Neutrino implementation

SWIFT can also accurately model the effects of massive neutrinos in cosmological simulations. At the background level, massive neutrinos and other relativistic species can be included by specifying their number and masses in the cosmology section of the parameter file (see Cosmology).

At the perturbation level, neutrinos can be included as a separate particle species (PartType6). To facilitate this, SWIFT implements the \(\delta f\) method for shot noise suppression (Elbers et al. 2020). The method works by statistically weighting the particles during the simulation, with weights computed from the Liouville equation using current and initial momenta. The method can be activated by specifying Neutrino:use_delta_f in the parameter file.

The implementation of the \(\delta f\) method in SWIFT assumes a specific method for generating the initial neutrino momenta (see below). This makes it possible to reproduce the initial momentum when it is needed without increasing the memory footprint of the neutrino particles. If perturbed initial conditions are not needed, the initial momenta can be generated internally by specifying Neutrino:generate_ics in the parameter file. This will assign PartType6 particles to each neutrino mass specified in the cosmology and generate new velocities based on the homogeneous (unperturbed) Fermi-Dirac distribution. In this case, placeholder neutrino particles should be provided in the initial conditions with arbitrary masses and velocities, distributed uniformly in the box. Placeholders can be spawned with the python script tools/

Relativistic Drift

At high redshift, neutrino particles move faster than the speed of light if the usual Newtonian expressions are used. To rectify this, SWIFT implements a relativistic drift correction. In this convention, the internal velocity variable (see theory/Cosmology) is \(v^i=a^2u^i=a^2\dot{x}^i\gamma^{-1}\), where \(u^i\) is the spatial part of the 4-velocity, \(a\) the scale factor, and \(x^i\) a comoving position vector. The conversion factor to the coordinate 3-velocity is \(\gamma=ac/\sqrt{a^2c^2+v^2}\). This factor is applied to the neutrino particles throughout the simulation.

Generating Fermi-Dirac momenta

The implementation of the \(\delta f\) method in SWIFT assumes that neutrinos were initially assigned a Fermi-Dirac momentum using the following method. Each particle has a fixed 64-bit unsigned integer \(\ell\) given by the particle ID [1] (plus an optional seed: Neutrino:neutrino_seed). This number is transformed into a floating point number \(u\in(0,1)\), using the following pseudo-code based on splitmix64:

m = l + 0x9E3779B97f4A7C15
m = (m ^ (m >> 30)) * 0xBF58476D1CE4E5B9;
m = (m ^ (m >> 27)) * 0x94D049BB133111EB;
m = m ^ (m >> 31);
u = (m + 0.5) / (UINT64_MAX + 1)

This is subsequently transformed into a Fermi-Dirac momentum \(q = F^{-1}(u)\) by evaluating the quantile function. To generate neutrino particle initial conditions with perturbations, one first generates momenta from the unperturbed Fermi-Dirac distribution using the above method and then applies perturbations in any suitable manner.

When using the \(\delta f\) method, SWIFT also assumes that PartType6 particles are assigned to all \(N_\nu\) massive species present in the cosmology, such that the particle with fixed integer \(\ell\) corresponds to species \(i = \ell\; \% \;N_\nu\in[0,N_\nu-1]\).

The sampled Fermi-Dirac speeds and neutrino masses are written into the snapshot files as SampledSpeeds and MicroscopicMasses.

Mesh Neutrinos

There are two additional implementations of neutrino physics. The first is an option to only apply the delta-f weighting scheme on the mesh. In this case, particle neutrinos participate like dark matter in the remaining gravity calculations. This mode can be activated with Neutrino:use_delta_f_mesh_only.

The second option is an implementation of the linear response method, once again on the mesh only, which requires a separate data file with transfer functions. Example settings in the paramter file for this mode are:

  use_linear_response: 1                         # Option to use the linear response method
  transfer_functions_filename: perturb.hdf5      # For linear response neutrinos, path to an hdf5 file with transfer functions, redshifts, and wavenumbers
  dataset_redshifts: Redshifts                   # For linear response neutrinos, name of the dataset with the redshifts (a vector of length N_z)
  dataset_wavenumbers: Wavenumbers               # For linear response neutrinos, name of the dataset with the wavenumbers (a vector of length N_k)
  dataset_delta_cdm: Functions/d_cdm             # For linear response neutrinos, name of the dataset with the cdm density transfer function (N_z x N_k)
  dataset_delta_baryon: Functions/d_b            # For linear response neutrinos, name of the dataset with the baryon density transfer function (N_z x N_k)
  dataset_delta_nu: Functions/d_ncdm[0]          # For linear response neutrinos, name of the dataset with the neutrino density transfer function (N_z x N_k)
  fixed_bg_density: 1                            # For linear response neutrinos, whether to use a fixed present-day background density

In this example, the code reads an HDF5 file “perturb.hdf5” with transfer functions. The file must contain a vector with redshifts of length \(N_z\), a vector with wavenumbers \(N_k\), and three arrays with dimensions \(N_z \times N_k\) of density transfer functions for cdm, baryons, and neutrinos respectively. It is recommended to store the units of the wavenumbers as an attribute at “Units/Unit length in cgs (U_L)”. The fixed_bg_density flag determines whether the linear response scales as \(\Omega_\nu(a)\) or the present-day value \(\Omega_{\nu,0}\), either of which may be appropriate depending on the particle initial conditions. An HDF5 file can be generated using classy with the script tools/

The linear response mode currently only supports degenerate mass models with a single neutrino transfer function.

Background Neutrinos Only

It is also possible to run without neutrino perturbations, even when specifying neutrinos in the background cosmology. This mode can be activated with Neutrino:use_model_none.

[1]Currently, it is not guaranteed that a particle ID is unique.