molecules:ism:propin

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:propin [2020/03/10 14:45] – muellermolecules:ism:propin [2021/06/14 15:14] (current) – mueller
Line 5: Line 5:
 **[[https://cdms.astro.uni-koeln.de/classic/predictions/daten/CH3CCH/Buhl_and_Snyder_1973.pdf|The Detection of a MM-Wave Transition of Methylacetylene]]**\\ **[[https://cdms.astro.uni-koeln.de/classic/predictions/daten/CH3CCH/Buhl_and_Snyder_1973.pdf|The Detection of a MM-Wave Transition of Methylacetylene]]**\\
 in: M.A. Gordon, L.E. Snyder (Eds.), Molecules in the Galactic Environment, 1973, 187−195.\\ in: M.A. Gordon, L.E. Snyder (Eds.), Molecules in the Galactic Environment, 1973, 187−195.\\
-The //J// = 5 – 4 transition with //K// = 0 was observed with the 36 foot (11 m) NRAO dish at 85457.3 MHz toward Sagittarius B.+The //J// = 5 – 4 transition with //K// = 0 was observed with the 36 foot (11 m) NRAO dish at 85457.3 MHz toward Sagittarius B.\\
  
 J. M. Hollis, L. E. Snyder, D. H. Blake, F. J. Lovas, R. D. Suenram, and B. L. Ulich\\ J. M. Hollis, L. E. Snyder, D. H. Blake, F. J. Lovas, R. D. Suenram, and B. L. Ulich\\
 identified the //J// = 9 – 8 transitions with //K// = 0 to 3 near 153.8 GHz employing the same instrument in their report on\\ identified the //J// = 9 – 8 transitions with //K// = 0 to 3 near 153.8 GHz employing the same instrument in their report on\\
 **[[https://ui.adsabs.harvard.edu/abs/1981ApJ...251..541H|New Interstellar Molecular Transitions in the 2 Millimeter Range]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1981ApJ...251..541H|New Interstellar Molecular Transitions in the 2 Millimeter Range]]**\\
-//Astrophys. J.// **251**, 541–548 (1981).+//Astrophys. J.// **251**, 541–548 (1981).\\
  
 E. Churchwell and J. M. Hollis\\ E. Churchwell and J. M. Hollis\\
Line 16: Line 16:
 **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...272..591C|The Kinetic Temperature and CH<sub>3</sub>CCH Column Density Profiles in Sgr B2, Orion and DR 21]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...272..591C|The Kinetic Temperature and CH<sub>3</sub>CCH Column Density Profiles in Sgr B2, Orion and DR 21]]**\\
 //Astrophys. J.// **272**, 591–608 (1983).\\ //Astrophys. J.// **272**, 591–608 (1983).\\
-These three high-mass star-forming regions were studied with the same instrument covering the //J// = 5 – 4 and 6 – 5 transitions.+These three high-mass star-forming regions were studied with the same instrument covering the //J// = 5 – 4 and 6 – 5 transitions.\\
  
 Further sources, including the dark Taurus Molecular Cloud 1 (TMC-1), were studied by\\ Further sources, including the dark Taurus Molecular Cloud 1 (TMC-1), were studied by\\
Line 25: Line 25:
 J. Askne, B. Höglund, Å. Hjalmarson, and W. M. Irvine\\ J. Askne, B. Höglund, Å. Hjalmarson, and W. M. Irvine\\
 **[[https://ui.adsabs.harvard.edu/abs/1984A&A...130..311A|Methyl Acetylene as a Temperature Probe in Molecular Clouds]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1984A&A...130..311A|Methyl Acetylene as a Temperature Probe in Molecular Clouds]]**\\
-//Astron. Astrophys.// **130**, 311–318 (1984).+//Astron. Astrophys.// **130**, 311–318 (1984).\\
  
 B. E. Turner, E. Herbst, and R. Terzieva\\ B. E. Turner, E. Herbst, and R. Terzieva\\
Line 31: Line 31:
 **[[https://doi.org/10.1086/313301|The Physics and Chemistry of Small Translucent Molecular Clouds. XIII. The Basic Hydrocarbon Chemistry]]**\\ **[[https://doi.org/10.1086/313301|The Physics and Chemistry of Small Translucent Molecular Clouds. XIII. The Basic Hydrocarbon Chemistry]]**\\
 //Astrophys. J. Suppl. Ser.// **126**, 427–460 (2000).\\ //Astrophys. J. Suppl. Ser.// **126**, 427–460 (2000).\\
-Propyne was detected in the sources CB 17 and CB 228; only an upper limit was determined for CB 24.+Propyne was detected in the sources CB 17 and CB 228; only an upper limit was determined for CB 24.\\
  
 ---- ----
Line 66: Line 66:
 **[[https://ui.adsabs.harvard.edu/abs/1992A&A...253L..29G|Interstellar detection of deuterated methyl acetylene,]]**\\ **[[https://ui.adsabs.harvard.edu/abs/1992A&A...253L..29G|Interstellar detection of deuterated methyl acetylene,]]**\\
 //Astron. Astrophys.// **253**, L29–L32 (1992)\\ //Astron. Astrophys.// **253**, L29–L32 (1992)\\
-refers to the methyl deuterated isotopolog, which was detected with the IRAM 30 m dish in TMC-1. +refers to the methyl deuterated isotopolog, which was detected with the IRAM 30 m dish in TMC-1.\\
  
 A. J. Markwick, S. B. Charnley, H. M. Butner, T. J. Millar\\ A. J. Markwick, S. B. Charnley, H. M. Butner, T. J. Millar\\
Line 72: Line 72:
 **[[https://doi.org/10.1086/432415|Interstellar CH<sub>3</sub>CCD]]**\\ **[[https://doi.org/10.1086/432415|Interstellar CH<sub>3</sub>CCD]]**\\
 //Astrophys. J. Lett.// **627**, L117−L120 (2005).\\ //Astrophys. J. Lett.// **627**, L117−L120 (2005).\\
-The authors used the OSO 20 m dish for a detection in TMC-1.+The authors used the OSO 20 m dish for a detection in TMC-1.\\ 
 + 
 +M. Agúndez, E. Roueff, C. Cabezas, J. Cernicharo, and N. Marcelino\\ 
 +reported on the\\ 
 +**[[https://doi.org/10.1051/0004-6361/202140843|First detection of doubly deuterated methyl acetylene (CHD<sub>2</sub>CCH and CH<sub>2</sub>DCCD)]]**\\ 
 +//Astron. Astrophys.// **649**, Art. No. A 171 (2021).\\ 
 +The identifications were made in the course of a molecular line survey of L483 at 3 mm carried out with the IRAM 30 m radio telescope. The survey samples cold material; the presence of the embedded Class 0 infrared source IRAS 18148−0440 is not visible in these data. 9 and 8 //a//-type transition frequencies with 4 ≤ //J// ≤ 7 and //K<sub>a</sub>// ≤ 1 were reported. The column density ratios of CH<sub>3</sub>CCH with CH<sub>2</sub>DCCH, CH<sub>3</sub>CCD, CHD<sub>2</sub>CCH, and CH<sub>2</sub>DCCD are about 5, 16, 34, and 42, respectively.\\ 
  
 ---- ----
  
-Contributor(s): H. S. P. Müller 03, 2020+Contributor(s): H. S. P. Müller 03, 2020; 06, 2021
  
 ---- ----
  • molecules/ism/propin.1583847910.txt.gz
  • Last modified: 2020/03/10 14:45
  • by mueller