BlackBody

class sherpa.astro.optical.BlackBody(name='blackbody')

Bases: sherpa.models.model.ArithmeticModel

Emission from a black body.

It is for use when the independent axis is in Angstroms.

refer

The reference point, in Angstroms.

ampl

The amplitude of the emission; it is defined at the reference point but its numerical value there also depends on the temperature.

temperature

The temperature in Kelvin.

See also

Bremsstrahlung

Notes

The functional form of the model for points is:

f(x) = ampl * g(refer) / g(x)

g(x) = x^5 * (exp(1.438786E8 / temperature / x) - 1)

and for integrated data sets the low-edge of the grid is used.

Attributes Summary

thawedparhardmaxes
thawedparhardmins
thawedparmaxes
thawedparmins
thawedpars

Methods Summary

apply(outer, \*otherargs, \*\*otherkwargs)
calc(p, x[, xhi])
get_center()
guess(dep, \*args, \*\*kwargs)	Set an initial guess for the parameter values.
reset()
set_center(\*args, \*\*kwargs)
startup()
teardown()

Attributes Documentation

thawedparhardmaxes

thawedparhardmins

thawedparmaxes

thawedparmins

thawedpars

Methods Documentation

apply(outer, *otherargs, **otherkwargs)

calc(p, x, xhi=None, **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.

reset()

set_center(*args, **kwargs)

startup()

teardown()