py21cmfast.inputs.GlobalParams¶
- class py21cmfast.inputs.GlobalParams(wrapped, ffi)[source]¶
Global parameters for 21cmFAST.
This is a thin wrapper over an allocated C struct, containing parameter values which are used throughout various computations within 21cmFAST. It is a singleton; that is, a single python (and C) object exists, and no others should be created. This object is not “passed around”, rather its values are accessed throughout the code.
Parameters in this struct are considered to be options that should usually not have to be modified, and if so, typically once in any given script or session.
Values can be set in the normal way, eg.:
>>> global_params.ALPHA_UVB = 5.5
The class also provides a context manager for setting parameters for a well-defined portion of the code. For example, if you would like to set
Z_HEAT_MAX
for a given run:>>> with global_params.use(Z_HEAT_MAX=25): >>> p21c.run_lightcone(...) # uses Z_HEAT_MAX=25 for the entire run. >>> print(global_params.Z_HEAT_MAX) 35.0
- Variables
ALPHA_UVB (float) – Power law index of the UVB during the EoR. This is only used if INHOMO_RECO is True (in
FlagOptions
), in order to compute the local mean free path inside the cosmic HII regions.EVOLVE_DENSITY_LINEARLY (bool) – Whether to evolve the density field with linear theory (instead of 1LPT or Zel’Dovich). If choosing this option, make sure that your cell size is in the linear regime at the redshift of interest. Otherwise, make sure you resolve small enough scales, roughly we find BOX_LEN/DIM should be < 1Mpc
SMOOTH_EVOLVED_DENSITY_FIELD (bool) – If True, the zeldovich-approximation density field is additionally smoothed (aside from the implicit boxcar smoothing performed when re-binning the ICs from DIM to HII_DIM) with a Gaussian filter of width
R_smooth_density*BOX_LEN/HII_DIM
. The implicit boxcar smoothing inperturb_field()
bins the density field on scale DIM/HII_DIM, similar to what Lagrangian codes do when constructing Eulerian grids. In other words, the density field is quantized into(DIM/HII_DIM)^3
values. If your usage requires smooth density fields, it is recommended to set this to True. This also decreases the shot noise present in all grid based codes, though it overcompensates by an effective loss in resolution. Added in 1.1.0.R_smooth_density (float) – Determines the smoothing length to use if SMOOTH_EVOLVED_DENSITY_FIELD is True.
HII_ROUND_ERR (float) – Rounding error on the ionization fraction. If the mean xHI is greater than
1 - HII_ROUND_ERR
, then finding HII bubbles is skipped, and a homogeneous xHI field of ones is returned. Added in v1.1.0.FIND_BUBBLE_ALGORITHM (int, {1,2}) – Choose which algorithm used to find HII bubbles. Options are: (1) Mesinger & Furlanetto 2007 method of overlapping spheres: paint an ionized sphere with radius R, centered on pixel where R is filter radius. This method, while somewhat more accurate, is slower than (2), especially in mostly ionized universes, so only use for lower resolution boxes (HII_DIM<~400). (2) Center pixel only method (Zahn et al. 2007). This is faster.
N_POISSON (int) –
If not using the halo field to generate HII regions, we provide the option of including Poisson scatter in the number of sources obtained through the conditional collapse fraction (which only gives the mean collapse fraction on a particular scale. If the predicted mean collapse fraction is less than N_POISSON * M_MIN, then Poisson scatter is added to mimic discrete halos on the subgrid scale (see Zahn+2010).Use a negative number to turn it off.
Note
If you are interested in snapshots of the same realization at several redshifts,it is recommended to turn off this feature, as halos can stochastically “pop in and out of” existence from one redshift to the next.
R_OVERLAP_FACTOR (float) – When using USE_HALO_FIELD, it is used as a factor the halo’s radius, R, so that the effective radius is R_eff = R_OVERLAP_FACTOR * R. Halos whose centers are less than R_eff away from another halo are not allowed. R_OVERLAP_FACTOR = 1 is fully disjoint R_OVERLAP_FACTOR = 0 means that centers are allowed to lay on the edges of neighboring halos.
