# #
background_phi_scf = fig2.add_subplot(111)
background_phi_scf.plot(background_rho_scf / background_rho_tot,
background_tau,
linewidth=2,
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)
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))
k_res_numerical = k[np.where(delta_max==max(delta_max))]*h ##evaluated today
print "k_res analytical %f Mpc-1, k_res numerical %f Mpc-1"%(k_res_analytical,k_res_numerical)
except CosmoComputationError: # this happens when CLASS fails
print "bug!"
k_res_numerical = 0
k_nl_scf[i][j] = 100 #arbitrary large number: bug
z_nl_scf[i][j] = 0 #arbitrary large number: bug
Omega_nl_scf[i][j] = 1e-30 #arbitrary small number
##2em iteration: find z_nl at which k_res becomes non linear
cosmo.empty()
cosmo.struct_cleanup()
if k_res_numerical != 0:
for j in range(N):
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()
