Diode laser spectroscopy of the ν4 band of benzene

Lindenmayer, Josef; Magg, Ulrich; Jones, Harold

doi:10.1016/0022-2852(88)90215-9

Cited by 33 publications

(11 citation statements)

References 6 publications

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“…The last feature in Figure 1, which is as strong as the n 7 Q-branch of HC 5 N, corresponds to benzene. Figures 1 and 3 show that a narrow feature is centered within a few tenths of the spectral resolution, which is 0.01 mm at this wavelength, of the expected Q-branch of the n 4 band of benzene (673.9732 cm Ϫ1 , i.e., 14.8374 mm; Lindemayer, Magg, & Jones 1988). This narrow feature cannot be associated with any of the lines of the P-branch of C 2 H 2 and HCN bending modes (see Fig.…”

Section: Resultsmentioning

confidence: 90%

[ITAL]Infrared Space Observatory's[/ITAL] Discovery of C[TINF]4[/TINF]H[TINF]2[/TINF], C[TINF]6[/TINF]H[TINF]2[/TINF], and Benzene in CRL 618

Cernicharo

Heras

Tielens³

et al. 2001

The Astrophysical Journal

527

121

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We report on the detection with the Infrared Space Observatory (ISO), for the first time in the circumstellar medium, of the polyacetylenic chains C 4 H 2 and C 6 H 2 and of benzene (C 6 H 6 ) in the direction of the proto-planetary nebula CRL 618. Surprisingly, the abundances of di-and triacetylene are only a factor of 2-4 lower than that of C 2 H 2 . Benzene is Ӎ40 times less abundant than acetylene. We suggest that the chemistry in CRL 618 has been strongly modified by the UV photons coming from the hot central star and by the shocks associated with its high-velocity winds. All the infrared bands arise from a region with kinetic temperatures between 200 and 250 K, probably the photodissociation region associated with the dense torus that surrounds the central star. C 4 H 2 and C 6 H 2 have also been detected in CRL 2688, so it seems that C-rich proto-planetary nebulae are the best organic chemistry factories in space.

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Section: Resultsmentioning

confidence: 90%

[ITAL]Infrared Space Observatory's[/ITAL] Discovery of C[TINF]4[/TINF]H[TINF]2[/TINF], C[TINF]6[/TINF]H[TINF]2[/TINF], and Benzene in CRL 618

Cernicharo

Heras

Tielens³

et al. 2001

The Astrophysical Journal

527

121

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show abstract

“…Line parameters for C 2 H 2 and CO 2 were obtained from the Geisa databank (Jacquinet-Husson et al 1999). Those for C 6 H 6 were provided to us by M. Dang-Nhu (personal communication, 1990); they were derived from molecular constants from Lindemayer et al (1988) and integrated band intensities from Dang-Nhu and Pliva (1989). We used a Lorentz halfwidth of 0.11 cm −1 atm −1 at 296 K varying as T −0.75 , which agrees with laboratory measurements of C 6 H 6 broadening by air and He (Waschull et al 1998).…”

Section: Radiative Transfer Modelingmentioning

confidence: 99%

Benzene on the Giant Planets*1

Bézard¹

2001

Icarus

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“…High-resolution Raman and infrared spectra have been used to determine the molecular structure in the electronic ground state [1][2][3]. A high-resolution Fourier transform spectrometer and a tunable infrared laser spectrometer have been used to study many vibrational bands in the ground state, and accuracies of the molecular constants have been improved [3][4][5][6][7]. Resolutions of these spectra were limited by a Doppler width.…”

Section: Introductionmentioning

confidence: 99%