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--- molecules:ism:ammoniak [2026/02/05 13:52] – mueller
+++ molecules:ism:ammoniak [2026/02/06 11:18] (current) – mueller
@@ Line 10: / Line 10: @@
 **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...271L..27K|First Detection of the Ground-State //J<sub>K</sub>// = 1<sub>0</sub> – 0<sub>0</sub> Submillimeter Transition of Interstellar Ammonia]]**\\
 //Astrophys. J.// **271**, L27–L30 (1983).\\
+\\
+T. L. Wilson, K. Ruf, C. M. Walmsley, R. N. Martin, T. A. Pauls, and W. Batria\\
+reported on the\\
+**[[https://ui.adsabs.harvard.edu/abs/1982A%26A...115..185W|Detection of the (8,8) and (9,9) Absorption Lines of Ammonia: the Hot Molecular Cloud toward Sgr B2]]**\\
+//Astron. Astrophys.// **115**, 185−189 (1982).\\
+Observations were made with the MPIfR 100 m Effelsberg telescope pointing toward Sgr B2(S).\\
+\\
+T. L. Wilson, C. Henkel, and S. Hüttemeister, G. Dahmen, A. Linhart, C. Lemme, and J. Schmidt-Burgk\\
+reported on\\
+**[[https://ui.adsabs.harvard.edu/abs/1993A%26A...276L..29W|Hot Ammonia Emission: Kinetic Temperature Gradients in Orion-KL]]**\\
+//Astron. Astrophys.// **276**, L29−L32 (1993).\\
+The MPIfR 100 m Effelsberg telescope was employed for observations of ammonia inversion transitions with 10 ≤ //J// = //K// ≤ 14.\\
+\\
+T. L. Wilson, C. Henkel, and S. Hüttemeister\\
+announced\\
+**[[https://doi.org/10.1051/0004-6361:20065591|The detection of the (J, K) = (18, 18) line of NH3]]**\\
+//Astron. Astrophys.// **460**, 533–538 (2006).\\
+Observations with the Effelsberg 100 m dish were successful toward Sgr B2(M) and Sgr B2(N); only an upper limit was reported for Orion KL.\\
 \\
@@ Line 16: / Line 37: @@
 **[[https://ui.adsabs.harvard.edu/abs/1988A%26A...205..235M|Vibrationally Excited Ammonia toward Orion-KL]]**\\
 //Astron. Astrophys.// **205**, 235–242 (1988).\\
-\\
+The IRAM 30 m dish was used for observations near 140.1 GHz.
+---
 NH<sub>2</sub>D was detected initially toward Sgr B2 and Orion KL:\\