def volume_radius_dmdr(mass, **cosmology):
"""The volume, radius, and dm/dr for a sphere of the given mass.
Uses the mean density of the universe.
Parameters
----------
mass: array
mass of the sphere in Solar Masses, M_sun.
Returns
-------
volume in Mpc^3
radius in Mpc
dmdr in Msun / Mpc
"""
rho_crit, rho_0 = cden.cosmo_densities(**cosmology)
volume = mass / rho_0
r = (volume / ((4. / 3.) * math.pi))**(1. / 3.)
dmdr = 4. * math.pi * r**2. * rho_0
return volume, r, dmdr
def volume_radius_dmdr(mass, **cosmology):
"""The volume, radius, and dm/dr for a sphere of the given mass.
Uses the mean density of the universe.
Parameters
----------
mass: array
mass of the sphere in Solar Masses, M_sun.
Returns
-------
volume in Mpc^3
radius in Mpc
dmdr in Msun / Mpc
"""
rho_crit, rho_0 = cden.cosmo_densities(**cosmology)
volume = mass / rho_0
r = (volume / ((4. / 3.) * math.pi))**(1./3.)
dmdr = 4. * math.pi * r**2. * rho_0
return volume, r, dmdr
def radius_to_mass(r, **cosmology):
"""The mass of a sphere of radius r in Mpc.
Uses the mean density of the universe.
"""
volume = (4./3.) * math.pi * r**3.
if 'rho_0' in cosmology:
rho_0 = cosmology['rho_0']
else:
rho_crit, rho_0 = cden.cosmo_densities(**cosmology)
mass = volume * rho_0
return mass
def radius_to_mass(r, **cosmology):
"""The mass of a sphere of radius r in Mpc.
Uses the mean density of the universe.
"""
volume = (4./3.) * math.pi * r**3.
if 'rho_0' in cosmology:
rho_0 = cosmology['rho_0']
else:
rho_crit, rho_0 = cden.cosmo_densities(**cosmology)
mass = volume * rho_0
return mass
import useful_functions as uf import distance as cd import density as den import constants as cc import reionization as cr from decimal import Decimal cosmo=uf.cosmo Mps_interpf=uf.Mps_interpf n_points=uf.n_points z_r=10. x_e=1. G=cc.G_const_Mpc_Msun_s/cc.M_sun_g #rho_c=3*H0**2/(8.*np.pi*G) rho_c=den.cosmo_densities(**cosmo)[0]*cc.M_sun_g #in units of g/Mpc^3 sigma_T=cc.sigma_T_Mpc tau_r=0.055 T_rad=2.73 #In Kelvin chi_r = uf.chi(z_r) chi_m = uf.chi(1100) chi_min=0.0001 k_min=1e-3 k_max=0.1 chi_array=np.linspace(chi_min,chi_m,n_points) #tau_r=0.046*omega_b_0*h*x_e[np.sqrt(omega_M_0(1+z_r)**3+(1-omega_M_0))-1] #get matter power spec data mu_e=1.44 m_p=cc.m_p_g #in grams rho_g0=cosmo['omega_b_0']*rho_c
import numpy as np import matplotlib.pyplot as plt import density as den import constants as cc import reionization as cr import useful_functions as uf #print (chi_m) cosmo=uf.cosmo zed=uf.zed n_points=2000 H0=cc.H100_s*cosmo['h'] x_e=1. G=cc.G_const_Mpc_Msun_s/cc.M_sun_g #rho_c=3*H0**2/(8.*np.pi*G) rho_c=den.cosmo_densities(**cosmo)[0]*cc.M_sun_g gamma=0.53 sigma_T=cc.sigma_T_Mpc z_r=6. chi_r=uf.chi(z_r) chi_m = uf.chi(1100) k_min=0.0001 k_max=10. chi=np.linspace(0.0001,chi_r,n_points) #chi = np.logspace(np.log(0.0001),np.log(chi_m),n_points) kpar = np.logspace(-4.,1.,n_points) Mps_interpf=uf.Mps_interpf #print (omega_b_0) #tau_r=0.046*omega_b_0*h*x_e[np.sqrt(omega_M_0(1+z_r)**3+(1-omega_M_0))-1] #get matter power spec data
