EBLAbsorptionNormSpectralModel

class gammapy.modeling.models.EBLAbsorptionNormSpectralModel(energy, param, data, redshift, alpha_norm, interp_kwargs=None)

Bases: gammapy.modeling.models.spectral.SpectralModel

Gamma-ray absorption models.

For more information see EBL absorption spectral model.

Parameters

energyQuantity

Energy node values

paramQuantity

Parameter node values

dataQuantity

Model value

redshiftfloat

Redshift of the absorption model

alpha_norm: float

Norm of the EBL model

interp_kwargsdict

Interpolation option passed to ScaledRegularGridInterpolator. By default the models are extrapolated outside the range. To prevent this and raise an error instead use interp_kwargs = {“extrapolate”: False}

Attributes Summary

alpha_norm	A model parameter.
covariance
default_parameters
frozen	Frozen status of a model, True if all parameters are frozen
is_norm_spectral_model	Whether model is a norm spectral model
parameters	Parameters (Parameters)
redshift	A model parameter.
tag
type

Methods Summary

__call__(energy)	Call self as a function.
copy(**kwargs)
energy_flux(energy_min, energy_max, **kwargs)	Compute energy flux in given energy range.
energy_flux_error(energy_min, energy_max[, ...])	Evaluate the error of the energy flux of a given spectrum in
evaluate(energy, redshift, alpha_norm)	Evaluate model for energy and parameter value.
evaluate_error(energy[, epsilon])	Evaluate spectral model with error propagation.
freeze()	Freeze all parameters
from_dict(data)
from_parameters(parameters, **kwargs)	Create model from parameter list
integral(energy_min, energy_max, **kwargs)	Integrate spectral model numerically if no analytical solution defined.
integral_error(energy_min, energy_max[, epsilon])	Evaluate the error of the integral flux of a given spectrum in a given energy range.
inverse(value[, energy_min, energy_max])	Return energy for a given function value of the spectral model.
inverse_all(values[, energy_min, energy_max])	Return energies for multiple function values of the spectral model.
plot(energy_bounds[, ax, sed_type, ...])	Plot spectral model curve.
plot_error(energy_bounds[, ax, sed_type, ...])	Plot spectral model error band.
read(filename[, redshift, alpha_norm, ...])	Build object from an XSPEC model.
read_builtin([reference, redshift, ...])	Read from one of the built-in absorption models.
reassign(datasets_names, new_datasets_names)	Reassign a model from one dataset to another
reference_fluxes(energy_axis)	Get reference fluxes for a given energy axis.
spectral_index(energy[, epsilon])	Compute spectral index at given energy.
to_dict([full_output])	Create dict for YAML serialisation
unfreeze()	Restore parameters frozen status to default

Attributes Documentation

alpha_norm

A model parameter.

Note that the parameter value has been split into a factor and scale like this:

value = factor x scale

Users should interact with the value, quantity or min and max properties and consider the fact that there is a factor` and scale an implementation detail.

That was introduced for numerical stability in parameter and error estimation methods, only in the Gammapy optimiser interface do we interact with the factor, factor_min and factor_max properties, i.e. the optimiser “sees” the well-scaled problem.

Parameters

namestr

Name

valuefloat or Quantity

Value

scalefloat, optional

Scale (sometimes used in fitting)

unitUnit or str, optional

Unit

minfloat, optional

Minimum (sometimes used in fitting)

maxfloat, optional

Maximum (sometimes used in fitting)

frozenbool, optional

Frozen? (used in fitting)

errorfloat

Parameter error

scan_minfloat

Minimum value for the parameter scan. Overwrites scan_n_sigma.

scan_maxfloat

Minimum value for the parameter scan. Overwrites scan_n_sigma.

scan_n_values: int

Number of values to be used for the parameter scan.

scan_n_sigmaint

Number of sigmas to scan.

scan_values: `numpy.array`

Scan values. Overwrites all of the scan keywords before.

scale_method{‘scale10’, ‘factor1’, None}

Method used to set factor and scale

interp{“lin”, “sqrt”, “log”}

Parameter scaling to use for the scan.

is_normbool

Whether the parameter represents the flux norm of the model.

covariance

default_parameters = <gammapy.modeling.parameter.Parameters object>

frozen

Frozen status of a model, True if all parameters are frozen

is_norm_spectral_model

Whether model is a norm spectral model

parameters

Parameters (Parameters)

redshift

A model parameter.

