'omega_b':0.02225,
'omega_cdm':0.1198,
'A_s':A_s,
'n_s':n_s,
'tau_reio':0.079,
'output':'tCl,lCl,mPk,dTk,vTk',
'use_big_theta_scf': 'yes',
'scf_has_perturbations': 'yes',
'attractor_ic_scf': 'no',
'write background':'yes',
'compute damping scale':'yes'}
try:
cosmo.set(params) # Set the parameters to the cosmological code
cosmo.compute() # solve physics
m_axion = 10**cosmo.log10_m_axion()*h*100/_c_
print "m_axion %f"%(m_axion)
# k_res_analytical = 0.79*m_axion*Theta_initial[j]*(10**ac[i])
k_res_analytical = 0.79*m_axion*Theta_initial[j]*(10**ac[i])
one_time = cosmo.get_transfer(0) # transfer functions at each time tau
k = one_time['k (h/Mpc)']
delta_phi_scf = np.abs(one_time['delta_phi_scf']) ##evaluated today
k_of_delta = interp1d(delta_phi_scf,k)
background = cosmo.get_background() # load background table
background_tau = background['conf. time [Mpc]'] # read conformal times in background table
background_z = background['z'] # read redshift
background_Om_scf = background['(.)Omega_scf'] # read redshift
background_z_at_tau = interp1d(background_tau,background_z)
phi_enveloppe = Theta_initial[j]*10**cosmo.log10_f_axion()*(2/(10**ac[i]))**(-3.*(1+wn)/2/n_axion) ##evaluated today
delta_max = np.sqrt(delta_phi_scf*delta_phi_scf*A_s*(k/K_star)**(n_s-1))/(phi_enveloppe)
print max(delta_max), np.where(delta_max==max(delta_max))
label=r'$f_{\rm EDE}$')
background_phi_scf.set_ylim(tau[0], tau[-1])
background_phi_scf.set_yscale('log')
background_phi_scf.set_xlabel(r'$f_{\rm EDE}(\tau)$')
background_phi_scf.set_xticks([0.0, 0.05, 0.1])
background_phi_scf.set_ylabel(r'$\tau \,\,\, \mathrm{[Mpc]}$', labelpad=-20)
background_phi_scf.invert_yaxis()
# fig_delta_phi_scf = ax_delta_phi_scf.pcolormesh(K,T,np.log10(delta_phi_scf*delta_phi_scf*K*K*K/2/np.pi/np.pi*A_s*(K/K_star)**(n_s-1)),cmap='coolwarm',vmin=np.log10(delta_phi_scf.min()*delta_phi_scf.min()*K.min()*K.min()*K.min()/2/np.pi*A_s*(K.min()/K_star)**(n_s-1)), vmax=np.log10(delta_phi_scf.max()*delta_phi_scf.max()*K.max()*K.max()*K.max()/2/np.pi*A_s*(K.max()/K_star)**(n_s-1))) #,shading='gouraud')
# fig_delta_phi_scf = ax_delta_phi_scf.pcolormesh(K,T,np.log10(delta_phi_scf*delta_phi_scf*A_s*(K/K_star)**(n_s-1)),cmap='coolwarm',vmin=np.log10(delta_phi_scf.min()*delta_phi_scf.min()*A_s*(K.min()/K_star)**(n_s-1)), vmax=np.log10(delta_phi_scf.max()*delta_phi_scf.max()*A_s*(K.max()/K_star)**(n_s-1))) #,shading='gouraud')
# ##delta_phi power spectrum
phi_enveloppe = Theta_initial * 10**M.log10_f_axion() * (
1.7 /
(10**log10_axion_ac * background_z_at_tau(T)))**(-3. *
(1 + wn) / 2 / n_axion)
print 10**M.log10_f_axion(), 10**M.log10_m_axion(
), Theta_initial * 10**M.log10_f_axion() * 2**(-3. * (1 + wn) / 2 / n_axion)
background_phi_scf_v2 = background_phi_scf.twiny()
