def shot_noise(nfn, nu, zs, mhalos, stellarmasses):
chis = remote_spectra.chifromz(zs)
Lcuts = Luminosity_from_flux(
Scut(nu),
zs) #Scut is in mJy=1e-29W/m**2/Hz. This Lcut will be in mJy Mpc**2
Lcuts = Lcuts * (3.086e22)**2 #now in mJy m**2 = 1e-29 W/Hz
Lcuts = Lcuts * 1e-29 #in W/Hz
Lcuts = Lcuts / 3.8e26 #insolarluminosities per hz
integrand = 1 / remote_spectra.chifromz(zs)**2 * 1 / (
1 + zs)**2 * shot_noise_chi_integral(nfn, nu, zs, Lcuts, mhalos,
stellarmasses)
#in 1/MPc**2*[shot_noise_chi_integral]=1/MPc**2*[stellar_mass_function]*L**2 = Mpc**-5*[L]**2=
#=Mpc**-5* [solar luminosity/Hz]**2
shot_noise = np.trapz(
integrand, chis
) #in MPc*[integrand]=1/Mpc*[shot_noise_chi_integral]=Mpc**-4*[L]**2=
if nu == 353:
changetomicrokelvinfactor = 1 * 1 / (287.45)
elif nu == 545:
changetomicrokelvinfactor = 1 * 1 / (58.04)
elif nu == 857:
changetomicrokelvinfactor = 1 * 1 / (2.27)
return shot_noise * changetomicrokelvinfactor**2
def survey_volume_mpc3(surveyarea_sqdeg, zmin, zmax):
chimax = remote_spectra.chifromz(zmax)
chimin = remote_spectra.chifromz(zmin)
svolume_mpc3 = 4. / 3. * np.pi * ((chimax)**3. - (chimin)**3.)
svolume_mpc3 *= (surveyarea_sqdeg / allsky_squaredeg)
print("Survey volume Gpc-3", svolume_mpc3 * 1e-9)
return svolume_mpc3
def convert_n_arcmin2_mpc3(n_arcmin2, z):
dz = 0.01
zmax = z + dz / 2.
zmin = z - dz / 2.
chimax = remote_spectra.chifromz(zmax)
chimin = remote_spectra.chifromz(zmin)
dV_shell_comov = 4. / 3. * np.pi * ((chimax)**3. - (chimin)**3.)
dV_dz = dV_shell_comov / dz
dV_dZdOmega = dV_dz / allsky_arcmin2
n_mpc3 = n_arcmin2 / dV_dZdOmega
return n_mpc3
def Scentral(nu, z, Mstar):
#flux from luminosity; eg eq 7 of 1611.04517
chi = remote_spectra.chifromz(z)
return Lnu(nu * (1 + z), z, Mstar) / (
(4 * np.pi) * chi**2 *
(1 + z)) # in units of [Lnu]/Mpc**2=solar_luminosity/Mpc**2/Hz
def Scentral(self,nu,z,Mhalo):
# flux from luminosity; eg eq 42 of https://arxiv.org/pdf/1309.0382.pdf
chi=remote_spectra.chifromz(z)
answer= self.Lnu(nu,z,Mhalo)/((4*np.pi)*chi**2*(1+z))
if self.L0!=1: # implementing Scut.
