Hi, Antony,
This problem occurs when I tried to output transfer functions and matter power spectra for more than one transfer redshifts. The results for the first several matter power files (corresponding to larger redshifts) read normal. However after the redshift falls below some values, the calculation of matterpower goes wrong, whereas the results for transfer functions look normal. Given that all cosmological parameters are reasonable, (I even run CAMB with a more "harsh" set of parameters and obtain the correct results), do you have any ideas on what's the cause and how to fix it?
Thanks!
CAMB: results for matterpower is NaN
Re: CAMB: results for matterpower is NaN
the .ini file is as follows,Xin Wang wrote:Hi, Antony,
This problem occurs when I tried to output transfer functions and matter power spectra for more than one transfer redshifts. The results for the first several matter power files (corresponding to larger redshifts) read normal. However after the redshift falls below some values, the calculation of matterpower goes wrong, whereas the results for transfer functions look normal. Given that all cosmological parameters are reasonable, (I even run CAMB with a more "harsh" set of parameters and obtain the correct results), do you have any ideas on what's the cause and how to fix it?
Thanks!
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#Parameters for CAMB
#output_root is prefixed to output file names
output_root = 1fin.mvn_theory/mnu2eV_part2_0728/mnu2eV_part2
#What to do
get_scalar_cls = T
get_vector_cls = F
get_tensor_cls = F
get_transfer = T
#if do_lensing then scalar_output_file contains additional columns of l^4 C_l^{pp} and l^3 C_l^{pT}
#where p is the projected potential. Output lensed CMB Cls (without tensors) are in lensed_output_file below.
do_lensing = T
# 0: linear, 1: non-linear matter power (HALOFIT), 2: non-linear CMB lensing (HALOFIT)
do_nonlinear = 1
#Maximum multipole and k*eta.
# Note that C_ls near l_max are inaccurate (about 5%), go to 50 more than you need
# Lensed power spectra are computed to l_max_scalar-100
# To get accurate lensed BB need to have l_max_scalar>2000, k_eta_max_scalar > 10000
# Otherwise k_eta_max_scalar=2*l_max_scalar usually suffices, or don't set to use default
l_max_scalar = 5000
k_eta_max_scalar = 10000
# Tensor settings should be less than or equal to the above
l_max_tensor = 1500
k_eta_max_tensor = 3000
#Main cosmological parameters, neutrino masses are assumed degenerate
# If use_phyical set phyiscal densities in baryone, CDM and neutrinos + Omega_k
use_physical = T
ombh2 = 0.2202036E-01
omch2 = 0.111601208E+00
omnuh2 = 0.21321962E-01
omk = 0
hubble = 0.7125778E+02
#effective equation of state parameter for dark energy, assumed constant
w = -0.1057545E+01
#constant comoving sound speed of the dark energy (1=quintessence)
cs2_lam = 1
#if use_physical = F set parameters as here
#omega_baryon = 0.0462
#omega_cdm = 0.2538
#omega_lambda = 0.7
#omega_neutrino = 0
temp_cmb = 2.726
helium_fraction = 0.24
# massless_neutrinos is the effective number (for QED + non-instantaneous decoupling)
# fractional part of the number is used to increase the neutrino temperature, e.g.
# 2.99 correponds to 2 neutrinos with a much higher temperature, 3.04 correponds to
# 3 neutrinos with a slightly higher temperature. 3.046 is consistent with CosmoMC.
massless_neutrinos = 0.839103E+00
massive_neutrinos = 3
#Neutrino mass splittings
nu_mass_eigenstates = 1
#nu_mass_degeneracies = 0 sets nu_mass_degeneracies = massive_neutrinos
#otherwise should be an array
#e.g. for 3 neutrinos with 2 non-degenerate eigenstates, nu_mass_degeneracies = 2 1
nu_mass_degeneracies = 0
#Fraction of total omega_nu h^2 accounted for by each eigenstate, eg. 0.5 0.5
nu_mass_fractions = 1
#Initial power spectrum, amplitude, spectral index and running. Pivot k in Mpc^{-1}.
initial_power_num = 1
pivot_scalar = 0.05
pivot_tensor = 0.05
scalar_amp(1) = 2.1953E-09
scalar_spectral_index(1) = 0.9705830E+00
scalar_nrun(1) = 0
tensor_spectral_index(1) = 0
#ratio is that of the initial tens/scal power spectrum amplitudes
initial_ratio(1) = 1
#note vector modes use the scalar settings above
#Reionization, ignored unless reionization = T, re_redshift measures where x_e=0.5
reionization = T
re_use_optical_depth = T
re_optical_depth = 0.8635178E-01
#If re_use_optical_depth = F then use following, otherwise ignored
#re_redshift = 10.4
#width of reionization transition. CMBFAST model was similar to re_delta_redshift~0.5.
