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--- molecules:ism:c_no [2021/12/20 12:39] – created mueller
+++ molecules:ism:c_no [2021/12/20 14:53] (current) – [Oxopropadienylidene, C<sub>3</sub>O] mueller
@@ Line 1: / Line 1: @@
-===== Detection of Oxoethenylidene, CCO, in the ISM =====
+===== On Oxygen-terminated Carbon Chain Molecules CnO in Space =====
+==== Oxoethenylidene, C<sub>2</sub>O ====
 CCO has been detected first toward TMC-1:\\
@@ Line 5: / Line 7: @@
 **[[https://ui.adsabs.harvard.edu/abs/1991ApJ...380L..39O|Detection of a new carbon-chain molecule, CCO]]**\\
 //Astrophys. J.// **380**, L39–L42 (1991).\\
-The //N<sub>J</sub>// = 1<sub>2</sub> – 0<sub>1</sub> and 2<sub>3</sub> – 1<sub>2</sub> transitions werev detected with the 43 m Green Bank telescope and the 45 m Nobeyama telecope, respectively, at 22258 and 45827 MHz.
+The //N<sub>J</sub>// = 1<sub>2</sub> – 0<sub>1</sub> and 2<sub>3</sub> – 1<sub>2</sub> transitions were detected with the 43 m Green Bank telescope and the 45 m Nobeyama telecope, respectively, at 22258 and 45827 MHz.\\
+\\
+R. G. Urso, M. E. Palumbo, C. Ceccarelli, N. Balucani, S. Bottinelli, C. Codella, F. Fontani, P. Leto, C. Trigilio, C. Vastel, R. Bachiller, G. A. Baratta, C. S. Buemi, E. Caux, A. Jaber Al-Edhari, B. Lefloch, A. López-Sepulcre, G. Umana, and L. Testi\\
+reported on\\
+**[[https://doi.org/10.1051/0004-6361/201834322|C<sub>2</sub>O and C<sub>3</sub>O in Low-mass Star-forming Regions]]**\\
+//Astron. Astrophys.// **628**, Art. No. A72 (2019).\\
+The C<sub>2</sub>O observations were carried out with the IRAM 30 m telescope at 3 mm. Three fine structure components of the //N// = 4 - 3 rotational transition around 92.5 GHz were detected toward the prestellar core L1544. Only the strongest of these components was searched for and detected toward the protostellar Elias 18.
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+==== Oxopropadienylidene, C<sub>3</sub>O ====
-Contributor(s): H. S. P. Müller; 12, 2003; 09, 2012
+H. E. Matthews, W. M. Irvine, P. Friberg, R. D. Brown, and P. D. Godfrey\\
+reported on\\
+**[[https://doi.org/10.1038/310125a0|A new Interstellar Molecule: Tricarbon Monoxide]]**\\
+//Nature// **310**, 125–126 (1984).\\
+The //J// = 2 − 1 transitions near 19.2 GHz was detected with good signal-to-noise ratio toward TMC-1 using the 43 m GBT.\\
+\\
+R. D. Brown, P. D. Godfrey, D. M. Cragg, E. H. N. Rice, W. M. Irvine, P. Friberg, H. Suzuki, M. Ohishi, N. Kaifu, and M. Morimoto\\
+extended the previous study subsequently in\\
+**[[https://doi.org/10.1086/163528|Tricarbon Monoxide in TMC-1]]**\\
+//Astrophys. J. // **297**, 302–308 (1985).\\
+The //J// = 5 − 4, 8 − 7, and 9 − 8 transitions near 48.1, 77.0, and 86.6 GHz were detected using various telescopes.\\
+\\
+The molecules was also detected in the circumstellar envelope of the C-rich AGB star CW Leonis by\\
+E. D. Tenenbaum, A. J. Apponi, L. M. Ziurys, M. Agúndez, J. Cernicharo, J. R. Pardo, and M. Guélin\\
+**[[https://doi.org/10.1086/508166|Detection of C<sub>3</sub>O in IRC +10216: Oxygen-Carbon Chain Chemistry in the Outer Envelope]]**\\
+//Astrophys. J. // **649**, L17–L20 (2006).\\
+Observations were carried out at 3 and 2 mm using the ARO 12 m dish and a 3 mm using the IRAM 30 m telescope.\\
+M. E. Palumbo, P. Leto, C. Siringo, and C. Trigilio\\
+reported on the\\
+**[[https://doi.org/10.1086/591017|Detection of C<sub>3</sub>O in the Low-Mass Protostar Elias 18]]**\\
+//Astrophys. J. // **297**, 302–308 (1985).\\
+The Noto 32 m dish was employed to serach for the //J// = 4 − 3 transition near 38.5 GHz.\\
+==== Oxopentatetraenylidene, C<sub>5</sub>O ====
+J. Cernicharo, M. Agúndez, C. Cabezas, B. Tercero, N. Marcelino, R. Fuentetaja, J. R. Pardo, and P. de Vicente\\
+reported on the\\
+**[[https://doi.org/10.1051/0004-6361/202142634|Discovery of HCCCO and C<sub>5</sub>O in TMC-1 with the QUIJOTE Line
+Survey]]**\\
+//Astron. Astrophys.// **656**, Art. No. L21 (2021).\\
+Oxopentatetraenylidene, C<sub>5</sub>O, was identified through six rotational transitions with 11 ≤ //J// ≤ 17 in the course of a molecular line survey of the prototypical cold dark molecular cloud TMC-1 carried out with the Yebes 40 m radio telescope between 31.0 and 50.3 GHz. Four transitions were unblended or only slightly blended, two were somewhat more blended. A value of //T//<sub>rot</sub> = 10.0 ± 0.5 K was derived through a rotation diagram. C<sub>5</sub>O is about 50 times less abundant than C<sub>2</sub>O and about 80 times less abundant than C<sub>3</sub>O. Only upper limits were derived for C<sub>4</sub>O and C<sub>6</sub>O; these were in both cases higher than those of C<sub>5</sub>O and thus not particularly constraining.\\
+----
+Contributor(s): H. S. P. Müller; 12, 2003; 09, 2012; 12, 2021
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