# Note that if you are playing with L0 you should remove this as if L0 is too high this will set all fluxes to 0.
answer[answer>self.Scut(nu)]=0
return answer
def Cl_1halo(self,nu1,nu2,intensities_nu1,intensities_nu2,satellites_nu1,satellites_nu2,ells):
# equation 13 of 1611.04517
chis=remote_spectra.chifromz(self.zs)
mhalos=np.exp(self.halomodel.lnms)
mhalos=mhalos[mhalos>self.Mmin]
Cl1_integrand=np.array([chis**2*self.Gnu(self.zs,ell/chis,chis,intensities_nu1,intensities_nu2,satellites_nu1,satellites_nu2)for ell in ells]) #in units of Mpc**2 [Gnu]
return np.trapz(Cl1_integrand[:,self.zs>0.1],chis[self.zs>0.1],axis=1)*conversion_factor
def shot_noise(self,freqind,sigma):
chis=remote_spectra.chifromz(self.zs)
centrals=self.central_intensities[freqind]
centrals[centrals==0]=1e-100
logcentrals=np.log(centrals)
dummylogs=np.linspace(np.min(logcentrals[logcentrals>-200])-0.5,self.Scut(self.frequencies[freqind]),200)
dnds=self.dndlns(dummylogs,logcentrals,sigma)
return np.trapz(chis**2*(np.trapz(dnds*np.exp(dummylogs[:,np.newaxis])**2,dummylogs,axis=0)),chis)
def setup_fluxes(self):
self.mhalos=np.exp(self.halomodel.lnms)
self.mhalos=self.mhalos[self.mhalos>self.Mmin]
self.central_intensities=[]
self.satellite_intensities=[]
self.chis=remote_spectra.chifromz(self.zs)
for frequency in self.frequencies:
self.central_intensities.append(self.Scentral(frequency,self.zs,self.mhalos[:,np.newaxis]))
self.satellite_intensities.append(self.satellite_intensity(frequency,self.zs,self.mhalos))
self.central_intensities.append(self.Scentral(frequency,self.zs,self.mhalos[:,np.newaxis]))
self.satellite_intensities.append(self.satellite_intensity(frequency,self.zs,self.mhalos))
def Cl_CIB_phi(self,nu,intensities,satellites,ells,Plin):
plin=np.zeros((len(ells),len(self.zs)))
chis=remote_spectra.chifromz(self.zs)
cls_CIBkappa=np.zeros(len(ells))
cls_CIBkappa_integrand=chis**2*self.Fnu(nu,intensities,satellites,chis,self.zs)*(self.lensing_kernel(chis))
for ell_index,ell in enumerate(ells):
plin[ell_index]=np.array([Plin(self.zs[i],ell/chis[i])for i in range(0,len(self.zs))] )
cls_CIBkappa[ell_index]=np.trapz(cls_CIBkappa_integrand*plin[ell_index],chis)/ell**2
return cls_CIBkappa*np.sqrt(conversion_factor)
def Cl_2halo(self,nu1,nu2,intensities_nu1,intensities_nu2,satellites_nu1,satellites_nu2,ells,Plin):
# equation 11 of 1611.04517
plin=np.zeros((len(ells),len(self.zs)))
chis=remote_spectra.chifromz(self.zs)
cls_2halo=np.zeros(len(ells))
if nu1==nu2:
Cl2_integrand=chis**2*self.Fnu(nu1,intensities_nu1,satellites_nu1,chis,self.zs)**2
else:
Cl2_integrand=chis**2*self.Fnu(nu1,intensities_nu1,satellites_nu1,chis,self.zs)*self.Fnu(nu2,intensities_nu2,satellites_nu2,chis,self.zs)
for ell_index,ell in enumerate(ells):
plin[ell_index]=np.array([Plin(self.zs[i],ell/chis[i])for i in range(0,len(self.zs))] )
cls_2halo[ell_index]=np.trapz(Cl2_integrand*(plin[ell_index]),chis)
return cls_2halo*conversion_factor
def Luminosity_from_flux(S, z):
#gives luminosity in [S] * Mpc**2
return 4 * np.pi * remote_spectra.chifromz(z)**2 * (1 + z) * S
def calc_Cl_CIBCIB(self):
print("Calculation Cl_CIBCIB, Cl_CIBtau, Cl_tautau...")
ell_sparse = np.arange(conf.estim_smallscale_lmin,
conf.estim_smallscale_lmax,
100) #we interpolate these spectra
integral_CIBCIB_1h = np.zeros(ell_sparse.shape[0])
integral_CIBCIB_2h = np.zeros(ell_sparse.shape[0])
zs = np.linspace(conf.z_min, conf.z_max, 100) #change this.
chi_sampling = remote_spectra.chifromz(zs)
for frequency_index in range(0, len(self.frequencies)):
zs = np.linspace(conf.z_min, conf.z_max, 100) #change this.
chi_sampling = remote_spectra.chifromz(zs)
frequency = self.frequencies[frequency_index]
for ell_id, ell in enumerate(ell_sparse):
#version 1. correct.
ks = (ell + (1. / 2.)) / chi_sampling
# integrand_chi_CIBtau = np.zeros( chi_sampling.shape[0] )
#limber approx
PCIBCIB_1h, PCIBCIB_2h = self.get_PCIBCIB(
ks, zs, frequency_index)
if frequency == 353:
changetomicrokelvinfactor = 1 / (287.45)
elif frequency == 545:
changetomicrokelvinfactor = 1 / (58.04)
elif frequency == 857:
changetomicrokelvinfactor = 1 / (2.27)
else:
print("frequency not defined at", frequency)
CIBfactor = changetomicrokelvinfactor #self.solar_luminosity_per_Megaparsec2_to_Jansky*changetomicrokelvinfactor
integrand_CIBCIB_1h = 1 / (
chi_sampling)**2 * CIBfactor**2 * PCIBCIB_1h
integrand_CIBCIB_2h = 1 / (
chi_sampling)**2 * CIBfactor**2 * PCIBCIB_2h
# integrand_CIBtau = 1/(chi_sampling)**2 * electronfactor * CIBfactor * PCIBe
integral_CIBCIB_1h[ell_id] = np.trapz(integrand_CIBCIB_1h,
chi_sampling)
integral_CIBCIB_2h[ell_id] = np.trapz(integrand_CIBCIB_2h,
chi_sampling)
#now log interpolate to get all ell
with np.errstate(divide='ignore'):
# plt.loglog(ell_sparse,integral_CIBCIB_2h)
#plt.loglog(ell_sparse,integral_CIBCIB_1h)
#p#lt.show()
lin_interp = scipy.interpolate.interp1d(
np.log10(ell_sparse),
np.log10(integral_CIBCIB_1h),
bounds_error=False,
fill_value="extrapolate")
self.Cl_CIBCIB_1h[frequency_index, :] = np.power(
10.0, lin_interp(np.log10(self.ls)))
self.Cl_CIBCIB_1h[
frequency_index, :conf.estim_smallscale_lmin] = 0.
