ...167L..97W|Discovery of Interstellar Silicon Monoxide]]**\\
 //Astrophys. J.// **167**, L97–L100 (1971).\\ //Astrophys. J.// **167**, L97–L100 (1971).\\
 The //J// = 3 – 2 transition of SiO near 130.2 GHz was detected in emission with the 11 m Kitt Peak telescope toward Sgr B2(OH).\\ The //J// = 3 – 2 transition of SiO near 130.2 GHz was detected in emission with the 11 m Kitt Peak telescope toward Sgr B2(OH).\\
 D. F. Dickinson\\ D. F. Dickinson\\
 reported on the\\ reported on the\\
-**[[http://cdsads.u-strasbg.fr/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.
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 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\\
 performed\\ performed\\
-**[[http://dx.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.
Line 21: Line 21:
 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\\
 detected\\ detected\\
-**[[http://cdsads.u-strasbg.fr/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.
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 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\\
 L. M. Ziurys, P. Friberg, and W. M. Irvine,\\ L. M. Ziurys, P. Friberg, and W. M. Irvine,\\
-**[[http://cdsads.u-strasbg.fr/abs/1989ApJ...343..201Z|Interstellar SiO as a Tracer of High-temperature Chemistry]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1989ApJ...343..201Z|Interstellar SiO as a Tracer of High-temperature Chemistry]]**\\
 //Astrophys. J.// **343**, 201–207 (1989).\\ //Astrophys. J.// **343**, 201–207 (1989).\\
 The absence of SiO was reported for TMC-1, L134N (aka L183) and for B335 (aka L663). Hence,\\ The absence of SiO was reported for TMC-1, L134N (aka L183) and for B335 (aka L663). Hence,\\
 J. Martin-Pintado, R. Bachiller, and A. Fuente\\ J. Martin-Pintado, R. Bachiller, and A. Fuente\\
 view\\ view\\
-**[[http://cdsads.u-strasbg.fr/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\\
-**[[http://cdsads.u-strasbg.fr/abs/1974ApJ...189L..31S|Detection of Possible Maser Emission Near 3.48 Millimeters from an Unidentified Molecular Species in Orion]]**\\+**[[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]]**\\
 //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 43:
 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\\
-**[[http://cdsads.u-strasbg.fr/abs/1974ApJ...189L..31S|Vibrationally Excited Silicon Monoxide in the Orion Nebula]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1974ApJ...189L..31S|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.
Line 49: Line 49:
 D. Buhl, L. E. Snyder, F. J. Lovas, and D. R. Johnson\\ D. Buhl, L. E. Snyder, F. J. Lovas, and D. R. Johnson\\
 reported subsequently on\\ reported subsequently on\\
-**[[http://cdsads.u-strasbg.fr/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.
Line 55: Line 55:
 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\\
 performed\\ performed\\
-**[[http://dx.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.
Line 61: Line 61:
 E. Gonzalez-Alfonso, J. Alcolea, and J. Cernicharo\\ E. Gonzalez-Alfonso, J. Alcolea, and J. Cernicharo\\
 reported on the\\ reported on the\\
-**[[http://cdsads.u-strasbg.fr/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\\
-**[[http://dx.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.\\
 investigated\\ investigated\\
-**[[http://dx.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.
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 L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, V. Bujarrabal, J. Alcolea, C. Balança, F. Herpin, K. M. Menten, and F. Wyrowski\\ L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, V. Bujarrabal, J. Alcolea, C. Balança, F. Herpin, K. M. Menten, and F. Wyrowski\\
 in the course of\\ in the course of\\
-**[[http://dx.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\\
 reported on an\\ reported on an\\
-**[[http://dx.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.
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