Halo Model Power Spectrum Modifier

Class providing modifiers to the one-halo and two-halo power spectrum terms in halo model galaxy clustering calculations. The modify method accepts the raw halo-model power spectrum at each wavenumber and modifies it in place for a specified term (one-halo or two-halo), allowing corrections such as baryonic feedback suppression, assembly bias, or scale-dependent effects to be applied without altering the underlying halo occupation distribution. Implementations may be mass-dependent (for per-halo corrections) or act globally on the full power spectrum array.

Default implementation: haloModelPowerSpectrumModifierIdentity

Methods

modify → void

Modify the power spectra in the halo model of clustering.

  • double precision , intent(in ), dimension(: ) :: wavenumber

  • type (enumerationHaloModelTermType), intent(in ) :: term

  • double precision , intent(inout), dimension(: ) :: powerSpectrum

  • double precision , intent(inout), dimension(:,:), optional :: powerSpectrumCovariance

  • double precision , intent(in ) , optional :: mass

haloModelPowerSpectrumModifierIdentity

A halo model power spectrum modifier class which applies an identity modifier.

(Default implementation)

Parameters

  • [redshift] (default 0.0d0) — The redshift at which the transfer function is defined.

haloModelPowerSpectrumModifierTriaxiality

A halo model power spectrum modifier class which attempts to modify power spectra to approximately account for the effects of halo triaxiality using the results of Smith and Watts (2005). Specifically, the one- and two-halo power spectra are multiplied by a correction factor, \(\Delta^2_\mathrm{triax}/\Delta^2_\mathrm{sphere}\), derived from the lower panels of Figures 3 and 2 of Smith and Watts (2005) respectively for their “JS02” profile model. Given the uncertainty in this correction, the power spectrum covariance (if provided) is incremented by \(\epsilon^2 ( [\Delta^2_\mathrm{triax}/\Delta^2_\mathrm{sphere}-1] \otimes [\Delta^2_\mathrm{triax}/\Delta^2_\mathrm{sphere}-1)\) where \(\epsilon=0.4\) is chosen to approximate the difference between “continuity” and “JS02” profiles in Smith and Watts (2005).