# FOURIER TRANSFORM EMISSION SPECTRA OF THE $4051 \AA$ BAND OF $C_{3}$

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 dc.creator Tanabashi, Akihiro en_US dc.creator Hirao, T. en_US dc.creator Amano, T. en_US dc.creator Bernath, P. F. en_US dc.date.accessioned 2006-06-15T20:59:01Z dc.date.available 2006-06-15T20:59:01Z dc.date.issued 2004 en_US dc.identifier 2004-WJ-01 en_US dc.identifier.uri http://hdl.handle.net/1811/21530 dc.description $^{a}$B.J. McCall, R.N. Casaes, M. \'{A}d\'{a}mkovics and R.J. Saykally, Chem. Phys. Lett. 374, 583-586 (2003) $^{b}$L. Gausset, G. Herzberg, A. Lagerqvist and B. Rosen, Astrophys. J. 142. 45-76 (1965) en_US dc.description Author Institution: Institute for Astrophysics and Planetary Sciences, Ibaraki University; Department of Chemistry, University of Waterloo en_US dc.description.abstract $C_{3}$ is an important molecule in astrophysics. Its spectra serves as probes into physical conditions (e.g. density, temperature) of astronomical objects such as carbon stars, interstellar clouds and comets. The $(000)-(000)$ band of the $4051 \AA$ band $(^{1} \Pi_{u} - X {^{1}}\Sigma^{+}_{g})$ of $C_{3}$ was recorded in emission with a Bruker IFS 120HR Fourier transform spectrometer at University of Waterloo. The band was excited by a microwave discharge in iso-propanol diluted in helium. This band was also re-examined by recent cavity ring down spectroscopy by McCall $et al.^{a}$ They observed low temperature spectrum of this band using a supersonic expansion source and showed the R(0) transition was incorrectly assigned in the previous laboratory work. Analysis of our new spectrum combined with the data by McCall et al. confirmed the lower J levels in the A state were perturbed as reported by Gausset $et al.^{b}$ The unidentified lines observed by McCall et al. can be identified to be extra transitions due to the perturbing state. Investigation into nature of the perturbation will be presented. en_US dc.format.extent 342864 bytes dc.format.mimetype image/jpeg dc.language.iso English en_US dc.title FOURIER TRANSFORM EMISSION SPECTRA OF THE $4051 \AA$ BAND OF $C_{3}$ en_US dc.type article en_US