def init(chain_index=None):
if args.cosmo_prior:
Hp = Planck15.H0.to(u.km / u.s / u.Mpc).value * Planck15.efunc(
true_params['z_p']) * (1 + 0.01 * randn())
Om = Planck15.Om0 * (1 + 0.01 * randn())
else:
Hp = Planck15.H0.to(u.km / u.s / u.Mpc).value * Planck15.efunc(
true_params['z_p']) * (1 + 0.1 * randn())
Om = Planck15.Om0 * (1 + 0.1 * randn())
w = -1 + 0.1 * randn()
c = cosmo.FlatwCDM(Hp / Planck15.efunc(true_params['z_p']), Om, w)
MMax_d_p = (45 + 5 * randn()) * (1 + cosmo.z_at_value(
c.luminosity_distance,
Planck15.luminosity_distance(true_params['z_p']).to(u.Gpc)))
smooth_max = 0.1 + 0.01 * randn()
MMax_d_p_2sigma = exp(log(MMax_d_p) + 2 * smooth_max)
alpha = 0.7 + 0.1 * randn()
beta = 0.1 * randn()
gamma = 3 + 0.1 * randn()
return {
'H_p': Hp,
'Om': Om,
'w0': w,
'MMax_d_p': MMax_d_p,
'MMax_d_p_2sigma': MMax_d_p_2sigma,
'alpha': alpha,
'beta': beta,
'gamma': gamma,
'xs': randn(nobs, 3)
}
def cl_z(self,
z=[],
l=np.arange(2000) + 1,
pk_params=None,
cosmo=None,
pk_func=None):
if not pk_func:
pk_func = self.class_pk
nz = len(z)
nl = len(l)
pk, kh = pk_func(z=z, pk_params=pk_params)
cls = np.zeros((nz, nl), dtype='float32') * u.Mpc**2
for i in np.arange(nz):
DC_i = cosmo.angular_diameter_distance(
z[i]).value #because camb k in h/mpc
lz = kh * DC_i - 0.5
pk_int = interp1d(lz,
pk[i] / DC_i**2,
bounds_error=False,
fill_value=0)
cls[i][:] += pk_int(l) * u.Mpc * (c /
(cosmo.efunc(z[i]) * cosmo.H0))
return cls
def sfr2_porciani_madau(z):
'''
SFR2 from porciani madau 2001
http://stacks.iop.org/0004-637X/548/i=2/a=522
'''
return exp(3.4 * z) / (exp(3.4 * z) + 22.) * Planck15.efunc(z) / (
(1 + z)**(3 / 2.))
def dL_df(z):
"""
Comoving differential distance at redshift per frequency.
[cMpc]/Hz, from Furlanetto et al. (2006)
"""
c_kms = c_ms / 1e3 # km/s
return c_kms / (cosmo.H0.value * cosmo.efunc(z)) * (z + 1)**2 / f21
from read_db import *#pairs, profile_array, color, plot_profile, profilelist, norms
from astropy.cosmology import Planck15
from astropy import constants
Ez = Planck15.efunc(zs)
Tmw = h.reverse_property_cascade('Tmw_tcut_profile')[0]
#Convert T to keV
Tmw *= constants.k_B.to('keV K**-1').value
rho_e_vol = np.array([rho*units.g/(units.cm**3) for rho in h.reverse_property_cascade('rho_e_vol_profile')[0]])
rho_g_vol = m_p*rho_e_vol*mu_e #g/cm^3
def entropy(T, rho_e):
return T/pow(rho_e, 2/3.)
Kmw = np.array([entropy(Tmw[elt]*units.keV, rho_g_vol[elt]/(m_p*units.g)) for elt in range(len(Tmw))])
Pmw = np.array([Tmw[elt]*units.keV*rho_g_vol[elt]/(m_p*units.g) for elt in range(len(Tmw))])
def K500_McCarthy08(r500_ind, cummass_profile_ind): #self-similar scaling
m500 = cummass_profile_ind[r500_ind] #check that this is in Msun
fb = 0.16
return 2561 * pow(m500/1e15, 2./3) * pow(fb/.13, -2./3) #keV cm^2
K500 = np.array([K500_McCarthy08(r500_ind(ind), cummass_profile[ind]) for ind in range(len(cummass_profile))])
T500 = np.array([pow(ne_500[ind], 2./3)*K500[ind] for ind in range(len(K500))]) #keV
P500 = ng_500*T500
cs = np.sqrt((T500s/(mu*constants.m_p)).to('kpc**2 yr**-2'))
bh = h['BH_central'][0]
def eta_to_kpar_fac(z):
return (2 * np.pi * Planck15.H0 * f21 * Planck15.efunc(z) /
(cnst.c * (1 + z)**2)).to(1 / un.Mpc).value
def dL_df(z, omega_m=0.266):
'''[Mpc]/Hz, from Furlanetto et al. (2006)'''
c_kms = 299792.458 #km/s
nu21 = 1420e6
return c_kms/(cosmo.H0.value * cosmo.efunc(z)) * (z+1)**2 / nu21
def dkpar_dkperp(z):
"""
Wedge line
"""
return (cosmo.H0.to("m/(s Mpc)").value * comoving_distance(z) *
cosmo.efunc(z) / (c_ms * (1 + z)))
