How to use pyccl - 10 common examples
To help you get started, we’ve selected a few pyccl examples, based on popular ways it is used in public projects.
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LSSTDESC / CLMM / clmm / modbackend / ccl.py View on Github 
def eval_sigma_crit (self, z_len, z_src):
a_len = _get_a_from_z (z_len)
a_src = np.atleast_1d (_get_a_from_z (z_src))
cte = ccl.physical_constants.CLIGHT**2 / (4.0 * np.pi * ccl.physical_constants.GNEWT * ccl.physical_constants.SOLAR_MASS) * ccl.physical_constants.PC_TO_METER
z_cut = (a_src < a_len)
if np.isscalar (a_len):
a_len = np.repeat (a_len, len (a_src))
res = np.zeros_like (a_src)
if np.any (z_cut):
Ds = ccl.angular_diameter_distance (self.cosmo, a_src[z_cut])
Dl = ccl.angular_diameter_distance (self.cosmo, a_len)
Dls = ccl.angular_diameter_distance (self.cosmo, a_len, a_src[z_cut])
res[z_cut] = (cte * Ds / (Dl * Dls)) * self.cor_factor * 1.0e-6 / self.cosmo['h']
res[~z_cut] = np.Inf
return np.squeeze (res)def eval_sigma_crit (self, z_len, z_src):
a_len = _get_a_from_z (z_len)
a_src = np.atleast_1d (_get_a_from_z (z_src))
cte = ccl.physical_constants.CLIGHT**2 / (4.0 * np.pi * ccl.physical_constants.GNEWT * ccl.physical_constants.SOLAR_MASS) * ccl.physical_constants.PC_TO_METER
z_cut = (a_src < a_len)
if np.isscalar (a_len):
a_len = np.repeat (a_len, len (a_src))
res = np.zeros_like (a_src)
if np.any (z_cut):
Ds = ccl.angular_diameter_distance (self.cosmo, a_src[z_cut])
Dl = ccl.angular_diameter_distance (self.cosmo, a_len)
Dls = ccl.angular_diameter_distance (self.cosmo, a_len, a_src[z_cut])
res[z_cut] = (cte * Ds / (Dl * Dls)) * self.cor_factor * 1.0e-6 / self.cosmo['h']
res[~z_cut] = np.Inf
return np.squeeze (res)def eval_sigma_crit (self, z_len, z_src):
a_len = _get_a_from_z (z_len)
a_src = np.atleast_1d (_get_a_from_z (z_src))
cte = ccl.physical_constants.CLIGHT**2 / (4.0 * np.pi * ccl.physical_constants.GNEWT * ccl.physical_constants.SOLAR_MASS) * ccl.physical_constants.PC_TO_METER
z_cut = (a_src < a_len)
if np.isscalar (a_len):
a_len = np.repeat (a_len, len (a_src))
res = np.zeros_like (a_src)
if np.any (z_cut):
Ds = ccl.angular_diameter_distance (self.cosmo, a_src[z_cut])
Dl = ccl.angular_diameter_distance (self.cosmo, a_len)
Dls = ccl.angular_diameter_distance (self.cosmo, a_len, a_src[z_cut])
res[z_cut] = (cte * Ds / (Dl * Dls)) * self.cor_factor * 1.0e-6 / self.cosmo['h']
res[~z_cut] = np.Inf
return np.squeeze (res)def eval_sigma_crit (self, z_len, z_src):
a_len = _get_a_from_z (z_len)
a_src = np.atleast_1d (_get_a_from_z (z_src))
cte = ccl.physical_constants.CLIGHT**2 / (4.0 * np.pi * ccl.physical_constants.GNEWT * ccl.physical_constants.SOLAR_MASS) * ccl.physical_constants.PC_TO_METER
z_cut = (a_src < a_len)
if np.isscalar (a_len):
a_len = np.repeat (a_len, len (a_src))
res = np.zeros_like (a_src)
if np.any (z_cut):
Ds = ccl.angular_diameter_distance (self.cosmo, a_src[z_cut])
Dl = ccl.angular_diameter_distance (self.cosmo, a_len)
Dls = ccl.angular_diameter_distance (self.cosmo, a_len, a_src[z_cut])
res[z_cut] = (cte * Ds / (Dl * Dls)) * self.cor_factor * 1.0e-6 / self.cosmo['h']
res[~z_cut] = np.Infself.hdpm_opts = {'nfw': {'truncated': False,
'projected_analytic': True,
'cumul2d_analytic': True},
'einasto': {},
'hernquist': {}}
self.halo_profile_model = ''
self.massdef = ''
self.delta_mdef = 0
self.hdpm = None
self.MDelta = 0.0
self.set_cosmo_params_dict ({})
self.set_halo_density_profile (halo_profile_model, massdef, delta_mdef)
self.cor_factor = 2.77533742639e+11 * _patch_comoving_coord_cluster_toolkit_rho_m (1.0, 0.0) / ccl.physical_constants.RHO_CRITICALdef set_cosmo_params_dict (self, cosmo_dict):
h = 0.67
Omega_c = 0.27
Omega_b = 0.045
if 'H0' in cosmo_dict:
h = cosmo_dict['H0'] / 100.0
if 'Omega_b' in cosmo_dict:
Omega_b = cosmo_dict['Omega_b']
if 'Omega_c' in cosmo_dict:
Omega_c = cosmo_dict['Omega_c']
self.cosmo = ccl.Cosmology (Omega_c = Omega_c, Omega_b = Omega_b, h = h, sigma8 = 0.8, n_s = 0.96, T_CMB = 0.0, Neff = 0.0,
transfer_function='bbks', matter_power_spectrum='linear')from astropy import units as u
import pickle
import polaraveraging
import clmm
cosmo_object_type = "astropy"
try:
import pyccl
except:
cosmo_object_type = "astropy"
if cosmo_object_type == "astropy":
from astropy.cosmology import FlatLambdaCDM
cosmo = FlatLambdaCDM(70., Om0 = 0.3) # astropy cosmology setting, will be replaced by ccl
elif cosmo_object_type == "ccl":
import pyccl as ccl
cosmo = ccl.Cosmology(Omega_c=0.25, Omega_b = 0.05,h = 0.7,n_s = 0.97, sigma8 = 0.8, Omega_k = 0.)
