def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
# define array for values of z and data points
self.z = np.array([], 'float64')
self.data = np.array([], 'float64')
self.error = np.array([], 'float64')
self.type = np.array([], 'int')
# read redshifts and data points
for line in open(self.data_directory + self.file, 'r'):
if (line.find('#') == -1):
self.z = np.append(self.z, float(line.split()[0]))
self.data = np.append(self.data, float(line.split()[1]))
self.error = np.append(self.error, float(line.split()[2]))
self.type = np.append(self.type, int(line.split()[3]))
# number of data points
self.num_points = np.shape(self.z)[0]
for i in range(self.num_points):
if self.type[i] == 3:
self.data[i] = self.data[i] * self.known_rs
self.error[i] = self.data[i] * sqrt(
(self.error[i] / self.data[i]) ** 2 + (self.rs_error / self.known_rs) ** 2)
self.type[i] = 4
def __init__(self, path, data, command_line):
"""
The structure differs significantly from other likelihoods, in order to
follow as simply as possible the data structure.
Each redshift bin in WiggleZ contains a .dataset file with information
on this redshift bin. The structure to read this has been encoded in
the class likelihood_mpk. It will be used also with the next data
release of SDSS.
The whole WiggleZ is then made out of the four likelihood_mpk:
WiggleZ_a, b, c and d, which are **defined dynamically** thanks to the
:func:`type` function in python, inheriting from
:class:`likelihood_mpk`.
Some additional keyword arguments are sent to the initialization of
these classes, in order to use the function
:meth:`add_common_knowledge`. It then gives a dictionary of shared
attributes that should be distributed to all four redshift bins.
"""
likelihood.__init__(self, path, data, command_line)
# This obscure command essentially creates dynamically 4 likelihoods,
# respectively called WiggleZ_a, b, c and d, inheriting from
# likelihood_mpk.
for elem in ['a', 'b', 'c', 'd']:
exec("WiggleZ_%s = type('WiggleZ_%s', (likelihood_mpk, ), {})" % \
(elem, elem))
# Initialize one after the other the four independant redshift bins (note:
# the order in the array self.redshift_bins_files) must be respected !
self.wigglez_a = WiggleZ_a(
self.data_directory + self.redshift_bins_files[0], data,
command_line, common=True, common_dict=self.common)
self.wigglez_b = WiggleZ_b(
self.data_directory + self.redshift_bins_files[1], data,
command_line, common=True, common_dict=self.common)
self.wigglez_c = WiggleZ_c(
self.data_directory + self.redshift_bins_files[2], data,
command_line, common=True, common_dict=self.common)
self.wigglez_d = WiggleZ_d(
self.data_directory + self.redshift_bins_files[3], data,
command_line, common=True, common_dict=self.common)
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
# define array for values of z and data points
self.z = np.array([], 'float64')
self.data = np.array([], 'float64')
self.error = np.array([], 'float64')
self.type = np.array([], 'int')
# read redshifts and data points
for line in open(self.data_directory + self.file, 'r'):
if (line.find('#') == -1):
self.z = np.append(self.z, float(line.split()[0]))
self.data = np.append(self.data, float(line.split()[1]))
self.error = np.append(self.error, float(line.split()[2]))
self.type = np.append(self.type, int(line.split()[3]))
# number of data points
self.num_points = np.shape(self.z)[0]
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
# define array for values of z and data points
self.z = np.array([], 'float64')
self.moduli = np.array([], 'float64')
# read redshifts and data points
for line in open(self.data_directory + self.z_mu_dmu, 'r'):
if (line.find('#') == -1):
self.z = np.append(self.z, float(line.split()[1]))
self.moduli = np.append(self.moduli, float(line.split()[2]))
# number of data points
self.num_points = np.shape(self.z)[0]
# define correlation m,atrix
covmat = np.zeros((self.num_points, self.num_points), 'float64')
# file containing correlation matrix
if self.has_syscovmat:
covmat_filename = self.covmat_sys
else:
covmat_filename = self.covmat_nosys
# read correlation matrix
i = 0
for line in open(self.data_directory + covmat_filename, 'r'):
if (line.find('#') == -1):
covmat[i] = line.split()
i += 1
# invert correlation matrix
self.inv_covmat = np.linalg.inv(covmat)
