def RhoNorm(self, Mvir):
'''
Return the normaliztion for mass function
'''
lnmarr = np.linspace(np.log(Mvir * 0.99), np.log(Mvir * 1.01), 10)
marr = np.exp(lnmarr).astype(np.float64)
cosmo0 = CosmologyFunctions(0, config_file, cosmo_dict)
#Byt giving m * h to sigm_m gives the sigma_m at z=0
sigma_m0 = np.array([cosmo0.sigma_m(m * cosmo0._h) for m in marr])
rho_norm = cosmo0.rho_bar()
lnMassSigmaSpl = InterpolatedUnivariateSpline(lnmarr, sigma_m0)
return rho_norm, lnMassSigmaSpl
def bias_mass_func_bocquet(redshift,
config_file,
cosmo_dict,
lM200,
uM200,
mspace,
bias=True,
Delta=200,
mtune=False,
marr=None):
'''
Wrote on Feb 20, 2017
Mass function of mass determined from critical density
of the Universe
redshift : Redshift of mass function
lM200 : Lower limit of M200c, i.e. critical M200
uM200 : Upper limit of M200c
mspace : mass space
bias : if weighted by ST bias (Doesn't work now)
M200 -solar unit/h
Both the output have no little h
mass function in dn/dlnM200 in 1/Mpc^3
marr solar unit/h
'''
cosmo0 = CosmologyFunctions(0, config_file, cosmo_dict)
cosmo_h = cosmo0._h
g0 = 3.54e-2 + cosmo0._omega_m0**0.09
g1 = 4.56e-2 + 2.68e-2 / cosmo0._omega_m0
g2 = 0.721 + 3.50e-2 / cosmo0._omega_m0
g3 = 0.628 + 0.164 / cosmo0._omega_m0
d0 = -1.67e-2 + 2.18e-2 * cosmo0._omega_m0
d1 = 6.52e-3 - 6.86e-3 * cosmo0._omega_m0
dd = d0 + d1 * redshift
gg = g0 + g1 * np.exp(-1. * ((g2 - redshift) / g3)**2.)
if mtune:
lnmarr = np.linspace(np.log(lM200), np.log(1e13), 30)
marr13 = np.exp(lnmarr).astype(np.float64)
marr14 = np.linspace(2e13, 1e14, 10)
marr15 = np.linspace(1.1e14, 1e15, 30)
#marr16 = np.linspace(1.2e15, 1e16, 30)
marr16 = np.linspace(1.1e15, 1e16, 30)
#marr17 = np.linspace(2**16, 10**17, 10)
marr = np.hstack([marr13, marr14, marr15, marr16])
lnmarr = np.log(marr)
elif marr is not None:
marr = marr / cosmo_h
lnmarr = np.log(marr)
else:
dlnm = np.float64(np.log(uM200 / lM200) / mspace)
lnmarr = np.linspace(np.log(lM200), np.log(uM200), mspace)
marr = np.exp(lnmarr).astype(np.float64)
#print('dlnm ', dlnm
#No little h
#Mass is in the unit of Solar/h and get the sigma without little h
sigma_m0 = np.array([cosmo0.sigma_m(m * cosmo_h) for m in marr])
rho_norm0 = cosmo0.rho_bar()
#print(marr, sigma_m0
cosmo = CosmologyFunctions(redshift, config_file, cosmo_dict)
lnMassSigmaSpl = InterpolatedUnivariateSpline(lnmarr,
sigma_m0 * cosmo._growth,
k=3)
if Delta == 200:
A = 0.222 * (1. + cosmo.redshift())**0.269
a = 1.71 * (1. + cosmo.redshift())**0.321
b = 2.24 * (1. + cosmo.redshift())**-0.621
c = 1.46 * (1. + cosmo.redshift())**-0.153
if Delta == 500:
raise Exception('Not implemeted')
A = 0.241 * (1. + cosmo.redshift())**0.370
a = 2.18 * (1. + cosmo.redshift())**0.251
b = 2.35 * (1. + cosmo.redshift())**-0.698
c = 2.02 * (1. + cosmo.redshift())**-0.310
mf, sarr, fsarr = [], [], []
for M200 in marr:
M1dM = gg + dd * np.log(M200)
mlow = M200 * 0.99
mhigh = M200 * 1.01
slow = lnMassSigmaSpl(np.log(mlow))
shigh = lnMassSigmaSpl(np.log(mhigh))
ds_dm = (shigh - slow) / (mhigh - mlow)
sigma = lnMassSigmaSpl(np.log(M200))
#print('%.2e %.2f %.2e'%(M200, sigma, ds_dm)
fsigma = A * np.exp(-c / sigma**2.) * ((sigma / b)**-a + 1.)
