Differences

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

--- molecules:ism:oh [2026/07/28 17:19] – mueller
+++ molecules:ism:oh [2026/07/29 11:43] (current) – mueller
@@ Line 18: / Line 18: @@
 **[[https://doi.org/10.1103/PhysRevLett.13.3|Detection of the Interstellar OH Lines at 1612 and 1720 Mc/sec]]**\\
 //Phys. Rev. Lett.// **15**, 3−5 (1964).\\
-These weaker HFS components were measured on the basis of improved spectroscopic parameters prior to their measurements in the laboratory.
+These weaker HFS components were measured with the same dish as above on the basis of improved spectroscopic parameters prior to their measurements in the laboratory.
 H. Weaver, D. R. W. Williams, N. H. Dieter, and W. T. Lum\\
@@ Line 50: / Line 50: @@
 R. Genzel, D. M. Watson, M. K. Crawford, and C. H. Townes\\
 investigated\\
-**[[https://doi.org/10.1086/163574|Detection of Interstellar OH in the Far-Infrared]]**\\
+**[[https://doi.org/10.1086/163574|The Neutral-Gas Disk around the Galactic Center]]**\\
 //Astrophys. J.// **297**, 766−786 (1985).\\
 The Kuiper Airborne Observatory was employed to observe also the low energy rotational transition of OH (<sup>2</sup>Π<sub>1/2</sub> //J// = 1.5 − 0.5) near 1.836 THz.\\
+\\
+K. E. S. Ford, D. A. Neufelf, P. F. Goldsmith, and G. J. Melnick\\
+announced the\\
+**[[https://doi.org/10.1086/374552|Detection of OH toward the Extreme Carbon Star IRC +10216]]**\\
+//Astrophys. J.// **589**, 430−438 (2003).\\
+The 305 m Arecibo dish was used to detect the two strongest HFS components of fundamental Λ-doubling transition near 1665 and 1667 MHz.\\
+\\
+J. R. Goicoechea, J. Cernicharo, M. R. Lerate, F. Daniel, M. J. Barlow, B. M. Swinyard, T. L. Lim, S. Viti, and J. Yates\\
+published on\\
+**[[https://doi.org/10.1086/503799|Far-Infrared Excited Hydroxyl Lines from Orion KL Outflows]]**\\
+//Astrophys. J.// **641**, L49−L52 (2006).\\
+Several rotational transitions of OH in both spin-ladders as well as between them were detected with ISO-LWS.\\
+\\
+T. Khouri, L. Velilla-Prieto, E. De Beck, W. H. T. Vlemmings, H. Olofsson, B. Lankhaar, J. H. Black, and A. Baudry\\
+described the\\
+**[[https://doi.org/10.1051/0004-6361/201935049|Detection of Highly Excited OH towards AGB Stars — A New Probe of Shocked Gas in the Extended Atmospheres]]**\\
+//Astron. Astrophys.// **623**, Art. No. L1 (2019).\\
+Employing ALMA, Λ-doubling transitions in //v// = 0 up to //N// = 18 were detected toward W Hya and R Dor; transitions in //v// = 1 up to //N// = 17 were detected toward W Hya.\\
+\\
+----
+F. F. Gardner, R. X. McGee, and M. W. Sinclair\\
+detected\\
+**[[https://ui.adsabs.harvard.edu/abs/1970ApL.....5...67G/abstract|<sup>18</sup>OH in Sagittarius]]**\\
+//Astrophys. Lett.// **5**, 67−71 (1970).\\
+The two strongest HFS components of the fundamental Λ-doubling transition were observed with the Parkes 64 m dish toward Sgr A and Sgr B2. The <sup>16</sup>O/<sup>18</sup>O rotio was ~314 and ~203, respectively, somewhat lower than ~500 terrestrial.\\
+\\
+F.F. Gardner and J.B. Whiteoak\\
+published on\\
+**[[https://doi.org/10.1093/mnras/176.1.57P|The Detection of Interstellar <sup>17</sup>OH]]**\\
+//Mon. Not. R. Astron. Soc.// **176**, 57P−60P (1976).\\
+Similar observations led to the detection in Sgr A. The <sup>18</sup>O/<sup>17</sup>O rotio was 4.2 ± 0.4, again slightly smaller than ~5.5 terrestrial.\\
+\\
+B. Parise, F. Du, F.-C. Liu, A. Belloche, H. Wiesemeyer, R. Güsten, K. M. Menten, H.-W. Hübers, and B. Klein\\
+announced the\\
+**[[https://doi.org/10.1051/0004-6361/201218784|Detection of OD towards the Low-Mass Protostar IRAS 16293−2422]]**\\
+//Astron. Astrophys.// **542**, Art. No. L5 (2012).\\
+The GREAT receiver on board SOFIA was employed for the observations. A relatively high ratio of OD to HDO was found.\\
+\\
 ----