molecules:ism:cf-plus

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molecules:ism:cf-plus [2019/02/25 22:38] – external edit 127.0.0.1molecules:ism:cf-plus [2019/10/18 13:02] (current) – mueller
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 Fluoromethylidynium, CF<sup>+</sup>, may seem like an odd molecule. However, it is isoelectronic to CO with a similar rotational constant, but a dipole moment that is about ten times larger. Its detection toward the PDR Orion-Bar was reported by\\ Fluoromethylidynium, CF<sup>+</sup>, may seem like an odd molecule. However, it is isoelectronic to CO with a similar rotational constant, but a dipole moment that is about ten times larger. Its detection toward the PDR Orion-Bar was reported by\\
 D. A. Neufeld, P. Schilke, K. M. Menten, M. G. Wolfire, J. H. Black, F. Schuller, H. S. P. Müller, S. Thorwirth, R. Güsten, and S. Philipp,\\ D. A. Neufeld, P. Schilke, K. M. Menten, M. G. Wolfire, J. H. Black, F. Schuller, H. S. P. Müller, S. Thorwirth, R. Güsten, and S. Philipp,\\
-**[[http://dx.doi.org/10.1051/0004-6361:200600015|Discovery of Interstellar CF<sup>+</sup>]]**\\+**[[https://doi.org/10.1051/0004-6361:200600015|Discovery of Interstellar CF<sup>+</sup>]]**\\
 //Astron. Astrophys.// **454**, L37–L40 (2006).\\ //Astron. Astrophys.// **454**, L37–L40 (2006).\\
 The //J// = 1 – 0 and 2 – 1 transitions were detected with the IRAM 30 m telescope at 102.6 and 205.2 GHz, respectively, as well as the 3 – 2 transition with the APEX 12 m dish at 307.7 GHz. The //J// = 1 – 0 and 2 – 1 transitions were detected with the IRAM 30 m telescope at 102.6 and 205.2 GHz, respectively, as well as the 3 – 2 transition with the APEX 12 m dish at 307.7 GHz.
  
 The //J// = 1 – 0 transition was also detected in two 3 mm molecular line surveys carried out with the 20 m OSO telescope:\\ The //J// = 1 – 0 transition was also detected in two 3 mm molecular line surveys carried out with the 20 m OSO telescope:\\
-**[[http://dx.doi.org/10.1134/S1063772910040037|Spectral scan of the star-forming region DR21(OH). Observations and LTE analysis]]**\\+**[[https://doi.org/10.1134/S1063772910040037|Spectral scan of the star-forming region DR21(OH). Observations and LTE analysis]]**\\
 //Astron. Rep.// **54**, 295–316 (2010);\\ //Astron. Rep.// **54**, 295–316 (2010);\\
-**[[http://dx.doi.org/10.1134/S1063772910120036|Spectral survey of the star-forming region W51 e1/e2 at 3 mm]]**\\+**[[https://doi.org/10.1134/S1063772910120036|Spectral survey of the star-forming region W51 e1/e2 at 3 mm]]**\\
 //Astron. Rep.// **54**, 1084–1104 (2010);\\ //Astron. Rep.// **54**, 1084–1104 (2010);\\
 both by S. V. Kalenskii and by L. E. B. Johansson.\\ both by S. V. Kalenskii and by L. E. B. Johansson.\\
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 The more recent detection of the //J// = 1 – 0 and 2 – 1 transitions by\\ The more recent detection of the //J// = 1 – 0 and 2 – 1 transitions by\\
 V. Guzmán, J. Pety, P. Gratier, J. R. Goicoechea, M. Gerin, E. Roueff, and D. Teyssier,\\ V. Guzmán, J. Pety, P. Gratier, J. R. Goicoechea, M. Gerin, E. Roueff, and D. Teyssier,\\
-**[[http://dx.doi.org/10.1051/0004-6361/201219449|The IRAM-30m line survey of the Horsehead PDR\\+**[[https://doi.org/10.1051/0004-6361/201219449|The IRAM-30m line survey of the Horsehead PDR\\
 I. CF<sup>+</sup> as a tracer of C<sup>+</sup> and as a measure of the fluorine abundance]]**\\ I. CF<sup>+</sup> as a tracer of C<sup>+</sup> and as a measure of the fluorine abundance]]**\\
 //Astron. Astrophys.// **543**, Art. No. 1 (2012);\\ //Astron. Astrophys.// **543**, Art. No. 1 (2012);\\
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 H. S. Liszt, J. Pety, M. Gerin, and R. Lucas,\\ H. S. Liszt, J. Pety, M. Gerin, and R. Lucas,\\
 detected with the IRAM 30 m telescope\\ detected with the IRAM 30 m telescope\\
-**[[http://dx.doi.org/10.1051/0004-6361/201323320|HCO, //c//-C<sub>3</sub>H and CF<sup>+</sup>: three new molecules in diffuse, translucent and “spiral-arm” clouds]]**\\+**[[https://doi.org/10.1051/0004-6361/201323320|HCO, //c//-C<sub>3</sub>H and CF<sup>+</sup>: three new molecules in diffuse, translucent and “spiral-arm” clouds]]**\\
 //Astron. Astrophys.// **564**, Art. No. A64 (2014). //Astron. Astrophys.// **564**, Art. No. A64 (2014).
  
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 Contributor(s): H. S. P. Müller; 09, 2005; 08, 2006; 11, 2012; 05, 2015 Contributor(s): H. S. P. Müller; 09, 2005; 08, 2006; 11, 2012; 05, 2015
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