input_params_post_SBRS.yaml

#---
# This parameter file is for fitting post-reconstruction galaxy power spectrum at z=1.0. We use SBRS model.
# Input observed power spectra and the diagonal terms of covariance matrix
# input observed (simulated) wiggle (with BAO) power spectrum
Pwig_ifile: ./input_files/z1mcut34/Rkaves.W10_fof_0.5000ga.dat   

# input nowiggle power spectrum
Pnow_ifile: ./input_files/z1mcut34/Rkaves.N10_fof_0.5000ga.dat   

# input diagonal terms of covariance matrix of Pwig-Pnow
diag_Cov_Pwnw_ifile: ./input_files/z1mcut34/Rkaves.diag_Cov_Pwnw_fof_a_0.5000.dat    

# input linear power spectrum
Pwig_linear: ./input_files/planck_camb_56106182_matterpower_z0.dat
Pnow_linear: ./input_files/planck_camb_56106182_matterpower_smooth_z0.dat

# Fitting parameters; assign initial value before fitting 
# ----- post-reconstruction SBRS model --------#
# Sigma2_dd, Sigma2_sd and Sigma2_ss depend on Sigma2_sm. The input values are random numbers  
init_params: {"alpha_perp": 1.0, "alpha_para": 1.0, "Sigma_xy": 10.0, "Sigma_z": 10.0, "Sigma_sm": 7.874, "Sigma_fog": 0.0, "f": 0.5, "b_1": 1.0, "b_partial": 0.0}

# We free parameter Sigma2_sm, but fix Sigma2_dd, Sigma2_sd and Sigma2_ss from theoretical calculation.
params_indices: [1, 1, 0, 0, 0, 0, 1, 1, 0]   
all_temperature: [0.01, 0.01, 1.0, 1.0, 1.0, 1.0, 0.1, 0.1, 0.1]

N_walkers: 40    # number of MCMC random walkers in each chain
Omega_m: 0.3075  # matter density of the background \Lambda CDM model
sim_z: 1.0       # redshift of the input files

# for sim_z in ['0', '0.6', '1.0', '1.5', '2.0', '2.5'], the corresponding growth factor is
# f_theory = [0.5198, 0.7862, 0.8730, 0.9290, 0.9572, 0.9724]         # f=dlnD/dlna, caculated from growth_fun.py
f_theory: 0.8730
# output file
ofile_name: 'Rkaves.fof_mcut34_wnw_10_diff_z{}_params{}_SBRS.out'  

#...