# find sum of all matrix elements (sounds odd that there is
# not a trace here instead, but this is correct!)
self.inv_covmat_sum = np.sum(self.inv_covmat)
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
# define array for values of z and data points
self.zd = np.array([], 'float64')
self.zs = np.array([], 'float64')
self.lambda_d = np.array([], 'float64')
self.mu_d = np.array([], 'float64')
self.sigma_d = np.array([], 'float64')
# read redshifts and data points
for line in open(self.data_directory + self.file, 'r'):
if (line.find("#") == -1):
self.zd = np.append(self.zd, float(line.split()[0]))
self.zs = np.append(self.zs, float(line.split()[1]))
self.lambda_d = np.append(
self.lambda_d, float(line.split()[2]))
self.mu_d = np.append(self.mu_d, float(line.split()[3]))
self.sigma_d = np.append(self.sigma_d, float(line.split()[4]))
# number of data points
self.num_points = np.shape(self.zd)[0]
def __init__(self, path, data, command_line):
# Standard initialization, reads the .data
likelihood.__init__(self, path, data, command_line)
# Extra needed cosmological paramters
self.need_cosmo_arguments(
data, {'output': 'tCl pCl lCl', 'lensing': 'yes'})
try:
import pywlik
except ImportError:
print " /|\ You must first activate the binaries from the wmap wrapper code,"
print "/_o_\ please run : source /path/to/montepython/wrapper_wmap/bin/clik_profile.sh"
print " and try again."
exit()
# try importing the wrapper_wmap
self.wmaplike = pywlik.wlik(self.large_data_directory, self.ttmin,
self.ttmax, self.temin, self.temax, self.use_gibbs, self.use_lowlpol)
# self.cls = np.loadtxt(self.cl_test_file)
# loglike = self.wmaplike(self.cls)
# print "got %g expected %g"%(loglike,-845.483)
self.l_max = max(self.ttmax, self.temax)
self.need_cosmo_arguments(data, {'l_max_scalars': self.l_max})
# deal with nuisance parameters
try:
self.use_nuisance
except:
self.use_nuisance = []
self.read_contamination_spectra(data)
pass
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
self.need_cosmo_arguments(data, {'output':'mPk'})
#################
# find number of galaxies for each mean redshift value
#################
# Compute the number of galaxies for each \bar z
# For this, one needs dn/dz TODO
# then n_g(\bar z) = int_{\bar z - dz/2}^{\bar z + dz/2} dn/dz dz
# self.z_mean will contain the central values
self.z_mean = np.zeros(self.nbin,'float64')
# Deduce the dz step from the number of bins and the edge values of z
self.dz = (self.zmax-self.zmin)/(self.nbin-1.)
i=0
for z in np.arange(self.zmin,self.zmax+self.dz,self.dz):
self.z_mean[i] = z
i+=1
# Store the z edge values
self.z_edges = np.zeros(self.nbin+1,'float64')
i = 0
for z in np.arange(self.zmin-self.dz/2.,self.zmax+self.dz,self.dz):
self.z_edges[i] = z
i+=1
# Store the total vector z, with edges + mean
self.z = np.zeros(2*self.nbin+1,'float64')
i=0
for z in np.arange(self.zmin-self.dz/2.,self.zmax+self.dz,self.dz/2.):
self.z[i] = z
i+=1
self.need_cosmo_arguments(data,{'z_max_pk':self.z[-1]})
# For each bin, compute the biais function,
self.b = np.zeros(self.nbin,'float64')
for Bin in range(self.nbin):
self.b[Bin] = sqrt(self.z_mean[Bin]+1.)
