Revised molecular constants and term values for the X2Π state of CH

Colin, Réginald; Bernath, Peter F.

doi:10.1016/j.jms.2010.06.013

Cited by 14 publications

(10 citation statements)

References 11 publications

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“…The constants we obtained are presented in Table 4. They are consistent with the work of Colin & Bernath (2010), as we included their data in our fit. Moreover, thanks to our observations of high J A-X transitions (see Fig.…”

Section: Revised Molecular Constants For 12 Chsupporting

confidence: 83%

“…Laboratory data was collected from the literature. For the X 2 Π fundamental state, we used the observations of Colin & Bernath (2010) of the ro-vibrational transitions in the ACE (Atmospheric Chemical Experiment; Bernath et al 2005) solar spectrum. The quality and resolution of this spectrum is close to laboratory standard (0.02 cm −1 in line position accuracy) and the 777 observed transitions allowed an accurate determination of the X 2 Π state constants up to v = 5.…”

Section: Observed Transitionsmentioning

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: Revised Molecular Constants For 12 Chsupporting

confidence: 83%

Section: Observed Transitionsmentioning

confidence: 99%

CH in stellar atmospheres: an extensive linelist

Masseron

Plez

Eck

et al. 2014

A&A

256

216

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“…The atomic line lists used in Coelho's models are a combination of lists from Coelho et al (2005), Castelli (2005a), and Castelli (2005b). In this work we adopt the same molecular opacities as in Coelho (2014), with the following updates 3 : C 2 D-A (from Brooke et al 2013), CH (from Johnson et al 2014, with energy levels substituted from Zachwieja 1995;Zachwieja 1997;Colin & Bernath 2010;Bembenek, Kepa & Rytel 1997;Kepa et al 1996), and CN A-X and B-X (from Brooke et al 2014). During the progress of this work, we identified that the file regarding the transition D-A of the molecule C 2 used in Coelho (2014) was corrupted.…”

Section: Coelhomentioning

confidence: 99%

Stellar spectral models compared with empirical data

Knowles

Sansom

Coelho

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The empirical MILES stellar library is used to test the accuracy of three different, state-of-theart, theoretical model libraries of stellar spectra. These models are widely used in the literature for stellar population analysis. A differential approach is used so that responses to elemental abundance changes are tested rather than absolute levels of the theoretical spectra. First we directly compare model line strengths and spectra to empirical data to investigate trends. Then we test how well line strengths match when element response functions are used to account for changes in [α/Fe] abundances. The aim is to find out where models best represent real star spectra, in a differential way, and hence identify good choices of models to use in stellar population analysis involving abundance patterns. We find that most spectral line strengths are well represented by these models, particularly iron-and sodium-sensitive indices. Exceptions include the higher order Balmer lines (Hδ, Hγ), in which the models show more variation than the data, particularly at low temperatures. C 2 4668 is systematically underestimated by the models compared to observations. We find that differences between these models are generally less significant than the ways in which models vary from the data. Corrections to C 2 line lists for one set of models are identified, improving them for future use.

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“…In the case of OH, NH, and CH, the new infrared solar atlas (Hase et al 2010) measured by the Atmospheric Chemistry Experiment (ACE) infrared Fourier transform spectrometer from orbit ) has led to an improvement in the spectroscopy. The infrared Fraunhofer lines were combined with laboratory measurements to extend the measured line positions to higher vibrational and rotational quantum numbers for OH (Bernath & Colin 2009), NH (Ram & Bernath 2010), and CH (Colin & Bernath 2010).…”

Section: Diatomic Moleculesmentioning

confidence: 99%

Division Xii/Commission 14/Working Group on Molecular Data

Federman¹,

Bernath²,

Müller³

2011

Proc. IAU

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The current report covers the period from the second half of 2003 to the first half of 2011, bringing the Working Group's efforts up to date, and is divided into three main sections covering rotational, vibrational, and electronic spectroscopy. Rather than being exhaustive, space limitations only allow us to highlight a representative sample of work on molecular spectra. Related research on collisions, reactions on grain surfaces, and astrochemistry appear in the report by another Working Group. These also recount recent conferences and workshops on molecular astrophysics.

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Revised molecular constants and term values for the X2Π state of CH

Cited by 14 publications

References 11 publications

CH in stellar atmospheres: an extensive linelist

CH in stellar atmospheres: an extensive linelist

Stellar spectral models compared with empirical data

Division Xii/Commission 14/Working Group on Molecular Data

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