As the attenuation law is not universal, one should use a model allowing different UV slope, 2175 bump strength whenever the spectral coverage allows it. For this purpose, one of the most used recipe is the one of Noll+09.
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In particular cases, for instance the SED fitting of a galaxy known to be starburst and a lack of rest-frame UV data, the Calzetti law can be used.
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One should always avoid to use recipe derived from measurements of individual stars (i.e extinction curves) such as the average LMC, SMC or MW extinction laws.
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The functional forms of FM90 or CCM89 are just analytical formulas and so even if they were initially applied to measurement of individual stars they could in principle also be used for galaxies. The FM recipe has a lot of parameters to fit though and setting the parameters to average values derived from measurement of individual stars is not recommended as the physical processes at stake are not the same.
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The Charlot and Fall 2000 recipe is dependent on the star formation history
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Attenuation curves derived with radiative transfer models are described by physically motivated parameters related to the structure of the ISM: dust/star geometry, local distribution of dust, type of dust grain, optical depth.
As the attenuation law is not universal, one should use a model allowing different UV slope, 2175 bump strength whenever the spectral coverage allows it. For this purpose, one of the most used recipe is the one of Noll+09.
In particular cases, for instance the SED fitting of a galaxy known to be starburst and a lack of rest-frame UV data, the Calzetti law can be used.
One should always avoid to use recipe derived from measurements of individual stars (i.e extinction curves) such as the average LMC, SMC or MW extinction laws.
The functional forms of FM90 or CCM89 are just analytical formulas and so even if they were initially applied to measurement of individual stars they could in principle also be used for galaxies. The FM recipe has a lot of parameters to fit though and setting the parameters to average values derived from measurement of individual stars is not recommended as the physical processes at stake are not the same.
The Charlot and Fall 2000 recipe is dependent on the star formation history
Attenuation curves derived with radiative transfer models are described by physically motivated parameters related to the structure of the ISM: dust/star geometry, local distribution of dust, type of dust grain, optical depth.