background_phi_scf_v2.set_ylim(tau[0], tau[-1])
# background_phi_scf_v2.set_xlim(phi_enveloppe[0],2*phi_enveloppe[-1])
background_phi_scf_v2.plot(phi_enveloppe / (10**M.log10_f_axion()),
tau,
'r--',
linewidth=2)
background_phi_scf_v2.set_xlabel(r'$\Theta=\phi/f_a$', fontsize=18)
# background_phi_scf_v2.set_xticks([0.0,0.5,1])
background_phi_scf_v2.invert_yaxis()
background_phi_scf_v2.plot(background_phi / (10**M.log10_f_axion()),
background_tau,
'r-',
linewidth=2,
one_time = M.get_transfer(background_z_at_tau(tau[i])) # transfer functions at each time tau
if i ==0: # if this is the first time in the loop: create the arrays (k, Theta0, phi)
k = one_time['k (h/Mpc)']
k_num = len(k)
Theta0 = np.zeros((tau_num,k_num))
cs2_fld = np.zeros((tau_num,k_num))
phi = np.zeros((tau_num,k_num))
# Theta0[i,:] = 0.25*one_time['d_g'][:]
a = 1/(1+background_z_at_tau(tau[i]))
if a > 10**log10ac and i_at_ac == 0:
i_at_ac=i
a_osc=10**log10ac/1.7
w_n = (n_axion-1)/(n_axion+1)
theta_osc = Theta_initial_fld *(a/a_osc)**(-3*(1+w_n)/(2*n_axion))
c = 3e5
m = 10**M.log10_m_axion()*M.h()*100/c
# print "m:",m
omega = m*np.sqrt(np.pi)*gamma((1.0+n_axion)/(2.0*n_axion))/gamma(1.0+1.0/(2*n_axion))*2**(-(1.0+n_axion)/2.0)*theta_osc**(n_axion-1.0)
# print "omega:",omega
cs2_fld[i,:] = (2*a*a*(n_axion-1)*omega*omega+k*k)/(2*a*a*(n_axion+1)*omega*omega+k*k)
phi[i,:] = one_time['phi'][:]
# Omega_scf = bg['(.)Omega_scf']
H = background['H [1/Mpc]']
Da = background['ang.diam.dist.']
z = background['z']
# tau = background['conf. time [Mpc]']
# H_of_z = interp1d(z,H)
zc = 1/(10**log10ac)-1
tau_ac = background_tau_at_z(zc)
k_of_cs2_at_ac = interp1d(cs2_fld[i_at_ac,:],k)
print cs2_fld[i_at_ac,:],i_at_ac
print i, j
# going over a_c and Om_fld values
params['log10_fraction_axion_ac'] = fEDE[j]
cosmo.empty()
cosmo.struct_cleanup()
# ensuring memory isn't being eaten up
# try to solve with a certain cosmology, no worries if it cannot
try:
cosmo.set(
params) # Set the parameters to the cosmological code
cosmo.compute() # solve physics
alpha[i][j] = (cosmo.log10_f_axion())
mu[i][j] = (cosmo.log10_m_axion())
# zc[i][j] = np.log10(cosmo.zc())
except CosmoComputationError: # this happens when CLASS fails
pass # eh, don't do anything
print('fEDE = %e \t ac = %e \t alpha = %.5f \t mu = %.5f\n' %
(fEDE[i], ac[j], alpha[i][j], mu[i][j]))
# print('fEDE = %e \t mu = %e \t alpha = %.5f \t zc = %.5f\n' %(fEDE[i], mu[j], alpha[i][j], zc[i][j]))
# # test that stuff is working by plotting the fluid energy density
# bg = cosmo.get_background()
# plt.loglog( bg['z'], bg['(.)rho_fld[0]'])
# plt.show()
###############################################################################################################################################