#print('%.2e %.2e %.2f %.2f %.2f %.2f %.2f'%(M200, fsigma, A, a, b, c, sigma)
mf.append(-1 * M1dM * fsigma * rho_norm0 * cosmo._h * cosmo._h *
ds_dm / sigma)
##mf.append(-1 * fsigma * rho_norm0 * ds_dm / sigma) #if need h^2/Mpc^3
sarr.append(sigma)
fsarr.append(fsigma)
mf = np.array(mf)
sarr = np.array(sarr)
fsarr = np.array(fsarr)
if 0:
return marr, mass_function * halo_bias_st(
delta_c_sigma_m2), sigma, fsigma
else:
return marr, mf, sarr, fsarr
def bias_mass_func_tinker(redshift,
config_file,
cosmo_dict,
lM,
uM,
mspace,
bias=True,
Delta=200,
mtune=False,
marr=None,
reduced=False):
'''
Wrote on Jan 26, 2017
Mass function of mass determined from mean density
of the Universe (i.e. omega_m(z) critical density)
redshift : Redshift of mass function
lM : Lower limit of marr
uM : Upper limit of marr
mspace : mass space
bias : if weighted by ST bias (Doesn't work now)
marr : Solar mass/h
M200 -solar unit/h
Both the output have no little h
mass function in dn/dlnM200 in 1/Mpc^3
marr solar unit / h
'''
DeltaTinker = np.log(
(200., 300., 400., 600., 800., 1200., 1600., 2400., 3200.))
# A
ATinker = (1.858659e-01, 1.995973e-01, 2.115659e-01, 2.184113e-01,
2.480968e-01, 2.546053e-01, 2.600000e-01, 2.600000e-01,
2.600000e-01)
Aspl = interp1d(DeltaTinker, ATinker,
kind='cubic') #fill_value='extrapolate')
# a
aTinker = (1.466904e+00, 1.521782e+00, 1.559186e+00, 1.614585e+00,
1.869936e+00, 2.128056e+00, 2.301275e+00, 2.529241e+00,
2.661983e+00)
aspl = interp1d(DeltaTinker, aTinker,
kind='cubic') #fill_value='extrapolate')
# b
bTinker = (2.571104e+00, 2.254217e+00, 2.048674e+00, 1.869559e+00,
1.588649e+00, 1.507134e+00, 1.464374e+00, 1.436827e+00,
1.405210e+00)
bspl = interp1d(DeltaTinker, bTinker,
kind='cubic') #fill_value='extrapolate')
# c
cTinker = (1.193958e+00, 1.270316e+00, 1.335191e+00, 1.446266e+00,
1.581345e+00, 1.795050e+00, 1.965613e+00, 2.237466e+00,
2.439729e+00)
cspl = interp1d(DeltaTinker, cTinker,
kind='cubic') #fill_value='extrapolate')
cosmo0 = CosmologyFunctions(0, config_file, cosmo_dict)
cosmo_h = cosmo0._h
if mtune:
lnmarr = np.linspace(np.log(lM), np.log(1e13), 30)
marr13 = np.exp(lnmarr).astype(np.float64)
marr14 = np.linspace(2e13, 1e14, 10)
marr15 = np.linspace(1.1e14, 1e15, 30)
#marr16 = np.linspace(1.2e15, 1e16, 30)
marr16 = np.linspace(1.1e15, 1e16, 30)
#marr17 = np.linspace(2**16, 10**17, 10)
marr = np.hstack([marr13, marr14, marr15, marr16])
lnmarr = np.log(marr)
elif marr is not None:
lnmarr = np.log(marr)
else:
dlnm = np.float64(np.log(uM / lM) / mspace)
lnmarr = np.linspace(np.log(lM), np.log(uM), mspace)
marr = np.exp(lnmarr).astype(np.float64)
#print('dlnm ', dlnm
#Should give mass in Msun/h to sigma_m() in CosmologyFunctions.py.
