Calzetti00¶
-
class
beast.physicsmodel.dust.attenuation.
Calzetti00
[source]¶ Bases:
beast.physicsmodel.dust.extinction.ExtinctionLaw
Calzetti et al. (2000, ApJ 533, 682) developed a recipe for dereddening the spectra of galaxies where massive stars dominate the radiation output, valid between 0.12 to 2.2 microns. Extrapolation down to 0.0912 microns
Note that the supplied color excess should be that derived for the stellar continuum,
EBV(stars)
, which is related to the reddening derived from the gas,EBV(gas)
, via the Balmer decrement byEBV(stars) = 0.44 times EBV(gas)
R_V
- Ratio of total to selective extinction, default is 4.05. Calzetti et al. (2000) estimateR_V = 4.05 +/- 0.80
from optical-IR observations of 4 starbursts.Methods Summary
function
(lamb[, Av, Rv, Alambda])Returns A(lambda) or tau for the Calzetti Law Methods Documentation
-
function
(lamb, Av=1, Rv=4.05, Alambda=True, **kwargs)[source]¶ Returns A(lambda) or tau for the Calzetti 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 4.05)
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
-