# Force the cosmological module to store Pk for k up to an arbitrary number
# (since self.r is not yet decided)... TODO
self.need_cosmo_arguments(data,{'P_k_max_1/Mpc':1.5*self.kmax})
# Define the k values for the integration (from kmin to kmax), at which the
# spectrum will be computed (and stored for the fiducial model)
# k_size is deeply arbitrary here, TODO
self.k_fid = np.zeros(self.k_size,'float64')
for i in range(self.k_size):
self.k_fid[i] = exp( i*1.0 /(self.k_size-1) * log(self.kmax/self.kmin) + log(self.kmin))
################
# Noise spectrum TODO properly
################
self.n_g = np.zeros(self.nbin,'float64')
#for index_z in range(self.nbin):
#print self.z_mean[index_z],self.z[2*index_z],self.z[2*index_z+2]
#self.n_g[index_z] = self.galaxy_distribution(self.z[2*index_z+2]) - self.galaxy_distribution(self.z[2*index_z])
#print self.n_g
self.n_g[0] = 6844.945
self.n_g[1] = 7129.45
self.n_g[2] = 7249.912
self.n_g[3] = 7261.722
self.n_g[4] = 7203.825
self.n_g[5] = 7103.047
self.n_g[6] = 6977.571
self.n_g[7] = 6839.546
self.n_g[8] = 6696.957
self.n_g[9] = 5496.988
self.n_g[10] = 4459.240
self.n_g[11] = 3577.143
self.n_g[12] = 2838.767
self.n_g[13] = 2229.282
self.n_g[14] = 1732.706
self.n_g[15] = 1333.091
self.n_g = self.n_g * self.efficiency * 41253.
# If the file exists, initialize the fiducial values,
# the spectrum will be read first, with k_size values of k and nbin values
# of z. Then, H_fid and D_A fid will be read (each with nbin values).
#self.Cl_fid = np.zeros((self.nlmax,self.nbin,self.nbin),'float64')
self.fid_values_exist = False
self.pk_nl_fid = np.zeros((self.k_size,2*self.nbin+1),'float64')
self.H_fid = np.zeros(2*self.nbin+1,'float64')
self.D_A_fid = np.zeros(2*self.nbin+1,'float64')
self.sigma_r_fid = np.zeros(self.nbin,'float64')
if os.path.exists(self.data_directory+'/'+self.fiducial_file):
self.fid_values_exist = True
fid_file = open(self.data_directory+'/'+self.fiducial_file,'r')
line = fid_file.readline()
while line.find('#')!=-1:
line = fid_file.readline()
while (line.find('\n')!=-1 and len(line)==1):
line = fid_file.readline()
for index_k in range(self.k_size):
for index_z in range(2*self.nbin+1):
self.pk_nl_fid[index_k,index_z] = float(line)
line = fid_file.readline()
for index_z in range(2*self.nbin+1):
self.H_fid[index_z] = float(line.split()[0])
self.D_A_fid[index_z] = float(line.split()[1])
line = fid_file.readline()
for index_z in range(self.nbin):
self.sigma_r_fid[index_z] = float(line)
line = fid_file.readline()
fid_file.seek(0)
fid_file.close()
# Else the file will be created in the loglkl() function.
return
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
############ read data ###########
self.z = np.zeros(self.num_z,'float64')
self.k = np.zeros(self.num_k,'float64')
self.pk_obs = np.zeros((self.num_k,self.num_z),'float64')
self.npk_obs = np.zeros((self.num_k,self.num_z),'float64')
covmat = np.zeros((self.num_k*self.num_z,self.num_k*self.num_z),'float64')
invcovmat = np.zeros((self.num_k*self.num_z,self.num_k*self.num_z),'float64')
self.inv_covmat = np.zeros((self.num_k,self.num_z,self.num_k,self.num_z),'float64')
self.dampcorr = np.zeros((self.num_k,self.num_z),'float64')
# k, z, pk, noise
inputfile = open(self.data_directory+self.table,'r')
for zz in range(self.num_z):
for kk in range(self.num_k):
line = inputfile.readline()
zzz = float(line.split()[0])
if self.z[zz] == 0.:
self.z[zz]=zzz
else:
if self.z[zz] != zzz:
print 'input data table not arranged as expected',self.z[zz],zzz
exit()
kkk = float(line.split()[1])
if self.k[kk] == 0.:
self.k[kk]=kkk
else:
if self.k[kk] != kkk:
