Cardelli89¶
- class beast.physicsmodel.dust.extinction.Cardelli89[source]¶
Bases:
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 purposes 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
- 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 to 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