#See the note in that function
sigma_m0 = np.array([cosmo0.sigma_m(m) for m in marr])
rho_norm0 = cosmo0.rho_bar()
#print(marr, sigma_m0
if redshift >= 3:
cosmo = CosmologyFunctions(3., config_file, cosmo_dict)
else:
cosmo = CosmologyFunctions(redshift, config_file, cosmo_dict)
lnMassSigmaSpl = InterpolatedUnivariateSpline(lnmarr,
sigma_m0 * cosmo._growth,
k=3)
if 0: #Delta == 200:
A = 0.186 * (1. + cosmo.redshift())**-0.14
a = 1.47 * (1. + cosmo.redshift())**-0.06
alpha = 10**(-(0.75 / np.log10(200. / 75.))**1.2)
b = 2.57 * (1. + cosmo.redshift())**-alpha
c = 1.19
if 0: #Delta == 400:
A = 0.212 * (1. + cosmo.redshift())**-0.14
a = 1.56 * (1. + cosmo.redshift())**-0.06
alpha = 10**(-(0.75 / np.log10(400. / 75.))**1.2)
b = 2.05 * (1. + cosmo.redshift())**-alpha
c = 1.34
if Delta > 0:
A = Aspl(np.log(Delta))
a = aspl(np.log(Delta))
b = bspl(np.log(Delta))
c = cspl(np.log(Delta))
else:
A = 0.1 * np.log10(Delta) - 0.05
a = 1.43 + (np.log10(Delta) - 2.3)**1.5
b = 1.0 + (np.log10(Delta) - 1.6)**-1.5
c = 1.2 + (np.log10(Delta) - 2.35)**1.6
alpha = 10**(-(0.75 / np.log10(Delta / 75.))**1.2)
mf, sarr, fsarr = [], [], []
for tm in marr:
mlow = tm * 0.99
mhigh = tm * 1.01
slow = lnMassSigmaSpl(np.log(mlow))
shigh = lnMassSigmaSpl(np.log(mhigh))
ds_dm = (shigh - slow) / (mhigh - mlow) #this will have one h
sigma = lnMassSigmaSpl(np.log(tm))
#print('%.2e %.2f %.2e'%(tm, sigma, ds_dm)
fsigma = A * np.exp(-c / sigma**2.) * ((sigma / b)**-a + 1.)
#print('%.2e %.2e %.2f %.2f %.2f %.2f %.2f'%(tm, fsigma, A, a, b, c, sigma)
if reduced:
mf.append(-1 * fsigma * rho_norm0 * ds_dm /
sigma) #if need h^2/Mpc^3
else:
mf.append(
-1 * fsigma * rho_norm0 * cosmo._h**3 * ds_dm / sigma
) #It will have h^3/Mpc^3 if the dn/dlnM has M in Msol unit
sarr.append(sigma)
fsarr.append(fsigma)
mf = np.array(mf)
sarr = np.array(sarr)
fsarr = np.array(fsarr)
if 0:
return marr, mass_function * halo_bias_st(
delta_c_sigma_m2), sigma, fsigma
else:
return marr, mf, sarr, fsarr
def bias_mass_func_st(redshift,
config_file,
cosmo_dict,
lMvir,
uMvir,
mspace,
bias=True,
marr=None):
'''
Sheth & Torman 1999 & Eq. 56-50 of CS02 in p21
Output:
MF = dn/dlnMvir (1/Mpc^3)
mass = Solar mass
'''
cosmo0 = CosmologyFunctions(0, config_file, cosmo_dict)
cosmo_h = cosmo0._h
if marr is not None:
lnmarr = np.log(marr)
else:
dlnm = np.float64(np.log(uMvir / lMvir) / mspace)
lnmarr = np.linspace(np.log(lMvir), np.log(uMvir), mspace)
marr = np.exp(lnmarr).astype(np.float64)
#print('dlnm ', dlnm
#No little h
#Need to give mass * h and get the sigma without little h
sigma_m0 = np.array([cosmo0.sigma_m(m * cosmo0._h) for m in marr])
rho_norm0 = cosmo0.rho_bar()
#print(marr, sigma_m0
lnMassSigma0Spl = InterpolatedUnivariateSpline(lnmarr, sigma_m0, k=3)
cosmo = CosmologyFunctions(redshift, config_file, cosmo_dict)
mf, nuarr, fnuarr = [], [], []
for m in marr:
mlow = m * 0.99
mhigh = m * 1.01
mass_array = np.logspace(np.log10(mlow), np.log10(mhigh), 2)
ln_mass_array = np.log(mass_array)
ln_sigma_m_array = np.log(
np.array([lnMassSigma0Spl(np.log(m1)) for m1 in mass_array]))
#Derivatives of dln_nu/dln_mass at ln_mass
lnSigma_m_lnM_derivative = abs(
(ln_sigma_m_array[1] - ln_sigma_m_array[0]) /
(ln_mass_array[1] - ln_mass_array[0])) #1 for first derivate
nu = cosmo.nu_m(m)
#This is (delta_c/sigma(m))^2. Here delta_c is slightly dependence on
