Differences

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

--- molecules:ism:cyanomethanimin [2019/10/23 22:07] – mueller
+++ molecules:ism:cyanomethanimin [2024/05/17 16:08] (current) – mueller
@@ Line 1: / Line 1: @@
-===== The Detection of Cyanomethanimine in the ISM =====
+===== The Detection of Cyanomethanimines in the ISM =====
-Cyanomethanimine, HNCHCN, is a slightly unsaturated sibling of [[molecules:ism:AAN|aminoacetonitrile]], H<sub>2</sub>NCH<sub>2</sub>CN. It has been identified recently by\\
+C-cyanomethanimine, HNCHCN, is a slightly unsaturated sibling of [[molecules:ism:aan|aminoacetonitrile]], H<sub>2</sub>NCH<sub>2</sub>CN. It has been identified recently by\\
 D. P. Zaleski, N. A. Seifert, A. L. Steber, M. T. Muckle, R. A. Loomis, J. F. Corby, O. Martinez, Jr., K. N. Crabtree, P. R. Jewell, J. M. Hollis, F. J. Lovas, D. Vasquez, J Nyiramahirw, N. Sciortino, K. Johnson, M. C. McCarthy, A. J. Remijan, and B. H. Pate,\\
 **[[https://doi.org/10.1088/2041-8205/765/1/L10|Detection of //E//-Cyanomethanimine toward Sagittarius B2(N) in the Green Bank Telescope PRIMOS Survey]]**\\
@@ Line 13: / Line 13: @@
 M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris,\\
 **[[https://doi.org/10.1086/523627|The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository]]**\\
-//Astrophys. J.// **672**, 352–360 (2008).
+//Astrophys. J.// **672**, 352–360 (2008).\\
+\\
 V. M. Rivilla, J. Martín-Pintado, I. Jiménez-Serra, S. Zeng, S. Martín, J. Armijos-Abendañdo, M. A. Requena-Torres, R. Aladro, and D. Riquelme\\
@@ Line 19: / Line 20: @@
 **[[https://doi.org/10.1093/mnrasl/sly228|Abundant Z-cyanomethanimine in the Interstellar Medium: Paving the Way to the Synthesis of Adenine]]**\\
 //Mon. Not. R. Soc. Astron.// **483**, L114–L119 (2019).\\
-The results were obtained in the course of a line survey of the Galactic center source G 0.693–0.03 at 3 mm using the IRAM 30 m dish; additional observation around 1.3 cm were carried out with the GBT 100 m dish. The E-conformer was also identified. The Z/E ratio of about six indicated thermal equilibrium at the kinetic temperature of the cloud. The excitation temperature, in contrast, is rather cold, about 8 K.
+The results were obtained in the course of a line survey of the Galactic center source G 0.693–0.03 at 3 mm using the IRAM 30 m dish; additional observation around 1.3 cm were carried out with the GBT 100 m dish. The //E//-conformer was also identified. The Z/E ratio of about six indicated thermal equilibrium at the kinetic temperature of the cloud. The excitation temperature, in contrast, is rather cold, about 8 K.\\
+\\
+D. San Andrés, V. M. Rivilla, L. Colzi, I. Jiménez-Serra, J. Martín-Pintado, A. Megías, Á. López-Gallifa, A. Martínez-Henares, S. Massalkhi, S. Zeng, M. Sanz-Novo, B. Tercero, P. de Vicente, S. Martín, M. A. Requena Torres, G. Molpeceres, and J. García de la Concepción\\
+described the\\
+**[[https://doi.org/10.3847/1538-4357/ad3af3|First Detection in Space of the High-energy Isomer of Cyanomethanimine: H<sub>2</sub>CNCN]]**\\
+//Astrophys. J.// **967**, Art. No 39 (2024).\\
+The results were obtained in the course of line surveys of the Galactic center source G 0.693–0.03 using the Yebes 40 m and IRAM 30 m telescopes. 14 //a//-type transitions with 2 ≤ //J// ≤ 10, //K<sub>a</sub>// ≤ 2 were identified between 31 and 107 GHz. Six of these transitions were unblended or only slightly blended. A non-thermal C-/N-cyanomethanimine ratio of ~32 was derived, while the //Z//-///E//-cyanomethanimine ratio of ~4.5 was deemed to be thermal, as may be expected for a pair of conformers. In contrast, N-cyanomethanimine is an isomer of C-cyanomethanimine, meaning, it requires the formal breaking of at least one bond for interconversion.\\
+\\
 ----
-Contributor(s): H. S. P. Müller; 02, 2013; 01, 2019
+Contributor(s): H. S. P. Müller; 02, 2013; 01, 2019; 05, 2024
 ----