re_delta_redshift = 1.2
#re_ionization_frac=-1 sets to become fully ionized using YHe to get helium contribution
#Otherwise x_e varies from 0 to re_ionization_frac
re_ionization_frac = -1
#RECFAST 1.5 recombination parameters;
RECFAST_fudge = 1.14
RECFAST_fudge_He = 0.86
RECFAST_Heswitch = 6
RECFAST_Hswitch = T
#Initial scalar perturbation mode (adiabatic=1, CDM iso=2, Baryon iso=3,
# neutrino density iso =4, neutrino velocity iso = 5)
initial_condition = 1
#If above is zero, use modes in the following (totally correlated) proportions
#Note: we assume all modes have the same initial power spectrum
initial_vector = -1 0 0 0 0
#For vector modes: 0 for regular (neutrino vorticity mode), 1 for magnetic
vector_mode = 0
#Normalization
COBE_normalize = F
##CMB_outputscale scales the output Cls
#To get MuK^2 set realistic initial amplitude (e.g. scalar_amp(1) = 2.3e-9 above) and
#otherwise for dimensionless transfer functions set scalar_amp(1)=1 and use
#CMB_outputscale = 1
CMB_outputscale = 7.4311e12
#Transfer function settings, transfer_kmax=0.5 is enough for sigma_8
#transfer_k_per_logint=0 sets sensible non-even sampling;
#transfer_k_per_logint=5 samples fixed spacing in log-k
#transfer_interp_matterpower =T produces matter power in regular interpolated grid in log k;
# use transfer_interp_matterpower =F to output calculated values (e.g. for later interpolation)
transfer_high_precision = T
transfer_kmax = 100
transfer_k_per_logint = 0
transfer_num_redshifts = 1
transfer_interp_matterpower = T
#Matter power spectrum output against k/h in units of h^{-3} Mpc^3
#--------------------------------------------------------------
transfer_redshift(1) = 3.5
#=============================================================
#Output files not produced if blank. make camb_fits to use use the FITS setting.
scalar_output_file = scalCls.dat
vector_output_file = vecCls.dat
tensor_output_file = tensCls.dat
total_output_file = totCls.dat
lensed_output_file = lensedCls.dat
lensed_total_output_file =lensedtotCls.dat
lens_potential_output_file = lenspotentialCls.dat
FITS_filename = scalCls.fits
#Bispectrum parameters if required; primordial is currently only local model (fnl=1)
#lensing is fairly quick, primordial takes several minutes on quad core
do_lensing_bispectrum = F
do_primordial_bispectrum = F
#1 for just temperature, 2 with E
bispectrum_nfields = 1
#set slice non-zero to output slice b_{bispectrum_slice_base_L L L+delta}
bispectrum_slice_base_L = 0
bispectrum_ndelta=3
bispectrum_delta(1)=0
bispectrum_delta(2)=2
bispectrum_delta(3)=4
#bispectrum_do_fisher estimates errors and correlations between bispectra
#note you need to compile with LAPACK and FISHER defined to use get the Fisher info
bispectrum_do_fisher= F
#Noise is in muK^2, e.g. 2e-4 roughly for Planck temperature
bispectrum_fisher_noise=0
bispectrum_fisher_noise_pol=0
bispectrum_fisher_fwhm_arcmin=7
#Filename if you want to write full reduced bispectrum (at sampled values of l_1)
bispectrum_full_output_file=
bispectrum_full_output_sparse=F
#Export alpha_l(r), beta_l(r) for local non-Gaussianity
bispectrum_export_alpha_beta=F
##Optional parameters to control the computation speed,accuracy and feedback
#If feedback_level > 0 print out useful information computed about the model
feedback_level = 1
# 1: curved correlation function, 2: flat correlation function, 3: inaccurate harmonic method
lensing_method = 1
accurate_BB = F
#massive_nu_approx: 0 - integrate distribution function
# 1 - switch to series in velocity weight once non-relativistic
massive_nu_approx = 1
#Whether you are bothered about polarization.
accurate_polarization = T
#Whether you are bothered about percent accuracy on EE from reionization
accurate_reionization = T
#whether or not to include neutrinos in the tensor evolution equations
do_tensor_neutrinos = F
#Whether to turn off small-scale late time radiation hierarchies (save time,v. accurate)
do_late_rad_truncation = T
#Computation parameters
#if number_of_threads=0 assigned automatically
number_of_threads = 0
#Default scalar accuracy is about 0.3% (except lensed BB) if high_accuracy_default=F
#If high_accuracy_default=T the default taget accuracy is 0.1% at L>600 (with boost parameter=1 below)
#Try accuracy_boost=2, l_accuracy_boost=2 if you want to check stability/even higher accuracy
#Note increasing accuracy_boost parameters is very inefficient if you want higher accuracy,
#but high_accuracy_default is efficient
high_accuracy_default=T
#Increase accuracy_boost to decrease time steps, use more k values, etc.
#Decrease to speed up at cost of worse accuracy. Suggest 0.8 to 3.
accuracy_boost = 1.
#Larger to keep more terms in the hierarchy evolution.
l_accuracy_boost = 1
#Increase to use more C_l values for interpolation.
#Increasing a bit will improve the polarization accuracy at l up to 200 -
#interpolation errors may be up to 3%
#Decrease to speed up non-flat models a bit
l_sample_boost = 1