All foreground models inherit from this type.

CIB_Planck2013{T}(; kwargs...)

Define CIB model parameters. Defaults are from Viero et al. 2013. All numbers not typed are converted to type T. This model has the following parameters and default values:

• nside::Int64 = 4096
• min_redshift = 0.0
• max_redshift = 5.0
• min_mass = 1e12
• box_size = 40000
• shang_zplat = 2.0
• shang_Td = 20.7
• shang_betan = 1.6
• shang_eta = 2.4
• shang_alpha = 0.2
• shang_Mpeak = 10^12.3
• shang_sigmaM = 0.3
• shang_Msmin = 1e11
• shang_Mmin = 1e10
• shang_I0 = 92
• jiang_gamma_1 = 0.13
• jiang_alpha_1 = -0.83
• jiang_gamma_2 = 1.33
• jiang_alpha_2 = -0.02
• jiang_beta_2 = 5.67
• jiang_zeta = 1.19

CO_CROWNED{T}(; kwargs...)

Define broadband CO model parameters. All numbers not typed are converted to type T. This model has the following parameters and default values:

• nside::Int64 = 4096
• hod::String = "shang"

LRG_Yuan23{T}(; kwargs...)

Define LRG model parameters. Defaults from Yuan et al. 2023 [arXiv:2306.06314]. All numbers not typed are converted to type T. This model has the following parameters and default values:

• nside::Int64 = 4096
• hod::String = "zheng"
• min_redshift = 0.0
• max_redshift = 5.0
• min_mass = 1e12
• box_size = 40000
• shang_Msmin = 1e11
• zheng_Mcut = 10^12.7
• zheng_M1 = 10^13.6
• zheng_sigma = 0.2
• zheng_kappa = 0.08
• zheng_alpha = 1.15
• yuan_ic = 0.8
• jiang_gamma_1 = 0.13
• jiang_alpha_1 = -0.83
• jiang_gamma_2 = 1.33
• jiang_alpha_2 = -0.02
• jiang_beta_2 = 5.67
• jiang_zeta = 1.19

Radio_Sehgal2009{T}(model parameters...)

Define CIB model parameters. Defaults are from Viero et al. 2013.

model = CIBModel{Float32}(a_0=0.4)

Line-of-sight integrated electron pressure

Line-of-sight integrated electron pressure

Line-of-sight integrated thermal pressure

Line-of-sight integrated thermal pressure

Compute the real-space beam from a harmonic-space beam.

build_c_lnm2r_interpolator(;cmin::T=1f-3, cmax::T=25.0f0,
    mmin::T=-7.1f0, mmax::T=0.0f0, nbin=100) where T

Generate a LinearInterpolation object that turns concentration and ln(M_halo) into satellite radius.

Helper function to build a tSZ interpolator

Helper function to build a tSZ interpolator

Build a linear interpolation function which maps log(Mh) to Nsh.

build_r2z_interpolator(min_z::T, max_z::T,
    cosmo::Cosmology.AbstractCosmology; n_bins=2000) where T

Construct a fast r2z linear interpolator.

Build a linear interpolation function which maps log(Mh) to Nsat.

Construct a z2r linear interpolator.

Build a linear interpolation function which maps log(Mh) to Ncen.

Build a linear interpolation function which maps log(Mh) to Nsat.

Generates a list of tuples which describe starting and ending chunk indices. Useful for parallelizing an array operation.

prune a profile grid for negative values, extrapolate instead

Utility function which prepends some zeros to an array. It makes a copy instead of modifying the input.

Quiescent fraction recipe from UniverseMachine

generate_sources(model, cosmo, halo_pos_inp, halo_mass_inp; verbose=true)

Produce a source catalog from a model and halo catalog. This converts the halo arrays into the type specified by model.

Arguments:

• model::AbstractCIBModel{T}: source model parameters
• cosmo::Cosmology.FlatLCDM{T}: background cosmology
• Healpix_res::Resolution: Healpix map resolution
• halo_pos_inp::AbstractArray{TH,2}: halo positions with dims (3, nhalos)
• halo_mass_inp::AbstractArray{TH,1}: halo masses

Keywords

• verbose::Bool=true: print out progress details

generate_sources(model, cosmo, halo_pos_inp, halo_mass_inp; verbose=true)

Produce a source catalog from a model and halo catalog. This converts the halo arrays into the type specified by model.

