astromodels.functions.functions_1D.extinction module

class astromodels.functions.functions_1D.extinction.Standard_Rv(value)[source]

Bases: Enum

An enumeration.

LMC = 3.16
MW = 3.08
SMC = 2.93
class astromodels.functions.functions_1D.extinction.ZDust(**kwargs)[source]

Bases: Function1D

description :

Extinction by dust grains from Pei (1992), suitable for IR, optical and UV energy bands, including the full energy ranges of the Swift UVOT and XMM-Newton OM detectors. Three models are included which characterize the extinction curves of (1) the Milky Way, (2) the LMC and (3) the SMC. The models can be modified by redshift and can therefore be applied to extragalactic sources. The transmission is set to unity shortward of 912 Angstroms in the rest frame of the dust. This is incorrect physically but does allow the model to be used in combination with an X-ray photoelectric absorption model such as phabs. Parameter 1 (method) describes which extinction curve (MW, LMC or SMC) will be constructed and should never be allowed to float during a fit. The extinction at V, A(V) = E(B-V) x Rv. Rv should typically remain frozen for a fit. Standard values for Rv are MW = 3.08, LMC = 3.16 and SMC = 2.93 (from table 2 of Pei 1992), although these may not be applicable to more distant dusty sources.

parameters :
e_bmv :

desc : color excess initial value : 1.0 min: 0 is_normalization : False delta : 0.1

rv :

desc : ratio of total to selective extinction initial value : 3.08 is_normalization : False delta : 0.1 fix: True

redshift :

desc : the redshift of the source initial value : 0. is_normalization : False min : 0 max : 15 delta : 0.1 fix: True


desc: the abundance table for the model initial value: mw allowed values: - mw - lmc - smc

function: _set_extinction_law

evaluate(x, e_bmv, rv, redshift)[source]
static info()
astromodels.functions.functions_1D.extinction.ms_dust(x, e_bmv, rv, a, lamb, b, n)[source]
astromodels.functions.functions_1D.extinction.ms_dust_xspec(x, e_bmv, rv, a, lamb, b, n)[source]
astromodels.functions.functions_1D.extinction.pei(rlambda, a_b, a, lamb, b, n) float[source]

ported from XSPEC originally by