#Omega_m across redshift. cosmo._growth is the growth fucntion
#This means delta_c increases as a function of redshift
#lnMassSigmaSpl returns the sigma(m) at z=0 when gives the log(Mvir)
delta_c_sigma_m2 = cosmo.delta_c(
) * cosmo.delta_c() / cosmo._growth / cosmo._growth / lnMassSigma0Spl(
np.log(m)) / lnMassSigma0Spl(np.log(m))
nu_d = 0.707 * delta_c_sigma_m2
nuf_1 = (1. + 1. / nu_d**0.3)
nuf_2 = (2. * nu_d)**0.5
nuf_3 = np.exp(-nu_d / 2.) / np.sqrt(np.pi)
nuf = 0.322 * nuf_1 * nuf_2 * nuf_3
if bias:
mf.append(
halo_bias_st(delta_c_sigma_m2) * nuf * rho_norm0 * cosmo._h *
cosmo._h * lnSigma_m_lnM_derivative / m)
else:
mf.append(nuf * rho_norm0 * cosmo._h * cosmo._h *
lnSigma_m_lnM_derivative / m)
mf = np.array(mf)
return marr, mf
def cl_WL_tSZ(config_file, cosmology, fwhm_k, fwhm_y, kk, yy, ky, zsfile,
P01, P02, P03, xc1, xc2, xc3, beta1, beta2, beta3,
omega_m0, sigma_8, odir, ofile):
'''
Compute WL X tSZ halomodel for a given source redshift distribution
'''
if ky:
sigma_k = fwhm_k * np.pi / 2.355 / 60. /180. #angle in radian
sigma_y = fwhm_y * np.pi / 2.355 / 60. /180. #angle in radian
sigmasq = sigma_k * sigma_y
elif kk:
sigma_k = fwhm_k * np.pi / 2.355 / 60. /180. #angle in radian
sigmasq = sigma_k * sigma_k
elif yy:
sigma_y = fwhm_y * np.pi / 2.355 / 60. /180. #angle in radian
sigmasq = sigma_y * sigma_y
else:
raise ValueError('Either kk, yy or ky should be True')
config = ConfigParser()
config.read(config_file)
if omega_m0 is None:
omega_m0 = config.getfloat(cosmology, 'omega_m0')
if sigma_8 is None:
sigma_8 = config.getfloat(cosmology, 'sigma_8')
omega_l0 = 1. - omega_m0
omega_b0 = config.getfloat(cosmology, 'omega_b0')
h = config.getfloat(cosmology, 'h')
n_scalar = config.getfloat(cosmology, 'n_scalar')
cosmo_dict = {'omega_m0':omega_m0, 'omega_l0':omega_l0, 'omega_b0':omega_b0, 'h':h, 'sigma_8':sigma_8, 'n_scalar':n_scalar}
cosmo0 = CosmologyFunctions(0, config_file, cosmo_dict)
cosmo_h = cosmo0._h
save_clfile = config.getboolean('halomodel', 'save_clfile')
print_cl = config.getboolean('halomodel', 'print_cl')
light_speed = config.getfloat('halomodel', 'light_speed') #km/s
mpctocm = config.getfloat('halomodel', 'mpctocm')
kB_kev_K = config.getfloat('halomodel', 'kB_kev_K')
sigma_t_cm = config.getfloat('halomodel', 'sigma_t_cm') #cm^2
rest_electron_kev = config.getfloat('halomodel', 'rest_electron_kev') #keV
constk = 3. * omega_m0 * (cosmo_h * 100. / light_speed)**2. / 2. #Mpc^-2
consty = mpctocm * sigma_t_cm / rest_electron_kev
zsarr, Ns = np.genfromtxt(zsfile, unpack=True)
if np.isscalar(zsarr):
zsarr = np.array([zsarr])
Ns = np.array([Ns])
else:
zint = np.sum(Ns) * (zsarr[1] - zsarr[0])
Ns /= zint
if P01 is None:
P01 = config.getfloat('halomodel', 'P01')
if P02 is None:
P02 = config.getfloat('halomodel', 'P02')
if P03 is None:
P03 = config.getfloat('halomodel', 'P03')
if xc1 is None:
xc1 = config.getfloat('halomodel', 'xc1')
if xc2 is None:
xc2 = config.getfloat('halomodel', 'xc2')
if xc3 is None:
xc3 = config.getfloat('halomodel', 'xc3')
if beta1 is None:
beta1 = config.getfloat('halomodel', 'beta1')
if beta2 is None:
beta2 = config.getfloat('halomodel', 'beta2')
if beta3 is None:
beta3 = config.getfloat('halomodel', 'beta3')
kRmax = config.getfloat('halomodel', 'kRmax')
kRspace = config.getint('halomodel', 'kRspace')
