Differences

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

--- molecules:ism:c3 [2019/01/23 22:44] – created admin
+++ molecules:ism:c3 [2020/02/15 14:20] (current) – mueller
@@ Line 1: / Line 1: @@
-=== On the Detection of Propadienediylidene, C3, in Space ===
+===== On the Detection of Propadienediylidene, C3, in Space =====
-The pure carbon chain molecule propadienediylidene, C3, has been detected in the circumstellar envelope of the famous carbon star CW Leo, aka IRC +10216, by
+The pure carbon chain molecule propadienediylidene, C<sub>3</sub>, has been detected in the circumstellar envelope of the famous carbon star CW Leo, aka IRC +10216, by\\
-K. H. Hinkle, J. J. Keady, and P. F. Bernath,
+K. H. Hinkle, J. J. Keady, and P. F. Bernath,\\
-[[http://dx.doi.org/10.1126/science.241.4871.1319|Detection of C3 in the Circumstellar Shell of IRC +10216]],
+**[[https://doi.org/10.1126/science.241.4871.1319|Detection of C<sub>3</sub> in the Circumstellar Shell of IRC +10216]]**,\\
-Science 241, 1319–1322 (1988)
+//Science// **241**, 1319–1322 (1988)\\
+at about the same time as the corresponding laboratory spectrum has been recorded. 15 //P// and //R// branch transitions of the ν<sub>3</sub> band were detected around 2040 cm<sup>–1</sup> of which 12 appear to be unblended.
-at about the same time as the corresponding laboratory spectrum has been recorded. 15 P and R branch transitions of the ν3 band were detected around 2040 cm–1 of which 12 appear to be unblended.
+Evidence for the presence of C<sub>3</sub> was obtained from the observation of a weak absorption feature at 1968.594 GHz with the KAO toward Sagittarius B2 which was tentatively assigned to //R//(2) of the low-lying ν<sub>2</sub> mode by\\
+A. van Orden, J. D. Cruzan, R. A. Provencal, T. F. Giesen, R. J. Saykally, R. T. Boreiko, and A. L. Betz,\\
+**[[https://ui.adsabs.harvard.edu/abs/1995ASPC...73...67V|A Search for the C<sub>3</sub> Carbon Cluster in the Interstellar Medium]]**,\\
+//ASP Conf. Ser.// **73**, 67–70 (1995)\\
+This detection was confirmed by\\
+J. Cernicharo, J. R. Goicoechea, and E. Caux,\\
+**[[https://doi.org/10.1086/312668|Far-infrared Detection of C<sub>3</sub> in Sagittarius B2 and IRC +10216]]**,\\
+//Astrophys. J.// **534**, L199–L202 (2000).\\
+The authors identified 9 transitions detected with ISO toward Sgr B2 along with the //R//(2) and //R//(4) toward CW Leo.
-Evidence for the presence of C3 was obtained from the observation of a weak absorption feature at 1968.594 GHz with the KAO toward Sagittarius B2 which was tentatively assigned to R(2) of the low-lying ν2 mode by
+C<sub>3</sub> has also been observed in the diffuse interstellar medium toward several stars by recording its //A// <sup>1</sup>Π<sub>u</sub> – //X// <sup>1</sup>Σ<sup>+</sup><sub>g</sub>, //v// = 0 – 0 electronic spectrum around 405.2 nm.\\
-A. van Orden, J. D. Cruzan, R. A. Provencal, T. F. Giesen, R. J. Saykally, R. T. Boreiko, and A. L. Betz,
+J. P. Maier, N. M. Lakin, G. A. H. Walker, and D. A. Bohlender,\\
-[[http://cdsads.u-strasbg.fr/abs/1995ASPC...73...67V|A Search for the C3 Carbon Cluster in the Interstellar Medium]],
+**[[https://doi.org/10.1086/320668|Detection of C<sub>3</sub> in Diffuse Interstellar Clouds]]**,\\
-ASP Conf. Ser. 73, 67–70 (1995)
+//Astrophys. J.// **553**, 267–273 (2001),\\
+studied sightlines toward 20 Aql, ζ Oph, and ζ Per. Two components were detected, a warm one around 60 K and a hot one around 250 K.
-This detection was confirmed by
+T. F. Giesen, B. Mookerjea, G. W. Fuchs, A. A. Breier, D. Witsch, R. Simon, and J. Stutzki\\
-J. Cernicharo, J. R. Goicoechea, and E. Caux,
+reported on the\\
-[[http://dx.doi.org/10.1086/312668|Far-infrared Detection of C3 in Sagittarius B2 and IRC +10216]],
+**[[https://doi.org/10.1051/0004-6361/201936538|First Detection of the Carbon Chain Molecules <sup>13</sup>CCC and C<sup>13</sup>CC towards SgrB2(M)]]**,\\
-Astrophys. J. 534, L199–L202 (2000).
+//Astron. Astrophys.// **633** Art. No. A120 (2020).\\
-The authors identified 9 transitions detected with ISO toward Sgr B2 along with the R(2) and R(4) toward CW Leo.
+The average <sup>12</sup>C/<sup>13</sup>C ratio per C atom is about 20.5, in the expected range. However, C<sup>13</sup>CC is slightly overabundant with a ratio of 14.8 ± 2.7 whereas <sup>13</sup>CCC is underabundant with a ratio of 12.7 ± 2.8; the latter value corresponds to a <sup>12</sup>C/<sup>13</sup>C ratio per C atom of 25.4 ± 5.6 because of two equivalent terminal C atoms.\\
+----
+Contributor(s): H. S. P. Müller; 08, 2010; 02, 2020
+----
-C3 has also been observed in the diffuse interstellar medium toward several stars by recording its A 1Πu – X 1Σ+g, v = 0 – 0 electronic spectrum around 405.2 nm.
-J. P. Maier, N. M. Lakin, G. A. H. Walker, and D. A. Bohlender,
-[[http://dx.doi.org/10.1086/320668|Detection of C3 in Diffuse Interstellar Clouds]],
-Astrophys. J. 553, 267–273 (2001),
-studied sightlines toward 20 Aql, ζ Oph, and ζ Per. Two components were detected, a warm one around 60 K and a hot one around 250 K.
-Contributor(s): H. S. P. Müller; 08, 2010