Radiative Transfer Spectra

Class providing spectral energy distributions of sources for Monte Carlo radiative transfer calculations—the luminosity (in \(L_\odot\) AA\(^{-1}\)) as a function of wavelength and the integrated luminosity over a wavelength range, used to initialize photon packet energies and to draw photon wavelengths from the source spectrum. Implementations include blackbody spectra, stellar population SEDs, and AGN power-law spectra, and determine the energy budget of photon packets launched into the computational domain.

Default implementation: radiativeTransferSpectrumBlackBody

Methods

luminosity → double precision

Return the luminosity in the given wavelength range.

  • double precision, intent(in ) :: wavelengthMinimum, wavelengthMaximum

spectrum → double precision

Return the spectrum (in units of \(L_\odot\) AA\(^{-1}\)) of the source at the given wavelength.

  • double precision, intent(in ) :: wavelength

radiativeTransferSpectrumAccretionDisk

A photon spectrum class that computes the spectral luminosity of radiation emitted by an accreting black hole accretion disk in radiative transfer calculations. The black hole mass and Eddington-scaled accretion rate are set by the [blackHoleMass] and [accretionRateEddington] parameters.

Parameters

  • [massBlackHole] (default 1.0d6) — The mass of the black hole at the center of the accretion disk.

  • [accretionRateEddington] (default 1.0d-1) — Accretion rate onto the black hole in units of the Eddington rate.

radiativeTransferSpectrumBandPassFilter

A photon spectrum class that applies a wavelength band-pass filter to another photon spectrum, returning zero luminosity outside the specified wavelength range. The passband is controlled by the [wavelengthMinimum] and [wavelengthMaximum] parameters (in units of AA).

Parameters

  • [wavelengthMinimum] (default 0.0d0) — The minimum wavelength (in units of AA) to pass the spectrum.

  • [wavelengthMaximum] (default huge(0.0d0)) — The maximum wavelength (in units of AA) to pass the spectrum.

radiativeTransferSpectrumBlackBody

A photon spectrum class that computes the spectral luminosity of a thermal blackbody source for use in radiative transfer calculations, scaling the Planck function to a specified bolometric luminosity. The blackbody temperature and total bolometric luminosity are set by the [temperature] (in Kelvin) and [luminosityBolometric] (in \(L_\odot\)) parameters.

(Default implementation)

Methods

  • temperature — Return the temperature of the black-body radiation field.

Parameters

  • [temperature] (default 5.0d3) — The temperature of the black body spectrum (in Kelvin).

  • [luminosityBolometric] (default 1.0d0) — The bolometric luminosity of the black body spectrum (in \(L_\odot\)).

  • [temperature] — The temperature (in Kelvin) of the blackbody radiation field, which sets the peak wavelength and total emitted flux via the Planck function.

radiativeTransferSpectrumPowerLaw

A photon spectrum class for power law spectra of the form

\[\begin{split}L_\lambda (\lambda) = \begin{array}{cc} A (\lambda/\lambda_\mathrm{min})^\alpha & \hbox{if } \lambda_\mathrm{min} \le \lambda < \lambda_\mathrm{max} \\ 0 & \hbox{otherwise,} \end{array}\end{split}\]

where \(A=\)normalization, \(\alpha=\)exponent, \(\lambda_\mathrm{min}=\)wavelengthMinimum, and \(\lambda_\mathrm{max}=\)wavelengthMaximum.

Parameters

  • [exponent] (default 1.73d0) — Exponent of the differential luminosity function.

  • [rateHydrogenIonizingPhotonsMinimum] (default 1.0d48) — The minimum ionizing photon production rate (\(Q_\mathrm{H,min}\), in photons/s) below which the power-law HII region luminosity function is truncated to zero.

  • [rateHydrogenIonizingPhotonsMaximum] (default huge(0.0d0)) — The maximum ionizing photon production rate (\(Q_\mathrm{H,max}\), in photons/s) above which the power-law HII region luminosity function is truncated to zero.

  • [exponent] (default 1.0d0) — Halo masses will be (pseudo-)uniformly distributed in \([\log(M)]^{1/(1+\alpha)}\) where \(\alpha=\)exponent.

  • [wavelengthMinimum] — The minimum wavelength (in units of AA) for the power-law spectrum.

  • [wavelengthMaximum] — The maximum wavelength (in units of AA) for the power-law spectrum.

  • [exponent] — The exponent of the power-law spectrum.