Arguments:

• model::AbstractCIBModel{T}: source model parameters
• cosmo::Cosmology.FlatLCDM{T}: background cosmology
• Healpix_res::Resolution: Healpix map resolution
• halo_pos_inp::AbstractArray{TH,2}: halo positions with dims (3, nhalos)
• halo_mass_inp::AbstractArray{TH,1}: halo masses

Keywords

• verbose::Bool=true: print out progress details

Produce a source catalog from a model and halo catalog.

Generate an array where the value at index i corresponds to the index of the first source of halo i. Takes an array where the value at index i corresponds to the number of subhalos that halo i has.

Compute angles of halos

Fill in basic halo properties.

get_cosmology(::Type{T}; h=0.69, Neff=3.04, OmegaK=0.0,
    OmegaM=0.29, OmegaR=nothing, Tcmb=2.7255, w0=-1, wa=0)

Construct a background cosmology. This function duplicates the cosmology() function in Cosmology.jl, but with the numeric type specified.

Arguments:

• ::Type{T}: numerical type to use for calculations

Keywords

• h - Dimensionless Hubble constant
• OmegaK - Curvature density (Ω_k)
• OmegaM - Matter density (Ω_m)
• OmegaR - Radiation density (Ω_r)
• Tcmb - CMB temperature in Kelvin; used to compute Ω_γ
• Neff - Effective number of massless neutrino species; used to compute Ω_ν
• w0 - CPL dark energy equation of state; w = w0 + wa(1-a)
• wa - CPL dark energy equation of state; w = w0 + wa(1-a)

Example

julia> get_cosmology(Float32; h=0.7)
Cosmology.FlatLCDM{Float32}(0.7f0, 0.7099147f0, 0.29f0, 8.5307016f-5)

Construct the necessary interpolator set.

Construct the necessary interpolator set.

Populate halos with radio sources according to the HOD in Sehgal et al. 2009.

The optional rng parameter provides an array of random number generators, one for each thread.

Inverse square law with redshift dependence.

Reads a collection of example halos out of the WebSky halo catalogs, and returns RA (rad), DEC (rad), redshift, and halo mass (M200c).

Reads in a standard Battaglia 2016 model from disk for tSZ.

m2r(m::T, cosmo::Cosmology.FlatLCDM{T}) where T

Convert virial mass to virial radius.

mz2c(m::T, z::T, cosmo::Cosmology.FlatLCDM{T}) where T

Compute concentration factor from Duffy et al. 2008.

Paint a source catalog onto a map.

This function creates the arrays for you.

paint!(result_map, nu_obs, model, sources, fluxes_cen, fluxes_sat)

Paint a source catalog onto a map, recording the fluxes in fluxes_cen and fluxes_sat.

Arguments:

• result_map::HealpixMap{T_map, RingOrder}: Healpix map to paint
• nu_obs: frequency in Hz
• model::AbstractCIBModel{T}: source model parameters
• sources: NamedTuple containing source information from generate_sources
• fluxes_cen::AbstractArray: buffer for writing fluxes of centrals
• fluxes_sat::AbstractArray: buffer for writing fluxes of satellites

paint!(result_map, model, sources, min_redshift, max_redshift)

'Paint' the LRG catalog onto a map.

Arguments:

• result_map::HealpixMap{T_map, RingOrder}: Healpix map to paint
• model::AbstractCIBModel{T}: source model parameters
• sources: NamedTuple containing source information from generate_sources
• fluxes_cen::AbstractArray: buffer for writing fluxes of centrals
• fluxes_sat::AbstractArray: buffer for writing fluxes of satellites

queryDiscRing!(result, ringinfo, resol::Resolution, theta, phi, radius; fact=0)

In-place calculation of a list of the indices of those pixels whose centers are closer than radius to direction (theta, phi). The three angles radius, theta, and phi must be expressed in radians.

If fact is nonzero, it must be a positive integer; it requires to carry the computation at a resolution fact * nside.

Convert RA (rad), DEC (rad), and redshift to xyz comoving radial dist.

Utility function to read an HDF5 table with x, y, z, M_h as the four rows. The hdf5 record is "halos".

Computes a real-space beam interpolator and a maximum

Returns a stored artifact: a precomputed SZpack table

Fills the result array with draws from the luminosity function.

Apply a beam to a profile grid

vecmap([T=Float64], nside::Int)

Generate a map of 3-tuples, showing the (x,y,z) values of the points on the unit 2-sphere for a Healpix map.

Compute redshift evolution factor for LF.