CrabSpectrum

class gammapy.spectrum.CrabSpectrum(reference='meyer')

Bases: object

Crab nebula spectral model.

The Crab nebula is often used as a standard candle in gamma-ray astronomy. Fluxes and sensitivities are often quoted relative to the Crab spectrum.

The following references are available:

• ‘meyer’, http://adsabs.harvard.edu/abs/2010A%26A…523A…2M, Appendix D
• ‘hegra’, http://adsabs.harvard.edu/abs/2000ApJ…539..317A
• ‘hess_pl’ and ‘hess_ecpl’: http://adsabs.harvard.edu/abs/2006A%26A…457..899A
• ‘magic_lp’ and ‘magic_ecpl’: http://adsabs.harvard.edu/abs/2015JHEAp…5…30A

Parameters:

reference : {‘meyer’, ‘hegra’, ‘hess_pl’, ‘hess_ecpl’, ‘magic_lp’, ‘magic_ecpl’}

Which reference to use for the spectral model.

Examples

Let’s first import what we need:

import astropy.units as u
from gammapy.spectrum import CrabSpectrum
from gammapy.spectrum.models import PowerLaw

Plot the ‘hess_ecpl’ reference Crab spectrum between 1 TeV and 100 TeV:

crab_hess_ecpl = CrabSpectrum('hess_ecpl')
crab_hess_ecpl.model.plot([1, 100] * u.TeV)

Use a reference crab spectrum as unit to measure a differential flux (at 10 TeV):

>>> pwl = PowerLaw(index=2.3, amplitude=1e-12 * u.Unit('1 / (cm2 s TeV)'), reference=1 * u.TeV)
>>> crab = CrabSpectrum('hess_pl').model
>>> energy = 10 * u.TeV
>>> dnde_cu = (pwl(energy) / crab(energy)).to('%')
>>> print(dnde_cu)
6.19699156377 %

And the same for integral fluxes (between 1 and 10 TeV):

>>> # compute integral flux in crab units
>>> emin, emax = [1, 10] * u.TeV
>>> flux_int_cu = (pwl.integral(emin, emax) / crab.integral(emin, emax)).to('%')
>>> print(flux_int_cu)
3.5350582166 %

Attributes Summary

references

Available references (see class docstring).

Attributes Documentation

references = ['meyer', 'hegra', 'hess_pl', 'hess_ecpl', 'magic_lp', 'magic_ecpl']

Available references (see class docstring).