  • [normalization] — The normalization (in units of \(L_\odot / \AA\)) of the power-law spectrum.

  • [normalization] — Parameter \(\sigma_{12}\) appearing in model for random errors in the halo mass function.

  • [fractionalErrorHighMass] — Parameter \(\sigma_\infty\) appearing in model for random errors in the halo mass function.

  • [exponent] — Parameter \(\gamma\) appearing in model for random errors in the halo mass function. Specifically, the fractional error is given by \(\sigma(M) = \left[ \sigma^2_{12} \left({M_\mathrm{halo} \over 10^{12}\mathrm{M}_\odot}\right)^{2\gamma} + \sigma^2_\infty \right]^{1/2}\), where \(\sigma_{12}=\)[normalization] and \(\gamma=\)[exponent].

  • [correlationModelTrivial] (default .true.) — If true, the correlation between mass errors of pairs of halos is unity for halos with identical mass and time, and zero otherwise. If false, a power-law correlation model in mass ratio and expansion factor ratio is used instead.

  • [correlationNormalization] (default 0.0d0) — Variable \(C_0\) in the model for the correlation between halo mass errors: \(C_{12} = C_0 [M_2/M_1]^\alpha [(1+z_2)/(1+z_1)]^\beta\).

  • [correlationMassExponent] (default 0.0d0) — Variable \(\alpha\) in the model for the correlation between halo mass errors: \(C_{12} = C_0 [M_2/M_1]^\alpha [(1+z_2)/(1+z_1)]^\beta\).

  • [correlationRedshiftExponent] (default 0.0d0) — Variable \(\beta\) in the model for the correlation between halo mass errors: \(C_{12} = C_0 [M_2/M_1]^\alpha [(1+z_2)/(1+z_1)]^\beta\).

  • [radiusLow] (default +0.0154d0) — The low-mass limit of the characteristic scale radius \(r_0\) (in Mpc) in the power-law scale radius model, giving the scale radius normalization for low-mass halos as a function of peak height and expansion factor.

  • [radiusHigh] (default +0.0962d0) — The high-mass limit of the characteristic scale radius \(r_1\) (in Mpc) in the power-law scale radius model, giving the scale radius normalization for high-mass halos.

  • [radiusTransition] (default +1.2137d0) — The peak height \(\nu\) at which the characteristic scale radius transitions between its low-mass and high-mass limiting values in the power-law scale radius model.

  • [radiusWidth] (default +0.5482d0) — The parameter \(\Delta r\) in the power-law scale radius model.

  • [massLow] (default +0.3895d0) — The parameter \(\alpha_0\) in the power-law scale radius model.

  • [massHigh] (default +0.2984d0) — The parameter \(\alpha_1\) in the power-law scale radius model.

  • [massTransition] (default -0.2583d0) — The parameter \(\alpha_\nu\) in the power-law scale radius model.

  • [massWidth] (default +16.6050d0) — The parameter \(\Delta \alpha\) in the power-law scale radius model.

  • [expansionFactorLow] (default -0.6977d0) — The parameter \(\beta_0\) in the power-law scale radius model.

  • [expansionFactorHigh] (default +0.7972d0) — The parameter \(\beta_1\) in the power-law scale radius model.

  • [expansionFactorTransition] (default +0.5395d0) — The parameter \(\beta_\nu\) in the power-law scale radius model.

  • [expansionFactorWidth] (default +0.4282d0) — The parameter \(\Delta \beta\) in the power-law scale radius model.

  • [scatter] (default +0.1513d0) — The scatter (in dex) in the scale radius at fixed halo mass and redshift in the power-law scale radius model, representing the intrinsic halo-to-halo variation in concentration.

  • [index] (default 0.9649d0) — The index of the power-law primordial power spectrum.

  • [running] (default 0.0d0) — The running, \(\d n_\mathrm{s} / \d \ln k\), of the power spectrum index.

  • [runningRunning] (default 0.0d0) — The running-of-the-running, \(\d^2 n_\mathrm{s} / \d \ln k^2\), of the power spectrum index.

  • [wavenumberReference] (default 1.0d0) — When a running power spectrum index is used, this is the wavenumber, \(k_\mathrm{ref}\), at which the index is equal to [index].

  • [runningSmallScalesOnly] (default .false.) — If true then the index runs only for \(k > k_\mathrm{ref}\), for smaller \(k\) the index is constant.