DELTA_CRIT_MODE (int) – The delta_crit to be used for determining whether a halo exists in a cell 0: delta_crit is constant (i.e. 1.686) 1: delta_crit is the sheth tormen ellipsoidal collapse correction to delta_crit
HALO_FILTER (int) – Filter for the density field used to generate the halo field with EPS 0: real space top hat filter 1: sharp k-space filter 2: gaussian filter
OPTIMIZE (bool) – Finding halos can be made more efficient if the filter size is sufficiently large that we can switch to the collapse fraction at a later stage.
OPTIMIZE_MIN_MASS (float) – Minimum mass on which the optimization for the halo finder will be used.
T_USE_VELOCITIES (bool) –
Whether to use velocity corrections in 21-cm fields
Note
The approximation used to include peculiar velocity effects works only in the linear regime, so be careful using this (see Mesinger+2010)
MAX_DVDR (float) –
Maximum velocity gradient along the line of sight in units of the hubble parameter at z. This is only used in computing the 21cm fields.
Note
Setting this too high can add spurious 21cm power in the early stages, due to the 1-e^-tau ~ tau approximation (see Mesinger’s 21cm intro paper and mao+2011). However, this is still a good approximation at the <~10% level.
VELOCITY_COMPONENT (int) – Component of the velocity to be used in 21-cm temperature maps (1=x, 2=y, 3=z)
DELTA_R_FACTOR (float) – Factor by which to scroll through filter radius for halos
DELTA_R_HII_FACTOR (float) – Factor by which to scroll through filter radius for bubbles
HII_FILTER (int, {0, 1, 2}) – Filter for the Halo or density field used to generate ionization field: 0. real space top hat filter 1. k-space top hat filter 2. gaussian filter
INITIAL_REDSHIFT (float) – Used to perturb field
CRIT_DENS_TRANSITION (float) – A transition value for the interpolation tables for calculating the number of ionising photons produced given the input parameters. Log sampling is desired, however the numerical accuracy near the critical density for collapse (i.e. 1.69) broke down. Therefore, below the value for CRIT_DENS_TRANSITION log sampling of the density values is used, whereas above this value linear sampling is used.
MIN_DENSITY_LOW_LIMIT (float) – Required for using the interpolation tables for the number of ionising photons. This is a lower limit for the density values that is slightly larger than -1. Defined as a density contrast.
RecombPhotonCons (int) – Whether or not to use the recombination term when calculating the filling factor for performing the photon non-conservation correction.
PhotonConsStart (float) – A starting value for the neutral fraction where the photon non-conservation correction is performed exactly. Any value larger than this the photon non-conservation correction is not performed (i.e. the algorithm is perfectly photon conserving).
PhotonConsEnd (float) – An end-point for where the photon non-conservation correction is performed exactly. This is required to remove undesired numerical artifacts in the resultant neutral fraction histories.
PhotonConsAsymptoteTo (float) – Beyond PhotonConsEnd the photon non-conservation correction is extrapolated to yield smooth reionisation histories. This sets the lowest neutral fraction value that the photon non-conservation correction will be applied to.
HEAT_FILTER (int) – Filter used for smoothing the linear density field to obtain the collapsed fraction: 0: real space top hat filter 1: sharp k-space filter 2: gaussian filter
CLUMPING_FACTOR (float) – Sub grid scale. If you want to run-down from a very high redshift (>50), you should set this to one.
Z_HEAT_MAX (float) – Maximum redshift used in the Tk and x_e evolution equations. Temperature and x_e are assumed to be homogeneous at higher redshifts. Lower values will increase performance.
R_XLy_MAX (float) – Maximum radius of influence for computing X-ray and Lya pumping in cMpc. This should be larger than the mean free path of the relevant photons.
NUM_FILTER_STEPS_FOR_Ts (int) – Number of spherical annuli used to compute df_coll/dz’ in the simulation box. The spherical annuli are evenly spaced in logR, ranging from the cell size to the box size.
spin_temp()
will create this many boxes of size HII_DIM, so be wary of memory usage if values are high.ZPRIME_STEP_FACTOR (float) – Logarithmic redshift step-size used in the z’ integral. Logarithmic dz. Decreasing (closer to unity) increases total simulation time for lightcones, and for Ts calculations.
