The sherpa.astro.optical module
Optical models intended for SED Analysis
The models match those used by the SpecView application 1, and are intended for un-binned one-dimensional data sets defined on a wavelength grid, with units of Angstroms. When used with a binned data set the lower-edge of each bin is used to evaluate the model. This module does not contain all the spectral components from SpecView (2).
References
Classes
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Optical model of an absorption edge. |
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Gaussian function for modeling absorption (equivalent width). |
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Lorentz function for modeling absorption (equivalent width). |
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This model has been replaced by Voigt1D |
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A model of emission due to an accretion disk. |
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Emission from a black body as a function of wavelength. |
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Bremsstrahlung emission. |
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Broken power-law model. |
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Galactic extinction: the Cardelli, Clayton, and Mathis model. |
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Gaussian function for modeling emission. |
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Lorentz function for modeling emission. |
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This model has been replaced by Voigt1D |
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UV extinction curve: Fitzpatrick and Massa 1988. |
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LMC extinction: the Howarth model. |
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Gaussian function for modeling absorption (log of fwhm). |
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Gaussian function for modeling emission (log of fwhm). |
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Gaussian function for modeling absorption (optical depth). |
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Polynomial model of order 5. |
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Power-law model. |
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Optically-thin recombination continuum model. |
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Galactic extinction: the Savage & Mathis model. |
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SMC extinction: the Prevot et al. 1984 model. |
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Galactic extinction: the Seaton model from Synphot. |
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Extragalactic extinction: Calzetti, Kinney and Storchi-Bergmann |