Structure
Linear (''l''-C3H)
μD=3.551 Debye 2Π electronic ground stateSimulated spectrum
A rotational spectrum of the 2Π electronic ground state of ''l''-C3H can be made using the PGopher software (a Program for Simulating Rotational Structure, C. M. Western, University of Bristol, http://pgopher.chm.bris.ac.uk) and molecular constants extracted from the literature. These constants include μ=3.551 Debye and others provided by Yamamoto et al. 1990, given in units of MHz: B=11189.052, D=0.0051365, ASO=432834.31, γ=-48.57, p=-7.0842, and q=-13.057. A selection rule of ΔJ=0,1 was applied, with S=0.5. The resulting simulation for the rotational spectrum of C3H at a temperature of 30 K agree well with observations. The simulated spectrum is shown in the figure at right with the approximate atmospheric transmission overplotted in blue. All of the strongest simulated lines with J < 8.5 are observed by Yamamoto et al.Cyclic (''c''-C3H)
μD=2.4 Debye electronic ground stateChemistry
The molecule C3H has been observed in cold, denseDominant formation reactions
Dominant destruction reactions
Contribution to carbon-chain molecule production
The C3H molecule provides the dominant pathway to the production of C4H+, and thereby all other CnH (n>3) molecules via the reactions:First astronomical detection
The first confirmation of the existence of the interstellar molecule C3H was announced by W.M Irvine et al. at the January 1985 meeting of the American Astronomical Society. The group detected C3H in both the spectrum of the evolved carbon star IRC+10216 and in the molecular cloud TMC-1. These results were formally published in July of the same year by Thaddeus et al. A 1987 paper by W.M. Irvine provides a comparison of detections for 39 molecules observed in cold (Tk ≅10K), dark clouds, with particular emphasis paid to tri-carbon species, including C3H.Subsequent astronomical detections
Later reports of astronomical detections of the C3H radical are given in chronological order below. In 1987, Yamamoto et al. report measurements of the rotational spectra of the cyclic C3H radical (c-C3H) in the laboratory and in interstellar space towards TMC-1. This publication marks the first terrestrial measurement of C3H. Yamamoto et al. precisely determine molecular constants and identify 49 lines in the c-C3H rotational spectrum. Both fine and hyperfine components are detected toward TMC-1, and the column density for the line of sight toward TMC-1 is estimated to be 6x1012cm−2, which is comparable to the linear C3H radical (l-C3H). M.L Marconi and A. Korth et al. reported a likely detection of C3H within the ionopause of Comet Halley in 1989. Using the heavy ion analyzer (PICCA) on board the Giotto spacecraft they determined that C3H was responsible for producing a peak at 37amu detected within ~4500 km of the comet nucleus. Marconi et al. argue that a gas phase progenitor molecule for C3H is unlikely to exist within the ionopause and suggest that desorption from circumnuclear CHON dust grains may have instead produced the observed C3H. In 1990, Yamamoto et al. detected C3H toward IRC + 10216 using the Nobeyama Radio Observatory's 45-m radio telescope. They determine an upper limit for the column density of the ν4 state 3x1012cm−2. From additional laboratory measurements they determine an extremely low vibrationally excited state for the C3H radical: ν4(2Σμ)=610197(1230) MHz, caused by the Renner-Teller effect in the ν4 (CCH bending) state. J.G. Mangum and A. Wootten report new detections of c-C3H towards 13 of 19 observed Galactic molecular clouds. They measure relative abundance of C3H to C3H2: N(c-C3H)/N(C3H2) = 9.04±2.87 x 10−2. This ratio does not change systematically for warmer sources, which they suggest provides evidence that the two ring molecules have a common precursor in C3H3+. L.A. Nyman et al. present a molecular line survey of the carbon star IRAS 15194-5115 using the 15m Swedish-ESO Submillimetre Telescope to probe the 3 and 1.3 mm bands. Comparing the molecular abundances with those of IRC + 10216, they find C3H to have similar abundances in both sources. In 1993, M. Guelin et al. map the emission from the 95 GHz and 98 GHz lines of the C3H radicals in IRC+10216. This reveals a shell-like distribution of the C3H emission and time-dependent chemistry. The close correspondence between the emission peaks of C3H and the speciesReferences
{{Molecules detected in outer space Alkynes Astrochemistry