New Spectroscopic Analysis of theB2Σ−–X2Π Band System of the CH Molecule

Kępa, R.; Para, Andrzej; Rytel, M.; Zachwieja, M.

doi:10.1006/jmsp.1996.0173

Cited by 52 publications

(40 citation statements)

References 3 publications

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“…We were able to determine for the first time the constants for the A 2 Δ v = 4 and v = 5 states. For the B−X transition (Table A.3), we observed transitions from higher J levels than Kepa (1996) and Bernath et al (1991;J < 15.5), and than Kumar et al (1998;J < 21.5). For the C−X transition, we also observe lines to higher rotational levels in our CEMP star spectrum than in laboratory spectra.…”

Section: Stellar Observations and Modellingmentioning

confidence: 80%

“…Assuming this barrier height, B 2 Σ − v = 1 levels have been included up to J = 20.5 in our list, although we were able to identify B−X transitions only up to J = 16.5 because the combination of low g f values and large predissociation broadening A47, page 7 of 29 A&A 571, A47 (2014) (a) Constants derived by Kepa (1996). …”

Section: The Bmentioning

confidence: 99%

“…For the A 2 Δ-X 2 Π transition, we merged the laboratory measurements of Bernath et al (1991) and Zachwieja (1995), with an average accuracy of 0.005 cm −1 over 665 and 432 observed transitions, respectively. The experimental data for the B 2 Σ − -X 2 Π transition was taken from Kepa (1996), Kumar et al (1998), andBernath et al (1991), with respective accuracies (and number of lines) of 0.015 cm −1 (169), 0.01 cm −1 (73), and 0.005 cm −1 (126). When the same line was present in different studies, we favoured the value from the most accurate measurement.…”

Section: Ch Laboratory Datamentioning

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: Stellar Observations and Modellingmentioning

confidence: 80%

Section: The Bmentioning

confidence: 99%

Section: Ch Laboratory Datamentioning

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 extensive study of the CH molecule was also presented by Lien (1984). The CH B-X (1, 0) band measured in the laboratory by Gerö (1941), Brooks & Smith (1974), Brzozowski et al (1976), Garland & Crosley (1985), Bernath et al (1991), Kȩpa et al (1996) and observed in the solar spectrum near 3633Å (see Grevesse & Sauval 1973). The first detection of the absorption CH B-X (1, 0) band of interstellar origin was reported by Meyer (1990) who observed the band towards HD 21483.…”

Section: Introductionmentioning

confidence: 99%

On the CH B‐X (1, 0) band in translucent clouds

et al. 2011

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We present observations of CH B-X (1, 0) band toward 13 translucent sightlines. The given precise positions (at 3627.403, 3633.289, 3636.222Å) are derived by means of shifting our spectra to the rest velocity frame using B-X (0, 0) features (at 3878, 3886 and 3890Å). The proposed oscillator strengths (equal to 0.00035, 0.00104, 0.00069, respectively) are based on f -values of the CH B-X (0, 0) system, i.e. 0.00110, 0.00320, 0.00210.

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“…Several channels lead to the formation of CH and N 2 , and are listed along with ⌬H 0 for each reaction. ⌬H 0 for channel ͑3͒ was determined in this study; for the other channels, it was calculated from previously published spectroscopic data on CH: [32][33][34][35] …”

Section: Introductionmentioning

confidence: 99%

Photodissociation dynamics of the HCNN radical

Faulhaber

Gascooke

Hoops

et al. 2006

The Journal of Chemical Physics

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The photodissociation dynamics of the diazomethyl ͑HCNN͒ radical have been studied using fast radical beam photofragment translational spectroscopy. A photofragment yield spectrum was obtained for the range of 25 510-40 820 cm −1 , and photodissociation was shown to occur for energies above 25 600 cm −1 . The only product channel observed was the formation of CH and N 2 . Fragment translational energy and angular distributions were obtained at several energies in the range covered by the photofragment yield spectrum. The fragment translational energy distributions showed at least two distinct features at energies up to 4.59 eV, and were not well fit by phase space theory at any of the excitation energies studied. A revised C-N bond dissociation energy and heat of formation for HCNN, D 0 ͑HC-NN͒ = 1.139± 0.019 eV and ⌬ f H 0 ͑HCNN͒ = 5.010± 0.023 eV, were determined.

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New Spectroscopic Analysis of theB2Σ−–X2Π Band System of the CH Molecule

Cited by 52 publications

References 3 publications

CH in stellar atmospheres: an extensive linelist

CH in stellar atmospheres: an extensive linelist

On the CH B‐X (1, 0) band in translucent clouds

Photodissociation dynamics of the HCNN radical

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