lin_interp = scipy.interpolate.interp1d(
np.log10(ell_sparse),
np.log10(integral_CIBCIB_2h),
bounds_error=False,
fill_value="extrapolate")
self.Cl_CIBCIB_2h[frequency_index, :] = np.power(
10.0, lin_interp(np.log10(self.ls)))
self.Cl_CIBCIB_2h[
frequency_index, :conf.estim_smallscale_lmin] = 0.
#'''
for zbin_id in range(conf.zbins_nr):
chi_min = remote_spectra.zbins_chi[zbin_id]
chi_max = remote_spectra.zbins_chi[zbin_id + 1]
# windownorm = 1./(chi_max-chi_min) #norm of the window function to make it 1 when integrating over chi
chi_sampling = np.logspace(np.log10(chi_min),
np.log10(chi_max),
num=100)
zs = remote_spectra.zfromchi(chi_sampling)
for ell_id, ell in enumerate(ell_sparse):
#version 1. correct.
ks = (ell + (1. / 2.)) / chi_sampling
# integrand_chi_CIBtau = np.zeros( chi_sampling.shape[0] )
#limber approx
PCIBCIB_1h, PCIBCIB_2h = self.get_PCIBCIB(
ks, zs, frequency_index)
if frequency == 353:
changetomicrokelvinfactor = 1 / (287.45)
elif frequency == 545:
changetomicrokelvinfactor = 1 / (58.04)
elif frequency == 857:
changetomicrokelvinfactor = 1 / (2.27)
else:
print("frequency not defined at", frequency)
CIBfactor = changetomicrokelvinfactor #self.solar_luminosity_per_Megaparsec2_to_Jansky*changetomicrokelvinfactor
integrand_CIBCIB_1h = 1 / (
chi_sampling)**2 * CIBfactor**2 * PCIBCIB_1h
integrand_CIBCIB_2h = 1 / (
chi_sampling)**2 * CIBfactor**2 * PCIBCIB_2h
# integrand_CIBtau = 1/(chi_sampling)**2 * electronfactor * CIBfactor * PCIBe
integral_CIBCIB_1h[ell_id] = np.trapz(
integrand_CIBCIB_1h, chi_sampling)
integral_CIBCIB_2h[ell_id] = np.trapz(
integrand_CIBCIB_2h, chi_sampling)
with np.errstate(divide='ignore'):
# plt.loglog(ell_sparse,integral_CIBCIB_2h)
#plt.loglog(ell_sparse,integral_CIBCIB_1h)
#p#lt.show()
lin_interp = scipy.interpolate.interp1d(
np.log10(ell_sparse),
np.log10(integral_CIBCIB_1h),
bounds_error=False,
fill_value="extrapolate")
self.Cl_CIBCIB_1h_binned[frequency_index,
zbin_id, :] = np.power(
10.0,
lin_interp(np.log10(self.ls)))
self.Cl_CIBCIB_1h_binned[
frequency_index,
zbin_id, :conf.estim_smallscale_lmin] = 0.
lin_interp = scipy.interpolate.interp1d(
np.log10(ell_sparse),
np.log10(integral_CIBCIB_2h),
bounds_error=False,
fill_value="extrapolate")
self.Cl_CIBCIB_2h_binned[frequency_index,
zbin_id, :] = np.power(
10.0,
lin_interp(np.log10(self.ls)))
self.Cl_CIBCIB_2h_binned[
frequency_index,
zbin_id, :conf.estim_smallscale_lmin] = 0.
print("Calculation Cl_CIBCIB done.")
def lensing_kernel(self,chi):
#possibly off by a factor of 2, check this.
chi_s=remote_spectra.chifromz(1100)
return 3/2*self.halomodel.omegam*self.halomodel.H0**2*(chi_s-chi)/(chi_s*chi)*1/(lightspeed/1000)**2*(1+remote_spectra.zfromchi(chi))
def Luminosity_from_flux(self,S,z):
#inverse of above
return 4 * np.pi * remote_spectra.chifromz(z)**2*(1+z)*S