cl = clmm.load_cluster('9687686568.p')
ra_l = cl.ra
dec_l = cl.dec
z = cl.z
e1 = cl.galcat['e1']
e2 = cl.galcat['e2']
ra_s = cl.galcat['ra']
dec_s = cl.galcat['dec']
theta, g_t , g_x = polaraveraging._compute_shear(ra_l, dec_l, ra_s, dec_s, e1, e2, sky = "flat") #calculate distance and tangential shear and cross shear for each source galaxy
#theta, g_t , g_x = compute_shear(ra_l, dec_l, ra_s, dec_s, e1, e2, sky = "curved") #curved sky
rMpc = polaraveraging._theta_units_conversion(theta,"Mpc",z,cosmo,cosmo_object_type=cosmo_object_type)raise ValueError (f"Halo density profile mass definition {massdef} not currently supported")
# Check if we have already an instance of the required object, if not create one
if not ((halo_profile_model == self.halo_profile_model) and (massdef == self.massdef) and (delta_mdef == self.delta_mdef)):
self.halo_profile_model = halo_profile_model
self.massdef = massdef
cur_cdelta = 0.0
cur_mdelta = 0.0
cur_values = False
if self.hdpm:
cur_cdelta = self.conc.c
cur_values = True
self.mdef = ccl.halos.MassDef (delta_mdef, self.mdef_dict[massdef])
self.conc = ccl.halos.ConcentrationConstant (self.mdef)
self.mdef.concentration = self.conc
self.hdpm = self.hdpm_dict[halo_profile_model] (self.conc, **self.hdpm_opts[halo_profile_model])
if cur_values:
self.conc.c = cur_cdeltadef __init__ (self, massdef = 'mean', delta_mdef = 200, halo_profile_model = 'nfw', z_max = 5.0):
self.mdef_dict = {'mean': 'matter',
'critial': 'critical',
'virial': 'critical'}
self.hdpm_dict = {'nfw': ccl.halos.HaloProfileNFW,
'einasto': ccl.halos.HaloProfileEinasto,
'hernquist': ccl.halos.HaloProfileHernquist}
self.hdpm_opts = {'nfw': {'truncated': False,
'projected_analytic': True,
'cumul2d_analytic': True},
'einasto': {},
'hernquist': {}}
self.halo_profile_model = ''
self.massdef = ''
self.delta_mdef = 0
self.hdpm = None
self.MDelta = 0.0
self.set_cosmo_params_dict ({})
self.set_halo_density_profile (halo_profile_model, massdef, delta_mdef)if not massdef in self.mdef_dict:
raise ValueError (f"Halo density profile mass definition {massdef} not currently supported")
# Check if we have already an instance of the required object, if not create one
if not ((halo_profile_model == self.halo_profile_model) and (massdef == self.massdef) and (delta_mdef == self.delta_mdef)):
self.halo_profile_model = halo_profile_model
self.massdef = massdef
cur_cdelta = 0.0
cur_mdelta = 0.0
cur_values = False
if self.hdpm:
cur_cdelta = self.conc.c
cur_values = True
self.mdef = ccl.halos.MassDef (delta_mdef, self.mdef_dict[massdef])
self.conc = ccl.halos.ConcentrationConstant (self.mdef)
self.mdef.concentration = self.conc
self.hdpm = self.hdpm_dict[halo_profile_model] (self.conc, **self.hdpm_opts[halo_profile_model])
if cur_values:
self.conc.c = cur_cdeltapyccl
Library of validated cosmological functions.
