FM

class sherpa.astro.optical.FM(name='fm')

Bases: sherpa.models.model.ArithmeticModel

UV extinction curve: Fitzpatrick and Massa 1988.

The UV extinction is calculated using [1]. This model is intended to be used to modify another model (e.g. by multiplying the two together). It is for use when the independent axis is in Angstrom.

ebv

E(B-V)

x0

Position of the Drude bump.

width

Width of the Drude bump.

c1

The intercept of the linear term.

c2

The slope of the linear term.

c3

Normalization of the Drude bump.

c4

Normalization of the FUV curvature.

See also

CCM, LMC, Seaton, SM, SMC, XGAL

Notes

When evaluated on a binned grid, the lower-edges of the bins are used for the calculation.

References

[1]	Fitzpatrick and Massa 1988 http://adsabs.harvard.edu/abs/1988ApJ...328..734F

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()