molecules:extragalactic:hc2nh_extragalactic

Differences

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

Link to this comparison view

molecules:extragalactic:hc2nh_extragalactic [2019/02/25 22:38] – external edit 127.0.0.1molecules:extragalactic:hc2nh_extragalactic [2019/10/22 16:20] (current) – mueller
Line 5: Line 5:
 An early account on Extragalactic acetylene was presented by\\ An early account on Extragalactic acetylene was presented by\\
 J. T. van Loon, A. A. Zijlstra, and M. A. T. Groenewegen,\\ J. T. van Loon, A. A. Zijlstra, and M. A. T. Groenewegen,\\
-**[[http://cdsads.u-strasbg.fr/abs/1999A%26A...346..805V|Luminous Carbon Stars in the Magellanic Clouds]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1999A%26A...346..805V|Luminous Carbon Stars in the Magellanic Clouds]]**\\
 //Astron. Astrophys.// **346**, (1999) 805.\\ //Astron. Astrophys.// **346**, (1999) 805.\\
 Telescopes of ESO and CTIO were used to carry out observations in the L-band (at 3 μm). Broad, strong absorption was found between 3.0 and 3.3 μm which was attributed to HCN and HCCH. As usual also in the later accounts, no spectroscopic information is given and no reference to laboratory spectroscopy. The band is caused by the strong CH stretching mode of both molecules, and the contributions of the molecules can not be disentangled. Telescopes of ESO and CTIO were used to carry out observations in the L-band (at 3 μm). Broad, strong absorption was found between 3.0 and 3.3 μm which was attributed to HCN and HCCH. As usual also in the later accounts, no spectroscopic information is given and no reference to laboratory spectroscopy. The band is caused by the strong CH stretching mode of both molecules, and the contributions of the molecules can not be disentangled.
  
-**[[http://dx.doi.org/10.1086/345680|Very Large Telescope Spectra of Carbon Stars in the Large Magellanic Cloud and Their Metallicity Dependence]]**\\+**[[https://doi.org/10.1086/345680|Very Large Telescope Spectra of Carbon Stars in the Large Magellanic Cloud and Their Metallicity Dependence]]**\\
 //Astrophys. J.// **580**, (2002) L133,\\ //Astrophys. J.// **580**, (2002) L133,\\
 by\\ by\\
Line 21: Line 21:
 J. Bernard-Salas, E. Peeters, G. C. Sloan, J. Cami, S. Guiles, and J. R. Houck\\ J. Bernard-Salas, E. Peeters, G. C. Sloan, J. Cami, S. Guiles, and J. R. Houck\\
 obtained\\ obtained\\
-**[[http://dx.doi.org/10.1086/509777|The //Spitzer// IRS spectrum of SMP LMC 11]]**\\+**[[https://doi.org/10.1086/509777|The //Spitzer// IRS spectrum of SMP LMC 11]]**\\
 //Astrophys. J.// **652**, (2006) L29.\\ //Astrophys. J.// **652**, (2006) L29.\\
 The spectrum resembles that of the protoplanetary nebula V353 Aur, which is somewhat better known as CRL (or AFGL) 618. Butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, were iditified by their unresolved //Q//-branches of the //ν//<sub>8</sub> band of butadiyne at 15.9 μm and the //ν//<sub>11</sub> band of hexatriyne at 16.1 μm, respectively, as in the Galactic source. The spectrum resembles that of the protoplanetary nebula V353 Aur, which is somewhat better known as CRL (or AFGL) 618. Butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, were iditified by their unresolved //Q//-branches of the //ν//<sub>8</sub> band of butadiyne at 15.9 μm and the //ν//<sub>11</sub> band of hexatriyne at 16.1 μm, respectively, as in the Galactic source.
Line 29: Line 29:
  
 Contributor(s): H. S. P. Müller; 5, 2012 Contributor(s): H. S. P. Müller; 5, 2012
- 
  
 ---- ----
  
  
  • molecules/extragalactic/hc2nh_extragalactic.1551130687.txt.gz
  • Last modified: 2019/02/25 22:38
  • by 127.0.0.1