Optimized computation of the voigt and complex probability functions

Humlíček, Josef

doi:10.1016/0022-4073(82)90078-4

Cited by 424 publications

(205 citation statements)

References 4 publications

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“…To obtain f, the measured profiles were fitted by a Voigt profile Vh(E) using the parameterization of Humlicek [54] implemented in the software package IGOR Pro 6. The Gaussian contribution h,G to the width of Vh(E) was corrected by the Gaussian shaped broadening g,G caused by the experimental setup:…”

Section: Calculation Of Crystallite Sizementioning

confidence: 99%

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Phase-transition-driven growth of compound semiconductor crystals from ordered metastable nanorods

et al. 2014

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Section: Calculation Of Crystallite Sizementioning

confidence: 99%

“…The total integral width of the physical Voigt profile f was calculated from the Gauss and the Lorentz width f,G and f,L with the help of the parameterization of Humlicek [54].…”

Section: Calculation Of Crystallite Sizementioning

confidence: 99%

Phase-transition-driven growth of compound semiconductor crystals from ordered metastable nanorods

et al. 2014

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“…For the calculation of the Voigt line shape function, MIRART uses an optimized combination of the Humlicek [Humlicek, 1982] and Hui-Armstrong-Wray [Hui et al, 1978] complex error function algorithm [Schreier, 1992] and switches to pure Lorentz line shape in the far wings; a further optimization similar in spirit to the work of Kuntz [1997] exploits the equidistant wave number grid. The wave number grid is chosen individually for each altitude level and molecule.…”

Section: A6 Modular Infrared Atmospheric Radiative Transfer (Mirart)mentioning

confidence: 99%

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

et al. 2005

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[1] We compare a number of radiative transfer models for atmospheric sounding in the millimeter and submillimeter wavelength range, check their consistency, and investigate their deviations from each other. This intercomparison deals with three different aspects of radiative transfer models: (1) the inherent physics of gaseous absorption lines and how they are modeled, (2) the calculation of absorption coefficients, and (3) the full calculation of radiative transfer for different geometries, i.e., up-looking, down-looking, and limblooking. The correctness and consistency of the implementations are tested by comparing calculations with predefined input such as spectroscopic data, line shape, continuum absorption model, and frequency grid. The absorption coefficients and brightness temperatures calculated by the different models are generally within about 1% of each other. Furthermore, the variability or uncertainty of the model results is estimated if (except for the atmospheric scenario) the input such as spectroscopic data, line shape, and continuum absorption model could be chosen freely. Here the models deviate from each other by about 10% around the center of major absorption lines. The main cause of such discrepancies is the variability of reported spectroscopic data for line absorption and of the continuum absorption model. Further possible causes of discrepancies are different frequency and pressure grids and differences in the corresponding interpolation routines, as well as differences in the line shape functions used, namely a prefactor of (n/n 0 ) or (n/n 0 ) 2 of the Van-Vleck-Weisskopf line shape function. Whether or not the discrepancies affect retrieval results remains to be investigated for each application individually.Citation: Melsheimer, C., et al. (2005), Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range, Radio Sci., 40, RS1007,

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“…There are several approximate methods for computing Voigt profiles available in the literature (e.g. Humlícek 1982;Weideman 1994;Zaghloul & Ali 2012). Also, much effort is spend succesfully on making these approximate methods faster and more accurate (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Random sampling technique for ultra-fast computations of molecular opacities for exoplanet atmospheres

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2017

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Context. Opacities of molecules in exoplanet atmospheres rely on increasingly detailed line-lists for these molecules. The line lists available today contain for many species up to several billions of lines. Computation of the spectral line profile created by pressure and temperature broadening, the Voigt profile, of all of these lines is becoming a computational challenge. Aims. We aim to create a method to compute the Voigt profile in a way that automatically focusses the computation time into the strongest lines, while still maintaining the continuum contribution of the high number of weaker lines. Methods. Here, we outline a statistical line sampling technique that samples the Voigt profile quickly and with high accuracy. The number of samples is adjusted to the strength of the line and the local spectral line density. This automatically provides high accuracy line shapes for strong lines or lines that are spectrally isolated. The line sampling technique automatically preserves the integrated line opacity for all lines, thereby also providing the continuum opacity created by the large number of weak lines at very low computational cost. Results. The line sampling technique is tested for accuracy when computing line spectra and correlated-k tables. Extremely fast computations (∼ 3.5 · 10 5 lines per second per core on a standard current day desktop computer) with high accuracy (≤ 1% almost everywhere) are obtained. A detailed recipe on how to perform the computations is given.

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Optimized computation of the voigt and complex probability functions

Cited by 424 publications

References 4 publications

Phase-transition-driven growth of compound semiconductor crystals from ordered metastable nanorods

Phase-transition-driven growth of compound semiconductor crystals from ordered metastable nanorods

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

Random sampling technique for ultra-fast computations of molecular opacities for exoplanet atmospheres

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