print 'input data table not arranged as expected',self.k[kk],kkk
exit()
self.pk_obs[kk,zz] = line.split()[2]
self.npk_obs[kk,zz] = line.split()[4]
inputfile.close()
# covariance matrix
inputfile = open(self.data_directory+self.covar,'r')
for np1 in range(self.num_k*self.num_z):
line = inputfile.readline()
for np2 in range(self.num_k*self.num_z):
covmat[np1,np2] = float(line.split()[np2])
inputfile.close()
# invert covariance matrix and store it with good indicing
invcovmat = np.linalg.inv(covmat)
for zz1 in range(self.num_z):
for kk1 in range(self.num_k):
for zz2 in range(self.num_z):
for kk2 in range(self.num_k):
self.inv_covmat[kk1,zz1,kk2,zz2]=invcovmat[zz1*self.num_k+kk1,zz2*self.num_k+kk2]
# damping factors
inputfile = open(self.data_directory+self.damp,'r')
for zz in range(self.num_z):
for kk in range(self.num_k):
line = inputfile.readline()
self.dampcorr[kk,zz] = float(line)
inputfile.close()
############ read theory ###########
# index of parameters entering in calculation of theoretical flux spectrum (Taylor expansion parameters)
index = 0
self.index_s8 = index
index+=1
self.index_ns = index
index+=1
self.index_Om = index
index+=1
self.index_H0 = index
index+=1
# self.index_zr = index
# index+=1
self.index_g = index
index+=1
self.index_tf = index
index+=1
self.index_t0 = index
index+=1
self.index_num = index
# read Taylor coefficients for these parameters
# each table contains:
#
# [k1, z1, 2nd order] ...... [k1, zmax, 2nd order]
# [k2, z1, 2nd order] ...... [k2, zmax, 2nd order]
# ...............................................
# [kmax, z1, 2nd order] ...... [kmax, zmax, 2nd order]
# [k1, z1, 1st order] ...... [k1, zmax, 1st order]
# [k2, z1, 1st order] ...... [k2, zmax, 1st order]
# ...............................................
# [kmax, z1, 1st order] ...... [kmax, zmax, 1st order]
self.taylor = np.zeros((self.index_num,self.num_k,self.num_z,2),'float64')
for param in range(self.index_num):
if (param == self.index_s8):
table_name = 's8_gamma1_new.dat'
if (param == self.index_ns):
table_name = 'n_gamma1_new.dat'
if (param == self.index_Om):
table_name = 'om_gamma1_new.dat'
if (param == self.index_H0):
table_name = 'h_gamma1_new.dat'
if (param == self.index_g):
table_name = 'coeff_gammaEQ1_all_pk_new.dat'
if (param == self.index_tf):
table_name = 'meanflux_gamma1_new.dat'
if (param == self.index_t0):
table_name = 't0_gamma1_new.dat'
# if (param == self.index_zr):
# table_name = 'highzreion.dat'
inputfile = open(self.data_directory+table_name,'r')
# reio table is special: only 1st order coefs, only 2nd half of table
# if (param == self.index_zr):
# for kk in range(self.num_k):
# for zz in range(self.num_z):
# self.taylor[param,kk,zz,1] = 0. # 2nd order fixed to zero
# for kk in range(self.num_k):
# line = inputfile.readline()for kk in range(self.num_k):
# for zz in range(self.num_z):
# self.taylor[param,kk,zz,0] = line.split()[zz]-1. # 1st order gets correction by one
# else:
# other tables
for kk in range(self.num_k):
line = inputfile.readline()
for zz in range(self.num_z):
self.taylor[param,kk,zz,1] = float(line.split()[zz])
for kk in range(self.num_k):
line = inputfile.readline()
for zz in range(self.num_z):
self.taylor[param,kk,zz,0] = float(line.split()[zz])
inputfile.close()
# read best-fit values around which Taylor expansion is performed
self.taylor_expansion_point = np.zeros((self.index_num,self.num_z),'float64')
self.taylor_expansion_point[self.index_s8,0] = 0.85
self.taylor_expansion_point[self.index_ns,0] = 0.95
self.taylor_expansion_point[self.index_Om,0] = 0.26
self.taylor_expansion_point[self.index_H0,0] = 72.