yRmax = config.getfloat('halomodel', 'yRmax')
yRspace = config.getint('halomodel', 'yRspace')
kmin = config.getfloat('halomodel', 'kmin') #1/Mpc
kmax = config.getfloat('halomodel', 'kmax')
kspace = config.getint('halomodel', 'kspace')
ellmin = config.getint('halomodel', 'ellmin')
ellmax = config.getfloat('halomodel', 'ellmax')
ellspace = config.getint('halomodel', 'ellspace')
mmin = config.getfloat('halomodel', 'mmin')
mmax = config.getfloat('halomodel', 'mmax')
mspace = config.getfloat('halomodel', 'mspace')
zmin = config.getfloat('halomodel', 'zmin')
zmax = config.getfloat('halomodel', 'zmax')
zspace = config.getfloat('halomodel', 'zspace')
dlnk = np.log(kmax/kmin) / kspace
lnkarr = np.linspace(np.log(kmin), np.log(kmax), kspace)
karr = np.exp(lnkarr).astype(np.float64)
#No little h
#Input Mpc/h to power spectra and get Mpc^3/h^3
pk_arr = np.array([cosmo0.linear_power(k/cosmo0._h) for k in karr]).astype(np.float64) / cosmo0._h / cosmo0._h / cosmo0._h
#np.savetxt('pk_vinu.dat', np.transpose((karr/cosmo0._h, pk_arr*cosmo0._h**3)))
#sys.exit()
#kc, pkc = np.genfromtxt('matterpower.dat', unpack=True)
#pkspl = InterpolatedUnivariateSpline(kc, pkc, k=2)
#pkh_arr = pkspl(karr/cosmo0._h)
#pk_arr = pkh_arr / cosmo0._h / cosmo0._h / cosmo0._h
pkspl = InterpolatedUnivariateSpline(karr, pk_arr, k=2)
#pl.loglog(karr, pk_arr)
#pl.show()
dlnm = np.log(mmax/mmin) / mspace
lnmarr = np.linspace(np.log(mmin), np.log(mmax), mspace)
marr = np.exp(lnmarr).astype(np.float64)
lnzarr = np.linspace(np.log(1.+zmin), np.log(1.+zmax), zspace)
zarr = np.exp(lnzarr) - 1.0
dlnz = np.log((1.+zmax)/(1.+zmin)) / zspace
print('dlnk, dlnm dlnz', dlnk, dlnm, dlnz)
if doPrintCl:
print('dlnk, dlnm dlnz', dlnk, dlnm, dlnz)
#No little h
#Need to give mass * h and get the sigma without little h
#The following lines are used only used for ST MF and ST bias
sigma_m0 = np.array([cosmo0.sigma_m(m * cosmo0._h) for m in marr])
rho_norm0 = cosmo0.rho_bar()
lnMassSigmaSpl = InterpolatedUnivariateSpline(lnmarr, sigma_m0, k=3)
hzarr, BDarr, rhobarr, chiarr, dVdzdOm, rho_crit_arr = [], [], [], [], [], []
bias, bias_t, Darr = [], [], []
marr2, mf, dlnmdlnm, Deltaarr = [], [], [], []
if config.get('halomodel', 'MF') == 'Tinker' and config.get('halomodel', 'MassToIntegrate') == 'm200m':
#Mass using critical density (ie. m200c)
tm200c = np.logspace(np.log10(1e8), np.log10(1e17), 50)
#m200m mass using mean mass density
tmarr = np.exp(lnmarr).astype(np.float64)
#tf = np.genfromtxt('../data/z_m_relation.dat')
#tz = tf[:,0]
#tmv = tf[:,1]
#tm200c = tf[:,2]
#tm200m = tf[:,3]
for i, zi in enumerate(zarr):
cosmo = CosmologyFunctions(zi, config_file, cosmo_dict)
rcrit = cosmo.rho_crit() * cosmo._h * cosmo._h
rbar = cosmo.rho_bar() * cosmo._h * cosmo._h
bn = cosmo.BryanDelta()
BDarr.append(bn) #OK
rho_crit_arr.append(rcrit) #OK
rhobarr.append(rbar)
chiarr.append(cosmo.comoving_distance() / cosmo._h)
hzarr.append(cosmo.E0(zi))
DD = bn/cosmo.omega_m()
DD200 = 200./cosmo.omega_m()
#Number of Msun objects/Mpc^3 (i.e. unit is 1/Mpc^3)
if config.get('halomodel', 'MF') == 'Tinker':
if config.get('halomodel', 'MassToIntegrate') == 'virial':
if DD > 200:
mFrac = marr * cosmo_h
print(1)
mFrac = marr * h0
#print bn, cosmo.omega_m(), bn/cosmo.omega_m()
