#Parameters for CAMB #output_root is prefixed to output file names output_root = test #What to do get_scalar_cls = T get_vector_cls = F get_tensor_cls = F get_transfer = T #if do_lensing then lens_potential_output_file contains the unlensed CMB and lensing potential power spectra #and lensed CMB Cls (without tensors) are in lensed_output_file, total in lensed_total_output_file. do_lensing = F # 0: linear, 1: non-linear matter power (HALOFIT), 2: non-linear CMB lensing (HALOFIT), # 3: both non-linear matter power and CMB lensing (HALOFIT) do_nonlinear = 0 #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 # To get accurate lensing potential you also need 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 = 2200 #k_eta_max_scalar = 4000 # 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 physical densities in baryons, CDM and neutrinos + Omega_k use_physical = T ombh2 = "I cannot tell you!" omch2 = "I cannot tell you!" omnuh2 = 0 omk = 0 hubble = "I cannot tell you!" #effective equation of state parameter for dark energy w = -1 #constant comoving sound speed of the dark energy (1=quintessence) cs2_lam = 1 #varying w is not supported by default, compile with EQUATIONS=equations_ppf to use crossing PPF w-wa model: #wa = 0 ##if use_tabulated_w read (a,w) from the following user-supplied file instead of above #use_tabulated_w = F #wafile = wa.dat #if use_physical = F set parameters as here temp_cmb = 2.7255 helium_fraction = 0.2454 #for share_delta_neff = T, the fractional part of massless_neutrinos gives the change in the effective number #(for QED + non-instantaneous decoupling) i.e. the increase in neutrino temperature, #so Neff = massless_neutrinos + sum(massive_neutrinos) #For full neutrino parameter details see http://cosmologist.info/notes/CAMB.pdf massless_neutrinos = 3.046 #number of distinct mass eigenstates nu_mass_eigenstates = 1 #array of the integer number of physical neutrinos per eigenstate, e.g. massive_neutrinos = 2 1 massive_neutrinos = 0 #specify whether all neutrinos should have the same temperature, specified from fractional part of massless_neutrinos share_delta_neff = F #nu_mass_fractions specifies how Omeganu_h2 is shared between the eigenstates #i.e. to indirectly specify the mass of each state; e.g. nu_mass_factions= 0.75 0.25 nu_mass_fractions = 1 #if share_delta_neff = F, specify explicitly the degeneracy for each state (e.g. for sterile with different temperature to active) #(massless_neutrinos must be set to degeneracy for massless, i.e. massless_neutrinos does then not include Deleta_Neff from massive) #if share_delta_neff=T then degeneracies is not given and set internally #e.g. for massive_neutrinos = 2 1, this gives equal temperature to 4 neutrinos: nu_mass_degeneracies = 2.030 1.015, massless_neutrinos = 1.015 nu_mass_degeneracies = #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) = "I cannot tell you!" scalar_spectral_index(1) = 0.9649 scalar_nrun(1) = 0 scalar_nrunrun(1) = 0 tensor_spectral_index(1) = 0 tensor_nrun(1) = 0 #Three parameterizations (1,2,3) for tensors, see http://cosmologist.info/notes/CAMB.pdf tensor_parameterization = 1 #ratio is that of the initial tens/scal power spectrum amplitudes, depending on parameterization #for tensor_parameterization == 1, P_T = initial_ratio*scalar_amp*(k/pivot_tensor)^tensor_spectral_index #for tensor_parameterization == 2, P_T = initial_ratio*P_s(pivot_tensor)*(k/pivot_tensor)^tensor_spectral_index #Note that for general pivot scales and indices, tensor_parameterization==2 has P_T depending on n_s initial_ratio(1) = 1 #tensor_amp is used instead if tensor_parameterization == 3, P_T = tensor_amp *(k/pivot_tensor)^tensor_spectral_index #tensor_amp(1) = 4e-10 #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 = 0.09 #If re_use_optical_depth = F then use following, otherwise ignored re_redshift = 11 #width of reionization transition. CMBFAST model was similar to re_delta_redshift~0.5. re_delta_redshift = 1.5 #re_ionization_frac=-1 sets it to become fully ionized using Yhe to get helium contribution #Otherwise x_e varies from 0 to re_ionization_frac re_ionization_frac = -1 #Parameters for second reionization of helium re_helium_redshift = 3.5 re_helium_delta_redshift = 0.5 #RECFAST 1.5.x recombination parameters; RECFAST_fudge = 1.14 RECFAST_fudge_He = 0.86 RECFAST_Heswitch = 6 RECFAST_Hswitch = T # CosmoMC parameters - compile with RECOMBINATION=cosmorec and link to CosmoMC to use these # # cosmorec_runmode== 0: CosmoMC run with diffusion # 1: CosmoMC run without diffusion # 2: RECFAST++ run (equivalent of the original RECFAST version) # 3: RECFAST++ run with correction function of Calumba & Thomas, 2010 # # For 'cosmorec_accuracy' and 'cosmorec_fdm' see CosmoMC for explanation #--------------------------------------------------------------------------------------- #cosmorec_runmode = 0 #cosmorec_accuracy = 0 #cosmorec_fdm = 0 #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 Culs #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 = 7.42835025e12 #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 = 50 transfer_k_per_logint = 100 transfer_num_redshifts = 1 transfer_interp_matterpower = T transfer_redshift(1) = 0 transfer_filename(1) = transfer_out.dat #Matter power spectrum output against k/h in units of h^{-3} Mpc^3 transfer_matterpower(1) = matterpower.dat #which variable to use for defining the matter power spectrum and sigma8 #main choices are 2: CDM, 7: CDM+baryon+neutrino, 8: CDM+baryon, 9: CDM+baryon+neutrino+de perts transfer_power_var = 7 #Output files not produced if blank. make camb_fits to 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 #whether to start output files with comment describing columns output_file_headers = T #write out various derived parameters derived_parameters = T # 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 = T #Whether to turn off small-scale late time radiation hierarchies (save time,v. accurate) do_late_rad_truncation = T #Which version of Halofit approximation to use (default currently Takahashi): #1. original, 2. Bird et al. update, 3. (1) plus fudge from http://www.roe.ac.uk/~jap/haloes/, 4. Takahashi #5. Use HMcode (Mead et al. 2015,2016), 6. Use halomodel (a standard calculation, without the accuracy tweaks of HMcode) #7. PKequal (arXiv:0810.0190, arXiv:1601.07230) halofit_version= #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 target 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 = 4 #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