# self.taylor_expansion_point[self.index_zr,0] = 6.
self.taylor_expansion_point[self.index_tf,0] = 0.178000
self.taylor_expansion_point[self.index_tf,1] = 0.2192
self.taylor_expansion_point[self.index_tf,2] = 0.2714000
self.taylor_expansion_point[self.index_tf,3] = 0.3285330
self.taylor_expansion_point[self.index_tf,4] = 0.379867
self.taylor_expansion_point[self.index_tf,5] = 0.42900
self.taylor_expansion_point[self.index_tf,6] = 0.513000
self.taylor_expansion_point[self.index_tf,7] = 0.600400
self.taylor_expansion_point[self.index_tf,8] = 0.657800
self.taylor_expansion_point[self.index_tf,9] = 0.756733
self.taylor_expansion_point[self.index_tf,10] = 0.896000
self.taylor_expansion_point[self.index_g,0] = 1.05
self.taylor_expansion_point[self.index_g,1] = 1.05
self.taylor_expansion_point[self.index_g,2] = 1.05
self.taylor_expansion_point[self.index_g,3] = 1.05
self.taylor_expansion_point[self.index_g,4] = 1.05
self.taylor_expansion_point[self.index_g,5] = 1.05
self.taylor_expansion_point[self.index_g,6] = 1.04
self.taylor_expansion_point[self.index_g,7] = 1.04
self.taylor_expansion_point[self.index_g,8] = 1.03
self.taylor_expansion_point[self.index_g,9] = 1.03
self.taylor_expansion_point[self.index_g,10] = 1.03
self.taylor_expansion_point[self.index_t0,0] = 20600
self.taylor_expansion_point[self.index_t0,1] = 21100
self.taylor_expansion_point[self.index_t0,2] = 21600
self.taylor_expansion_point[self.index_t0,3] = 22000
self.taylor_expansion_point[self.index_t0,4] = 22300
self.taylor_expansion_point[self.index_t0,5] = 22492
self.taylor_expansion_point[self.index_t0,6] = 22600
self.taylor_expansion_point[self.index_t0,7] = 22600
self.taylor_expansion_point[self.index_t0,8] = 22505
self.taylor_expansion_point[self.index_t0,9] = 22200
self.taylor_expansion_point[self.index_t0,10] = 21529
# flux spectrum of best-fit model
self.pkth = np.zeros((self.num_k,self.num_z),'float64')
inputfile = open(self.data_directory+'B2_gamma1_all.txt','r')
for zz in range(self.num_z):
for kk in range(self.num_k):
self.pkth[kk,zz] = float(inputfile.readline())
inputfile.close()
# resolution box size correction
inputfile = open(self.data_directory+'res_box_table_all.txt','r')
for kk in range(self.num_k):
line = inputfile.readline()
for zz in range(self.num_z):
rb = float(line.split()[zz])
self.pkth[kk,zz] *= rb
inputfile.close()
######## end read theory ##########
# necessary class parameters. mPk and k_max=2h/Mpc needed to have sigma_8 computed and accurate !
self.need_cosmo_arguments(data,{'output':'mPk', 'P_k_max_h/Mpc':2})
return
def __init__(self, path, data, command_line):
likelihood.__init__(self, path, data, command_line)
self.need_cosmo_arguments(data,{'output':'mPk'})
# Define array of l values, and initialize them
self.l = np.zeros(self.nlmax,'float64')
for nl in range(self.nlmax):
self.l[nl] = 1.*math.exp(self.dlnl*nl)
#print self.l[:]
#exit()
########################################################
# Find distribution of dn_dz (not normalized) in each bin
########################################################
# Assuming each bin contains the same number of galaxies, we find the bin
# limits in z space
# Compute the total number of galaxies until zmax (no normalization yet)
n_tot = 0.
for z in np.arange(0,self.zmax+self.dz,self.dz):
gd_1 = self.galaxy_distribution(z)
gd_2 = self.galaxy_distribution(z+self.dz)
n_tot += 0.5*(gd_1+gd_2)*self.dz
# For each bin, compute the limit in z space
# Create the array that will contain the z boundaries for each bin. The
# first value is already correctly set to 0.
self.z_bin_edge = np.zeros(self.nbin+1,'float64')
for Bin in range(self.nbin-1):
bin_count = 0.
