Cardelli89¶
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class
beast.physicsmodel.dust.extinction.
Cardelli89
[source]¶ Bases:
beast.physicsmodel.dust.extinction.ExtinctionLaw
Cardelli89 Milky Way R(V) dependent Extinction Law
From Cardelli, Clayton, and Mathis (1989, ApJ, 345, 245).
Fitzpatrick99 should be used instead except for historical puposes as this newer law is based on 10x more observations and a better treatment of the optical/NIR photometry based portion of the curves.
Methods Summary
function
(lamb[, Av, Rv, Alambda])Cardelli89 extinction Law Methods Documentation
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function
(lamb, Av=1.0, Rv=3.1, Alambda=True, **kwargs)[source]¶ Cardelli89 extinction Law
Parameters: lamb: float or ndarray(dtype=float)
wavelength [in Angstroms] at which evaluate the law.
Av: float
desired A(V) (default: 1.0)
Rv: float
desired R(V) (default: 3.1)
Alambda: bool
if set returns +2.5*1./log(10.)*tau, tau otherwise
Returns: r: float or ndarray(dtype=float)
attenuation as a function of wavelength depending on Alambda option +2.5*1./log(10.)*tau, or tau
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