BBodyFreq

class sherpa.astro.models.BBodyFreq(name='bbodyfreq')

Bases: sherpa.models.model.RegriddableModel1D

A one-dimensional Blackbody model (frequency).

This model can be used when the independent axis is in frequency space.

T

The temperature if the blackbody, in Kelvin.

ampl

The amplitude of the blackbody component.

See also

BBody

Notes

The blackbody emission is calculated as a function of frequency (v) using Wien’s law (hv >> kT):

f(v) = ampl * 2 * h * v^3 * exp(-h * v / (k * T)) / c^2

where T is the blackbody temperature in Kelvin, h is Planck’s constant, k is Boltzmann’s constant, and c the speed of light.

Attributes Summary

thawedparhardmaxes
thawedparhardmins
thawedparmaxes
thawedparmins
thawedpars

Methods Summary

apply(outer, *otherargs, **otherkwargs)
calc(pars, xlo, *args, **kwargs)
get_center()
guess(dep, *args, **kwargs)	Set an initial guess for the parameter values.
regrid(*arrays)
reset()
set_center(*args, **kwargs)
startup()	Called before a model may be evaluated multiple times.
teardown()	Called after a model may be evaluated multiple times.

Attributes Documentation

thawedparhardmaxes

thawedparhardmins

thawedparmaxes

thawedparmins

thawedpars

Methods Documentation

apply(outer, *otherargs, **otherkwargs)

calc(pars, xlo, *args, **kwargs)

get_center()

guess(dep, *args, **kwargs)

Set an initial guess for the parameter values.

Attempt to set the parameter values, and ranges, for the model to match the data values. This is intended as a rough guess, so it is expected that the model is only evaluated a small number of times, if at all.

regrid(*arrays)

reset()

set_center(*args, **kwargs)

startup()

Called before a model may be evaluated multiple times.

See also

teardown()

teardown()

Called after a model may be evaluated multiple times.

See also

setup()