Note that the parameter value has been split into a factor and scale like this:

value = factor x scale

Users should interact with the value, quantity or min and max properties and consider the fact that there is a factor` and scale an implementation detail.

That was introduced for numerical stability in parameter and error estimation methods, only in the Gammapy optimiser interface do we interact with the factor, factor_min and factor_max properties, i.e. the optimiser “sees” the well-scaled problem.

Parameters

namestr

Name

valuefloat or Quantity

Value

scalefloat, optional

Scale (sometimes used in fitting)

unitUnit or str, optional

Unit

minfloat, optional

Minimum (sometimes used in fitting)

maxfloat, optional

Maximum (sometimes used in fitting)

frozenbool, optional

Frozen? (used in fitting)

errorfloat

Parameter error

scan_minfloat

Minimum value for the parameter scan. Overwrites scan_n_sigma.

scan_maxfloat

Minimum value for the parameter scan. Overwrites scan_n_sigma.

scan_n_values: int

Number of values to be used for the parameter scan.

scan_n_sigmaint

Number of sigmas to scan.

scan_values: `numpy.array`

Scan values. Overwrites all of the scan keywords before.

scale_method{‘scale10’, ‘factor1’, None}

Method used to set factor and scale

interp{“lin”, “sqrt”, “log”}

Parameter scaling to use for the scan.

is_normbool

Whether the parameter represents the flux norm of the model.

tag = ['EBLAbsorptionNormSpectralModel', 'ebl-norm']

type

Methods Documentation

__call__(energy)

Call self as a function.

copy(**kwargs)

energy_flux(energy_min, energy_max, **kwargs)

Compute energy flux in given energy range.

\[G(E_{min}, E_{max}) = \int_{E_{min}}^{E_{max}} E \phi(E) dE\]

Parameters

energy_min, energy_maxQuantity

Lower and upper bound of integration range.

**kwargsdict

Keyword arguments passed to func:integrate_spectrum

energy_flux_error(energy_min, energy_max, epsilon=0.0001, **kwargs)

Evaluate the error of the energy flux of a given spectrum in

a given energy range.

Parameters

energy_min, energy_maxQuantity

Lower and upper bound of integration range.

epsilonfloat

Step size of the gradient evaluation. Given as a fraction of the parameter error.

Returns

energy_flux, energy_flux_errtuple of Quantity

Energy flux and energy flux error between energy_min and energy_max.

evaluate(energy, redshift, alpha_norm)

Evaluate model for energy and parameter value.

evaluate_error(energy, epsilon=0.0001)

Evaluate spectral model with error propagation.

Parameters

energyQuantity

Energy at which to evaluate

epsilonfloat

Step size of the gradient evaluation. Given as a fraction of the parameter error.

Returns

dnde, dnde_errortuple of Quantity

Tuple of flux and flux error.

freeze()

Freeze all parameters

classmethod from_dict(data)

classmethod from_parameters(parameters, **kwargs)

Create model from parameter list

Parameters

parametersParameters

Parameters for init

Returns

modelModel

Model instance

integral(energy_min, energy_max, **kwargs)

Integrate spectral model numerically if no analytical solution defined.

\[F(E_{min}, E_{max}) = \int_{E_{min}}^{E_{max}} \phi(E) dE\]

Parameters

energy_min, energy_maxQuantity

Lower and upper bound of integration range.

**kwargsdict

Keyword arguments passed to integrate_spectrum()

integral_error(energy_min, energy_max, epsilon=0.0001, **kwargs)

Evaluate the error of the integral flux of a given spectrum in a given energy range.

Parameters

energy_min, energy_maxQuantity

Lower and upper bound of integration range.

epsilonfloat

Step size of the gradient evaluation. Given as a fraction of the parameter error.

Returns

flux, flux_errtuple of Quantity

Integral flux and flux error between energy_min and energy_max.

inverse(value, energy_min=<Quantity 0.1 TeV>, energy_max=<Quantity 100. TeV>)

Return energy for a given function value of the spectral model.

Calls the scipy.optimize.brentq numerical root finding method.

Parameters

valueQuantity

Function value of the spectral model.

energy_minQuantity

Lower energy bound of the roots finding

energy_maxQuantity

Upper energy bound of the roots finding

Returns

energyQuantity

Energies at which the model has the given value.

inverse_all(values, energy_min=<Quantity 0.1 TeV>, energy_max=<Quantity 100. TeV>)

Return energies for multiple function values of the spectral model.

Calls the scipy.optimize.brentq numerical root finding method.