mf.append(bias_mass_func_tinker(zi, config_file, cosmo_dict, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=DD, marr=mFrac, reduced=False)[1])
marr2.append(marr)
dlnmdlnm.append(np.ones_like(marr))
else:
mFrac = np.array([HuKravtsov(zi, mv, rcrit, bn, config.getfloat('halomodel', 'MassDef') * cosmo.omega_m(), cosmo_h, 1)[2] for mv in marr]) * cosmo_h
mf.append(bias_mass_func_tinker(zi, config_file, cosmo_dict, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=config.getfloat('halomodel', 'MassDef'), marr=mFrac, reduced=False)[1])
marr2.append(marr)
dlnmdlnm.append([dlnMdensitydlnMcritOR200(config.getfloat('halomodel', 'MassDef') * cosmo.omega_m(), bn, mFm/cosmo_h, mv, zi, cosmo_h, 1) for mv,mFm in zip(marr, mFrac)]) #dlnmFrac/dlnMv. In the bias_mass_func_tinker() I have computed dn/dlnM where M is in the unit of Msol. I have therefore include h in that mass function. Therefore, I just need to multiply dlnmFrac/dlnMv only
print(2)
mFrac = np.array([HuKravtsov(zi, mv, rcrit, bn, float(config['massfunc']['MassDef'])/cosmo.omega_m(), h0, 1)[2] for mv in marr]) * h0
mf.append(bias_mass_func_tinker(zi, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=float(config['massfunc']['MassDef']), marr=mFrac, reduced=False)[1])
marr2.append(marr)
dlnmdlnm.append([dlnMdensitydlnMcritOR200(float(config['massfunc']['MassDef']) / cosmo.omega_m(), bn, mFm/h0, mv, zi, h0, 1) for mv,mFm in zip(marr, mFrac)]) #dlnmFrac/dlnMv. In the bias_mass_func_tinker() I have computed dn/dlnM where M is in the unit of Msol. I have therefore include h in that mass function. Therefore, I just need to multiply dlnmFrac/dlnMv only
#print dlnmdlnm
#print a
input_mvir = 1
elif config.get('halomodel', 'MassToIntegrate') == 'm200c':
#XXX
#m200m = np.array([HuKravtsov(zi, mv, rcrit, 200, 200*cosmo.omega_m(), cosmo_h, 0)[2] for mv in marr]) #* cosmo_h
#print m200m
#XXX
if DD200 > 200:
mFrac = marr * cosmo_h
#print 200, cosmo.omega_m(), 200/cosmo.omega_m()
mf.append(bias_mass_func_tinker(zi, config_file, cosmo_dict, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=DD200, marr=mFrac, reduced=False)[1])
marr2.append(marr)
dlnmdlnm.append(np.ones_like(marr))
else:
mFrac = np.array([HuKravtsov(zi, m2c, rcrit, 200, config.getfloat('halomodel', 'MassDef') * cosmo.omega_m(), cosmo_h, 0)[2] for m2c in marr]) * cosmo_h
mf.append(bias_mass_func_tinker(zi, config_file, cosmo_dict, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=config.getfloat('halomodel', 'MassDef'), marr=mFrac)[1])
marr2.append(marr)
for m2,mFm in zip(marr, mFrac):
dlnmdlnm.append(dlnMdensitydlnMcritOR200(config.getfloat('halomodel', 'MassDef') * cosmo.omega_m(), 200., mFm/cosmo_h, m2, zi, cosmo_h, 0)) #dlnM200m/dlnMv. In the bias_mass_func_tinker() I have computed dn/dlnM where M is in the unit of Msol. I have therefore include h in that mass function. Therefore, I just need to multiply dlnM200m/dlnMv only
mFrac = np.array([HuKravtsov(zi, m2c, rcrit, 200, float(config['massfunc']['MassDef'])/cosmo.omega_m(), h0, 0)[2] for m2c in marr]) * h0
mf.append(bias_mass_func_tinker(zi, mFrac.min(), mFrac.max(), mspace, bias=False, Delta=float(config['massfunc']['MassDef']), marr=mFrac)[1])
marr2.append(marr)
for m2,mFm in zip(marr, mFrac):