TK_at_Z_HEAT_MAX (float) – If positive, then overwrite default boundary conditions for the evolution equations with this value. The default is to use the value obtained from RECFAST. See also XION_at_Z_HEAT_MAX.
XION_at_Z_HEAT_MAX (float) – If positive, then overwrite default boundary conditions for the evolution equations with this value. The default is to use the value obtained from RECFAST. See also TK_at_Z_HEAT_MAX.
Pop (int) – Stellar Population responsible for early heating (2 or 3)
Pop2_ion (float) – Number of ionizing photons per baryon for population 2 stellar species.
Pop3_ion (float) – Number of ionizing photons per baryon for population 3 stellar species.
NU_X_BAND_MAX (float) – This is the upper limit of the soft X-ray band (0.5 - 2 keV) used for normalising the X-ray SED to observational limits set by the X-ray luminosity. Used for performing the heating rate integrals.
NU_X_MAX (float) – An upper limit (must be set beyond NU_X_BAND_MAX) for performing the rate integrals. Given the X-ray SED is modelled as a power-law, this removes the potential of divergent behaviour for the heating rates. Chosen purely for numerical convenience though it is motivated by the fact that observed X-ray SEDs apprear to turn-over around 10-100 keV (Lehmer et al. 2013, 2015)
NBINS_LF (int) – Number of bins for the luminosity function calculation.
P_CUTOFF (bool) – Turn on Warm-Dark-matter power suppression.
M_WDM (float) – Mass of WDM particle in keV. Ignored if P_CUTOFF is False.
g_x (float) – Degrees of freedom of WDM particles; 1.5 for fermions.
OMn (float) – Relative density of neutrinos in the universe.
OMk (float) – Relative density of curvature.
OMr (float) – Relative density of radiation.
OMtot (float) – Fractional density of the universe with respect to critical density. Set to unity for a flat universe.
Y_He (float) – Helium fraction.
wl (float) – Dark energy equation of state parameter (wl = -1 for vacuum )
SHETH_b (float) –
Sheth-Tormen parameter for ellipsoidal collapse (for HMF).
Note
The best fit b and c ST params for these 3D realisations have a redshift, and a
DELTA_R_FACTOR
dependence, as shown in Mesinger+. For converged mass functions at z~5-10, set DELTA_R_FACTOR=1.1 and SHETH_b=0.15 and SHETH_c~0.05.For most purposes, a larger step size is quite sufficient and provides an excellent match to N-body and smoother mass functions, though the b and c parameters should be changed to make up for some “stepping-over” massive collapsed halos (see Mesinger, Perna, Haiman (2005) and Mesinger et al., in preparation).
- For example, at z~7-10, one can set DELTA_R_FACTOR=1.3 and SHETH_b=0.15
and SHETH_c=0.25, to increase the speed of the halo finder.
SHETH_c (float) – Sheth-Tormen parameter for ellipsoidal collapse (for HMF). See notes for SHETH_b.
Zreion_HeII (float) – Redshift of helium reionization, currently only used for tau_e
FILTER (int, {0, 1}) – Filter to use for smoothing. 0. tophat 1. gaussian
external_table_path (str) – The system path to find external tables for calculation speedups. DO NOT MODIFY.
R_BUBBLE_MIN (float) – Minimum radius of bubbles to be searched in cMpc. One can set this to 0, but should be careful with shot noise if running on a fine, non-linear density grid. Default is set to L_FACTOR which is (4PI/3)^(-1/3) = 0.620350491.
M_MIN_INTEGRAL – Minimum mass when performing integral on halo mass function.
M_MAX_INTEGRAL – Maximum mass when performing integral on halo mass function.
T_RE – The peak gas temperatures behind the supersonic ionization fronts during reionization.
VAVG – Avg value of the DM-b relative velocity [im km/s], ~0.9*SIGMAVCB (=25.86 km/s) normally.
Methods
__init__
(wrapped, ffi)filtered_repr
(filter_params)Get a fully unique representation of the instance that filters out some parameters.
items
()Yield (name, value) pairs for each element of the struct.
keys
()Return a list of names of elements in the struct.
use
(**kwargs)Set given parameters for a certain context.
Attributes
An ffi char pointer to the path to which external tables are kept.
An ffi char pointer to the path to which external tables are kept.