Spherical Collapse Solvers

Class providing numerical solvers for the collapse of spherical density perturbations in a given cosmology—computing the critical linear overdensity \(\delta_\mathrm{c}\), the virial density contrast \(\Delta_\mathrm{vir}\), and the turnaround-to-virial radius ratio as functions of cosmic time by integrating the spherical collapse equations. These tabulated quantities are consumed by criticalOverdensityClass and virialDensityContrastClass implementations, allowing the halo collapse threshold and virial radius definition to vary with redshift and cosmological model.

Default implementation: sphericalCollapseSolverCllsnlssMttrCsmlgclCnstnt

Methods

criticalOverdensity → void

Returns a tabulation of the critical overdensity for collapse.

  • double precision , intent(in ) :: time

  • logical , intent(in ) :: tableStore

  • class (table1D), allocatable, intent(inout) :: criticalOverdensity_

virialDensityContrast → void

Returns a tabulation of the virial density contrast.

  • double precision , intent(in ) :: time

  • logical , intent(in ) :: tableStore

  • class (table1D), allocatable, intent(inout) :: virialDensityContrast_

radiusTurnaround → void

Returns a tabulation of the ratio of turnaround to virial radii.

  • double precision , intent(in ) :: time

  • logical , intent(in ) :: tableStore

  • class (table1D), allocatable, intent(inout) :: radiusTurnaround_

linearNonlinearMap → void

Returns a mapping of linear to nonlinear density overdensity.

  • double precision , intent(in ) :: time

  • class (table2DLinLinLin), allocatable, intent(inout) :: linearNonlinearMap_

sphericalCollapseSolverBaryonsDarkMatterDarkEnergy

A spherical collapse solver for universes consisting of baryons, collisionless dark matter, and dark energy, computing the evolution of a spherical top-hat overdensity through turnaround and virialization. Baryons can be treated as either clustering or non-clustering via [baryonsClustering], and the energy-fixing radius for dark energy is set by [radiusFixed].

Parameters

  • [baryonsCluster] — If true baryons are assumed to cluster in the same way as collisionless matter. If false, baryons are assumed not to cluster at all.

  • [energyFixedAt] (default var_str('turnaround')) — The radius at which the energy of a spherical top-hat perturbation in a dark energy cosmology can be considered to be fixed.

  • [tablePointsPerOctave] (default 300) — The number of points per octave of time at which to tabulate solutions.

sphericalCollapseSolverCllsnlssMttrCsmlgclCnstnt

A spherical collapse solver for universes consisting of collisionless matter and a cosmological constant.

(Default implementation)

Methods

  • getTable — Get the requested table.

  • restoreTable — Restore a tabulated solution from file.

  • storeTable — Store a tabulated solution to file.

  • tabulate — Construct a tabulated solution.

sphericalCollapseSolverCllsnlssMttrDarkEnergy

A spherical collapse solver for universes consisting of collisionless matter and dark energy.

Parameters

  • [energyFixedAt] (default var_str('turnaround')) — The radius at which the energy of a spherical top-hat perturbation in a dark energy cosmology can be considered to be fixed.