z =self.z_bin_edge[Bin]
while (bin_count <= n_tot/self.nbin):
gd_1 = self.galaxy_distribution(z)
gd_2 = self.galaxy_distribution(z+self.dz)
bin_count += 0.5*(gd_1+gd_2)*self.dz
z += self.dz
self.z_bin_edge[Bin+1] = z
self.z_bin_edge[self.nbin] = self.zmax
# Fill array of discrete z values
self.z = np.zeros(self.nzmax,'float64')
for nz in range(self.nzmax):
self.z[nz] = (nz*1.0)/(self.nzmax-1.0)*self.zmax
# Force the cosmological module to store Pk for redshifts up to max(self.z)
self.need_cosmo_arguments(data,{'z_max_pk':self.z[-1]})
# Force the cosmological module to store Pk for k up to an arbitrary number
# (since self.r is not yet decided)... TODO
self.need_cosmo_arguments(data,{'P_k_max_1/Mpc':self.k_max})
# Fill distribution for each bin (convolving with photo_z distribution)
self.eta_z = np.zeros((self.nzmax,self.nbin),'float64')
for Bin in range(self.nbin):
for nz in range(self.nzmax):
z = self.z[nz]
self.eta_z[nz,Bin] = 0.
for nz2 in range(1,self.nzmax):
if ((self.z[nz2] >= self.z_bin_edge[Bin]) and (self.z[nz2] <= self.z_bin_edge[Bin+1])):
gd = self.galaxy_distribution(self.z[nz2])
pzd = self.photo_z_distribution(z,self.z[nz2])
integrand_plus = gd*pzd
else:
integrand_plus = 0.
if ((self.z[nz2-1] >= self.z_bin_edge[Bin]) and (self.z[nz2-1] <= self.z_bin_edge[Bin+1])):
gd = self.galaxy_distribution(self.z[nz2-1])
pzd = self.photo_z_distribution(z,self.z[nz2-1])
integrand_minus = gd*pzd
else:
integrand_minus = 0.
self.eta_z[nz,Bin] += 0.5*(integrand_plus+integrand_minus)*(self.z[nz2]-self.z[nz2-1])
#for nz in range(self.nzmax):
# print self.z[nz],self.eta_z[nz,0],self.eta_z[nz,1],self.eta_z[nz,2],self.eta_z[nz,3],self.eta_z[nz,4],self.galaxy_distribution(self.z[nz])
#exit()
# integrate eta(z) over z (in view of normalizing it to one)
self.eta_norm = np.zeros(self.nbin,'float64')
for Bin in range(self.nbin):
self.eta_norm[Bin] = np.sum(0.5*(self.eta_z[1:,Bin]+self.eta_z[:-1,Bin])*(self.z[1:]-self.z[:-1]))
################
# Noise spectrum
################
# Number of galaxies per steradian
self.noise = 3600.*self.gal_per_sqarcmn*(180./math.pi)**2
# Number of galaxies per steradian per bin
self.noise = self.noise/self.nbin
# Noise spectrum (diagonal in bin*bin space, independent of l and Bin)
self.noise = self.rms_shear**2/self.noise
# TEST
#self.noise = 0
###########
# Read data
###########
# If the file exists, initialize the fiducial values
self.Cl_fid = np.zeros((self.nlmax,self.nbin,self.nbin),'float64')
self.fid_values_exist = False
if os.path.exists(self.data_directory+'/'+self.fiducial_file):
self.fid_values_exist = True
fid_file = open(self.data_directory+'/'+self.fiducial_file,'r')
line = fid_file.readline()
while line.find('#')!=-1:
line = fid_file.readline()
while (line.find('\n')!=-1 and len(line)==1):
line = fid_file.readline()
for nl in range(self.nlmax):
for Bin in range(self.nbin):
for Bin2 in range(self.nbin):
self.Cl_fid[nl,Bin,Bin2] = float(line)
line = fid_file.readline()
# Else the file will be created in the loglkl() function.
return
