Source code for gammapy.modeling.models.spectral_crab

# Licensed under a 3-clause BSD style license - see LICENSE.rst
import numpy as np
from astropy import units as u
from gammapy.modeling import Parameter
from .spectral import (
    ExpCutoffPowerLawSpectralModel,
    LogParabolaSpectralModel,
    PowerLawSpectralModel,
    SpectralModel,
)

__all__ = [
    "create_crab_spectral_model",
    "MeyerCrabSpectralModel",
]


[docs]class MeyerCrabSpectralModel(SpectralModel): """Meyer 2010 log polynomial Crab spectral model. Reference: https://ui.adsabs.harvard.edu/abs/2010A%26A...523A...2M, Appendix D """ norm = Parameter("norm", value=1, frozen=True, is_norm=True) coefficients = [-0.00449161, 0, 0.0473174, -0.179475, -0.53616, -10.2708]
[docs] @staticmethod def evaluate(energy, norm): polynomial = np.poly1d(MeyerCrabSpectralModel.coefficients) log_energy = np.log10(energy.to_value("TeV")) log_flux = polynomial(log_energy) flux = u.Quantity(np.power(10, log_flux), "erg / (cm2 s)", copy=False) return norm * flux / energy**2
[docs]def create_crab_spectral_model(reference="meyer"): """Create a Crab nebula reference 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', https://ui.adsabs.harvard.edu/abs/2010A%26A...523A...2M, Appendix D * 'hegra', https://ui.adsabs.harvard.edu/abs/2000ApJ...539..317A * 'hess_pl' and 'hess_ecpl': https://ui.adsabs.harvard.edu/abs/2006A%26A...457..899A * 'magic_lp' and 'magic_ecpl': https://ui.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.modeling.models import PowerLaw, create_crab_spectral_model Plot the 'hess_ecpl' reference Crab spectrum between 1 TeV and 100 TeV:: crab_hess_ecpl = create_crab_spectral_model('hess_ecpl') crab_hess_ecpl.plot([1, 100] * u.TeV) Use a reference crab spectrum as unit to measure a differential flux (at 10 TeV):: >>> pwl = PowerLawSpectralModel( index=2.3, amplitude=1e-12 * u.Unit('1 / (cm2 s TeV)'), reference=1 * u.TeV ) >>> crab = create_crab_spectral_model('hess_pl') >>> energy = 10 * u.TeV >>> dnde_cu = (pwl(energy) / crab(energy)).to('%') >>> print(dnde_cu) 6.196991563774588 % 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) 3.535058216604496 % """ if reference == "meyer": return MeyerCrabSpectralModel() elif reference == "hegra": return PowerLawSpectralModel( amplitude=2.83e-11 * u.Unit("1 / (cm2 s TeV)"), index=2.62, reference=1 * u.TeV, ) elif reference == "hess_pl": return PowerLawSpectralModel( amplitude=3.45e-11 * u.Unit("1 / (cm2 s TeV)"), index=2.63, reference=1 * u.TeV, ) elif reference == "hess_ecpl": return ExpCutoffPowerLawSpectralModel( amplitude=3.76e-11 * u.Unit("1 / (cm2 s TeV)"), index=2.39, lambda_=1 / (14.3 * u.TeV), reference=1 * u.TeV, ) elif reference == "magic_lp": return LogParabolaSpectralModel( amplitude=3.23e-11 * u.Unit("1 / (cm2 s TeV)"), alpha=2.47, beta=0.24 / np.log(10), reference=1 * u.TeV, ) elif reference == "magic_ecpl": return ExpCutoffPowerLawSpectralModel( amplitude=3.80e-11 * u.Unit("1 / (cm2 s TeV)"), index=2.21, lambda_=1 / (6.0 * u.TeV), reference=1 * u.TeV, ) else: raise ValueError(f"Invalid reference: {reference!r}")