dlnmdlnm.append(dlnMdensitydlnMcritOR200(float(config['massfunc']['MassDef']) / cosmo.omega_m(), 200., mFm/h0, m2, zi, h0, 0)) #dlnM200m/dlnMv. In the bias_mass_func_tinker() I have computed dn/dlnM where M is in the unit of Msol. I have therefore include h in that mass function. Therefore, I just need to multiply dlnM200m/dlnMv only
input_mvir = 0
elif config.get('halomodel', 'MassToIntegrate') == 'm200m':
#raise ValueError('Use MassToIntegrate=virial/m200c. m200m is not working')
#Temporary mass array of m200m from m200c
tm200m = np.array([HuKravtsov(zi, tt, rcrit, 200, 200.*cosmo.omega_m(), cosmo._h, 0)[2] for tt in tm200c])
#m200m vs m200c spline
tmspl = InterpolatedUnivariateSpline(tm200m, tm200c)
#Now m200c from m200m, i.e. tmarr which is the integrating
#variable
m200c = tmspl(tmarr)
#m200m Msol/h
m200m = tmarr * cosmo_h
marr2.append(m200c)
mf.append(bias_mass_func_tinker(zi, config_file, cosmo_dict, m200m.min(), m200m.max(), mspace, bias=False, Delta=200, marr=m200m)[1])
input_mvir = 0
elif config.get('halomodel', 'MF') == 'Bocquet':
if config.get('halomodel', 'MassToIntegrate') == 'virial':
m200 = np.array([HuKravtsov(zi, mv, rcrit, bn, 200, cosmo_h, 1)[2] for mv in marr])
mf.append(bias_mass_func_bocquet(zi, config_file, cosmo_dict, m200.min(), m200.max(), mspace, bias=False, marr=m200)[1])
marr2.append(marr)
for mv,m2 in zip(marr, m200):
dlnmdlnm.append(dlnMdensitydlnMcritOR200(200., bn, m2, mv, zi, cosmo_h, 1))
input_mvir = 1
elif config.get('halomodel', 'MassToIntegrate') == 'm200':
tmf = bias_mass_func_bocquet(zi, config_file, cosmo_dict, marr.min(), marr.max(), mspace, bias=False, marr=marr)[1]
mf.append(tmf)
dlnmdlnm.append(np.ones(len(tmf)))
input_mvir = 0
elif config.get('halomodel', 'MF') == 'ST':
mf.append(bias_mass_func_st(zi, config_file, cosmo_dict, marr.min(), marr.max(), mspace, bias=False, marr=marr)[1])
marr2.append(marr)
dlnmdlnm.append(np.ones_like(marr))
input_mvir = 1
#raise ValueError('MF should be Tinker or Bocquet')
#Bias is calculated by assuming that the mass is virial. I need to change that
#print DD
#for m in marr:
# print '%.2e T %.2f'%(m, halo_bias_tinker(DD, cosmo.delta_c() / cosmo._growth / lnMassSigmaSpl(np.log(m))))
# print '%.2e ST %.2f'%(m, halo_bias_st(cosmo.delta_c() * cosmo.delta_c() / cosmo._growth / cosmo._growth / lnMassSigmaSpl(np.log(m)) / lnMassSigmaSpl(np.log(m))))
#sys.exit()
if config.get('halomodel', 'MF') == 'Tinker':
if DD >= 200:
bias.append(np.array([halo_bias_tinker(DD, cosmo.delta_c() / cosmo._growth / lnMassSigmaSpl(np.log(m))) for m in marr]))
else:
bias.append(np.array([halo_bias_tinker(config.getfloat('halomodel', 'MassDef') * cosmo.omega_m(), cosmo.delta_c() / cosmo._growth / lnMassSigmaSpl(np.log(m))) for m in mFrac/cosmo_h]))
elif config.get('halomodel', 'MF') == 'ST' or config.get('halomodel', 'MF') == 'Bocquet':
bias.append(np.array([halo_bias_st(cosmo.delta_c() * cosmo.delta_c() / cosmo._growth / cosmo._growth / lnMassSigmaSpl(np.log(m)) / lnMassSigmaSpl(np.log(m))) for m in marr]))
dVdzdOm.append(cosmo.E(zi) / cosmo._h) #Mpc/h, It should have (km/s/Mpc)^-1 but in the cosmology code the speed of light is removed
Darr.append(cosmo._growth)
#pl.title('%.2f'%zi)
#pl.scatter(np.array([halo_bias_st(cosmo.delta_c() * cosmo.delta_c() / cosmo._growth / cosmo._growth / lnMassSigmaSpl(np.log(m)) / lnMassSigmaSpl(np.log(m))) for m in marr]), np.array([halo_bias_tinker(200, cosmo.delta_c() / cosmo._growth / lnMassSigmaSpl(np.log(m))) for m in marr]))
