Analysis of the 0–0 Band of theC2Σ+–X2Π Band System in the12CH and13CH Isotopic Radicals

Bembenek, Z.; Ruan, Ke; Rytel, M.

doi:10.1006/jmsp.1996.7246

Cited by 15 publications

(18 citation statements)

References 22 publications

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“…As our identifications carry a lower accuracy than laboratory measurements, we did not attempt to use these lines in our global fit. However, thanks to the inclusion of more recent laboratory data from and Bembenek et al (1997) compared to Jorgensen et al (1996), we were able to improve the C−X linelist (see Fig. 4).…”

Section: Notesmentioning

confidence: 94%

“…Using our calculated levels up to the dissociation energy limit, we compute the partition function Q following Tatum (1966), Bembenek et al (1997). where T is the temperature, g i = 2J + 1 is the multiplicity of a single Λ-doubling rotational level of energy E i , and k is the Boltzmann constant. For the X 2 Π, A 2 Δ, B 2 Σ − , and C 2 Σ + states we used the constants derived in this work.…”

Section: Partition Functionmentioning

confidence: 99%

“…When the same line was present in different studies, we favoured the value from the most accurate measurement. For the C 2 Σ + -X 2 Π transition, we used the experimental data from Bembenek et al (1997;56 lines), Ubachs et al (1986;35 lines), and Heimer (1932;159 lines) for the 0−0 transition with respective accuracies of 0.02 cm −1 , 0.003 cm −1 , 0.2 cm −1 , and 124 lines) for the 1−1 transition with an accuracy of 0.05 cm −1 , and Herzberg & Johns (1969;42 lines) for the 2−2 transition, with an accuracy of 0.2 cm −1 . Some line assignments from these papers did not correspond to the identification we could make with PGopher.…”

Section: Ch Laboratory Datamentioning

confidence: 99%

“…The experimental data were taken from Zachwieja (1997), Para (1996), and Bembenek et al (1997;see Sect. 3.2).…”

Section: Revised Molecular Constants Formentioning

confidence: 99%

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CH in stellar atmospheres: an extensive linelist

Masseron

Plez

Eck

et al. 2014

A&A

256

216

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The advent of high-resolution spectrographs and detailed stellar atmosphere modelling has strengthened the need for accurate molecular data. Carbon-enhanced metal-poor (CEMP) stars spectra are interesting objects with which to study transitions from the CH molecule. We combine programs for spectral analysis of molecules and stellar-radiative transfer codes to build an extensive CH linelist, including predissociation broadening as well as newly identified levels. We show examples of strong predissociation CH lines in CEMP stars, and we stress the important role played by the CH features in the Bond-Neff feature depressing the spectra of barium stars by as much as 0.2 mag in the λ = 3000−5500 Å range. Because of the extreme thermodynamic conditions prevailing in stellar atmospheres (compared to the laboratory), molecular transitions with high energy levels can be observed. Stellar spectra can thus be used to constrain and improve molecular data.

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Section: Notesmentioning

confidence: 94%

Section: Partition Functionmentioning

confidence: 99%

Section: Ch Laboratory Datamentioning

confidence: 99%

“…The experimental data were taken from Zachwieja (1997), Para (1996), and Bembenek et al (1997;see Sect. 3.2).…”

Section: Revised Molecular Constants Formentioning

confidence: 99%

See 2 more Smart Citations

CH in stellar atmospheres: an extensive linelist

Masseron

Plez

Eck

et al. 2014

A&A

256

216

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“…Table 3: Measured transition frequencies of the 0-0 vibronic band of the C 2 Σ + -X 2 Π transition of CH (in cm -1 ). a: Ubachs et al [23], b: Bembenek et al [24], c: This work, d: Heimer [21] Satellite lines included in the fit: R12ee(0. [22]; all other lines from this work…”

Section: Acknowledgementmentioning

confidence: 99%

Cavity ring-down UV spectroscopy of the C2Σ+-X2Π electronic transition of CH

Linnartz

Ubachs

2019

Journal of Molecular Spectroscopy

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Rotationally resolved spectra of the C 2 Σ + -X 2 Π electronic system of the CH radical were measured using cavity ring-down spectroscopy in supersonically expanding, planar hydrocarbon plasma. The experimental conditions allowed the study of highly excited rotational levels starting from vibrationally excited states. Here we present some 200+ new or more accurately recorded transitions in the 0-0, 1-1 and 2-2 vibronic bands in the ultraviolet between 30900-32400 cm -1 (324-309 nm). The resulting data, compared to earlier measurements, allows for the determination of more precise molecular constants for each vibrational state and therefore more precise equilibrium values. From this an equilibrium bond length of 1.115798(17) Å for the C 2 Σ + state is determined. A comprehensive list with observed transitions for each band has been compiled from all available experimental studies and constraints are placed on the predissociation lifetimes.

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