Parameters

valuesQuantity

Function values of the spectral model.

energy_minQuantity

Lower energy bound of the roots finding

energy_maxQuantity

Upper energy bound of the roots finding

Returns

energylist of Quantity

each element contain the energies at which the model has corresponding value of values.

plot(energy_bounds, ax=None, sed_type='dnde', energy_power=0, n_points=100, **kwargs)

Plot spectral model curve.

kwargs are forwarded to matplotlib.pyplot.plot

By default a log-log scaling of the axes is used, if you want to change the y axis scaling to linear you can use:

from gammapy.modeling.models import ExpCutoffPowerLawSpectralModel
from astropy import units as u

pwl = ExpCutoffPowerLawSpectralModel()
ax = pwl.plot(energy_bounds=(0.1, 100) * u.TeV)
ax.set_yscale('linear')

Parameters

axAxes, optional

Axis

energy_boundsQuantity

Plot energy bounds passed to MapAxis.from_energy_bounds

sed_type{“dnde”, “flux”, “eflux”, “e2dnde”}

Evaluation methods of the model

energy_powerint, optional

Power of energy to multiply flux axis with

n_pointsint, optional

Number of evaluation nodes

**kwargsdict

Keyword arguments forwarded to plot

Returns

axAxes, optional

Axis

plot_error(energy_bounds, ax=None, sed_type='dnde', energy_power=0, n_points=100, **kwargs)

Plot spectral model error band.

Note

This method calls ax.set_yscale("log", nonpositive='clip') and ax.set_xscale("log", nonposx='clip') to create a log-log representation. The additional argument nonposx='clip' avoids artefacts in the plot, when the error band extends to negative values (see also https://github.com/matplotlib/matplotlib/issues/8623).

When you call plt.loglog() or plt.semilogy() explicitly in your plotting code and the error band extends to negative values, it is not shown correctly. To circumvent this issue also use plt.loglog(nonposx='clip', nonpositive='clip') or plt.semilogy(nonpositive='clip').

Parameters

axAxes, optional

Axis

energy_boundsQuantity

Plot energy bounds passed to MapAxis.from_energy_bounds

sed_type{“dnde”, “flux”, “eflux”, “e2dnde”}

Evaluation methods of the model

energy_powerint, optional

Power of energy to multiply flux axis with

n_pointsint, optional

Number of evaluation nodes

**kwargsdict

Keyword arguments forwarded to matplotlib.pyplot.fill_between

Returns

axAxes, optional

Axis

classmethod read(filename, redshift=0.1, alpha_norm=1, interp_kwargs=None)

Build object from an XSPEC model.

Parameters

filenamestr

File containing the model.

redshiftfloat

Redshift of the absorption model

alpha_norm: float

Norm of the EBL model

interp_kwargsdict

Interpolation option passed to ScaledRegularGridInterpolator.

classmethod read_builtin(reference='dominguez', redshift=0.1, alpha_norm=1, interp_kwargs=None)

Read from one of the built-in absorption models.

Parameters

reference{‘franceschini’, ‘dominguez’, ‘finke’}

name of one of the available model in gammapy-data

redshiftfloat

Redshift of the absorption model

alpha_norm: float

Norm of the EBL model

References

1

Franceschini et al., “Extragalactic optical-infrared background radiation, its time evolution and the cosmic photon-photon opacity”, # noqa: E501 Link

2

Dominguez et al., ” Extragalactic background light inferred from AEGIS galaxy-SED-type fractions” # noqa: E501 Link

3

Finke et al., “Modeling the Extragalactic Background Light from Stars and Dust” Link

reassign(datasets_names, new_datasets_names)

Reassign a model from one dataset to another

Parameters

datasets_namesstr or list

Name of the datasets where the model is currently defined

new_datasets_namesstr or list

Name of the datasets where the model should be defined instead. If multiple names are given the two list must have the save length, as the reassignment is element-wise.

Returns

modelModel

Reassigned model.

reference_fluxes(energy_axis)

Get reference fluxes for a given energy axis.

Parameters

energy_axisMapAxis

Energy axis

Returns

fluxesdict of Quantity

Reference fluxes

spectral_index(energy, epsilon=1e-05)

Compute spectral index at given energy.

Parameters

energyQuantity

Energy at which to estimate the index

epsilonfloat

Fractional energy increment to use for determining the spectral index.

Returns

indexfloat

Estimated spectral index.

to_dict(full_output=False)

Create dict for YAML serialisation

unfreeze()

Restore parameters frozen status to default