#pl.show()
if config.get('halomodel', 'MF') =='Tinker' and config.get('halomodel', 'MassToIntegrate') == 'm200m':
mf = np.array(mf).flatten()
else:
mf = np.array(mf).flatten() * np.array(dlnmdlnm).flatten()
hzarr = np.array(hzarr)
BDarr = np.array(BDarr)
rhobarr = np.array(rhobarr)
chiarr = np.array(chiarr)
dVdzdOm = np.array(dVdzdOm) * chiarr * chiarr
rho_crit_arr = np.array(rho_crit_arr)
marr2 = np.array(marr2).flatten()
zchispl = InterpolatedUnivariateSpline(zarr, chiarr, k=2)
chisarr = zchispl(zsarr)
bias = np.array(bias).flatten()
bias_t = np.array(bias_t).flatten()
Darr = np.array(Darr)
#ellarr = np.linspace(1, 10001, 10)
ellarr = np.logspace(np.log10(ellmin), np.log10(ellmax), ellspace)
cl_arr, cl1h_arr, cl2h_arr = [], [], []
for ell in ellarr:
pk = pkspl(ell/chiarr)
if ky:
cl1h, cl2h, cl = integrate_kyhalo(ell, lnzarr, chiarr, dVdzdOm, marr2, mf, BDarr, rhobarr, rho_crit_arr, bias, Darr, pk, zsarr, chisarr, Ns, dlnz, dlnm, omega_b0, omega_m0, cosmo_h, constk, consty, input_mvir, mspace, kRmax, kRspace, yRmax, yRspace, P01, P02, P03, xc1, xc2, xc3, beta1, beta2, beta3)
if kk:
cl1h, cl2h, cl = integrate_kkhalo(ell, lnzarr, chiarr, dVdzdOm, marr2, mf, BDarr, rhobarr, rho_crit_arr, bias, Darr, pk, zsarr, chisarr, Ns, dlnz, dlnm, omega_b0, omega_m0, cosmo_h, constk, consty, input_mvir, mspace, kRmax, kRspace)
if yy:
cl1h, cl2h, cl = integrate_yyhalo(ell, lnzarr, chiarr, dVdzdOm, marr2, mf, BDarr, rhobarr, rho_crit_arr, bias, Darr, pk, dlnz, dlnm, omega_b0, omega_m0, cosmo_h, constk, consty, input_mvir, mspace, yRmax, yRspace, P01, P02, P03, xc1, xc2, xc3, beta1, beta2, beta3)
cl_arr.append(cl)
cl1h_arr.append(cl1h)
cl2h_arr.append(cl2h)
if print_cl:
print('l %.2 Cl_1h %.2e Cl_2h %.2e Cl %.2e'%(ell, cl1h, cl2h, cl))
if doPrintCl:
print(ell, cl1h, cl2h, cl)
convolve = np.exp(-1 * sigmasq * ellarr * ellarr)# i.e. the output is Cl by convolving by exp(-sigma^2 l^2)
cl = np.array(cl_arr) * convolve
cl1h = np.array(cl1h_arr) * convolve
cl2h = np.array(cl2h_arr) * convolve
if save_clfile:
np.savetxt(os.path.join(odir, ofile), np.transpose((ellarr, cl1h, cl2h, cl)), fmt='%.2f %.3e %.3e %.3e', header='l Cl1h Cl2h Cl')
return ellarr, cl1h, cl2h, cl
x = (a1 * f**(2. * p) + 0.75**2.)**(-0.5) + 2. * f
Mfrac = M * Delta * (1. / conc / x)**3
Rfrac = (3. * Mfrac / deltao / rho / 4. / np.pi)**(1. / 3.)
return M, R, Mfrac, Rfrac, rho_s, Rs
if __name__ == '__main__':
z = 0.07
Mvir = 1e15
cosmo = CosmologyFunctions(z, 'wlsz.ini', 'battaglia')
omega_b = cosmo._omega_b0
omega_m = cosmo._omega_m0
cosmo_h = cosmo._h
BryanDelta = cosmo.BryanDelta()
rho_critical = cosmo.rho_crit() * cosmo._h * cosmo._h
rho_bar = cosmo.rho_bar() * cosmo._h * cosmo._h
for D in np.arange(1, 100, 10):
M, R, Mfrac, Rfrac, rho_s, Rs = HuKravtsov(z, Mvir, rho_critical,
BryanDelta,
D * cosmo.omega_m(),
cosmo_h, True)
print('%.2e %.2f %.2e %.2f %.2e %.2f' %
(M, R, Mfrac, Rfrac, rho_s, Rs))
sys.exit()
print('rho_critical = %.2e , rho_bar = %.2e' % (rho_critical, rho_bar))
print('Mvir, Rvir, Mfrac, Rfrac, rho_s, Rs')
Mvir, Rvir, Mfrac, Rfrac, rho_s, Rs = MvirToMRfrac(Mvir, z, BryanDelta,
rho_critical, cosmo_h)
print('%.2e %.2f %.2e %.2f %.2e %.2f' %
(Mvir, Rvir, Mfrac, Rfrac, rho_s, Rs))
Mvir, Rvir, Mfrac, Rfrac, rho_s, Rs = MfracToMvir(Mfrac,