def T_line(z,line_name="CII",fduty=1.0):
mass_bin, dndlnM= hmf(z)
L_line= mhalo_to_lline(mass_bin, z, line_name=line_name)
L_line*=p.Lsun
nu_rest_line_Hz=p.nu_rest(line_name)*p.Ghz_to_hz
integrand=dndlnM * L_line
integration=simps(integrand, np.log(mass_bin))
factor=fduty*(p.c_in_m**3/8.0/np.pi)*((1+z)**2/(p.kb_si*nu_rest_line_Hz**3*p.cosmo.H_z(z)))
result=factor*integration
return result
def I_line(z,line_name="CII"):
#mass_range=np.logspace(np.log10(Mmin), np.log10(Mmax),num=500)
mass_bin, dndlnM= hmf(z)
L_line = mhalo_to_lline(mass_bin, z, line_name=line_name)
L_line *= p.Lsun
#factor= (p.c_in_m)/(4*p.Ghz_to_hz*np.pi*p.nu_rest(line_name=line_name)*p.cosmo.H_z(z))
factor= (p.c_in_m)/(4*p.Ghz_to_hz*np.pi*p.nu_rest(line_name=line_name)*p.cosmo.H_z(z))
integrand=factor * dndlnM * L_line
integration=simps(integrand, np.log(mass_bin))
return (integration)/(p.jy_unit)# In Jy/sr unit
def nu_obs_to_z(nu_obs, line_name='CII'):
"""
This function evaluates the redshift of a particular line emission
corresponding to the observed frequency.
return: redshift of line emission.
"""
nu_rest_line = p.nu_rest(line_name=line_name)
assert (
nu_obs <= nu_rest_line
), "Observed frequency cannot be smaller than the %s rest frame frequency. In that case z will be negative, which is non physical" % (
line_name)
z = (nu_rest_line / nu_obs) - 1
return z
def inu(z, line_name='CII'):
mass_bin, dndlnM= hmf(z)
L_line= mhalo_to_lline(mass_bin, z, line_name=line_name)
L_line*=p.Lsun
#factor= (p.c_in_m)/(4*p.Ghz_to_hz*np.pi*p.nu_rest(line_name=line_name)*p.cosmo.H_z(z))
dl_bi_dnu= (p.c_in_m)*(1+z)**2/(p.Ghz_to_hz*p.nu_rest(line_name=line_name)*p.cosmo.H_z(z))
da=p.cosmo.D_co(z) # For a flat universe
dl=p.cosmo.D_luminosity(z)
#factor= (p.c_in_m)/(4*p.Ghz_to_hz*np.pi*p.nu_rest(line_name=line_name))
integrand=(dndlnM * L_line * da**2 * dl_bi_dnu) / (4 * np.pi * dl**2)
integration=simps(integrand, np.log(mass_bin))
return integration/(p.jy_unit)
def V_pix(z, theta_min, delta_nu, line_name='CII'):
'''
z: redshift
lambda_line: frequncy of line emission in micrometer
theta_min: beam size in arc-min
delta_nu: the frequency resolution in GHz
'''
theta_rad = theta_min * p.minute_to_radian
nu = p.nu_rest(line_name) * p.Ghz_to_hz
delta_nu *= p.Ghz_to_hz
lambda_line = freq_to_lambda(nu)
y = lambda_line * (1 + z)**2 / cosmo.H_z(z)
res = cosmo.D_co(z)**2 * y * (theta_rad)**2 * delta_nu
return res * (p.m_to_mpc)**3
def V_surv(z, S_area, B_nu, line_name='CII'):
'''
Calculates the survey volume in MPc.
z: redshift
lambda_line: frequncy of line emission in micrometer
A_s: Survey area in degree**2
B_nu: Total frequency band width resolution in GHz
return: Survey volume.
'''
nu = p.nu_rest(line_name) * p.Ghz_to_hz
B_nu *= p.Ghz_to_hz
Sa_rad = S_area * (p.degree_to_radian)**2
lambda_line = freq_to_lambda(nu)
y = lambda_line * (1 + z)**2 / cosmo.H_z(z)
res = cosmo.D_co(z)**2 * y * (Sa_rad) * B_nu
return res * (p.m_to_mpc)**3
def calc_intensity_3d(boxsize,
ngrid,
halocat_file,
halo_redshift,
line_name='CII',
halo_cutoff_mass=1e11,
use_scatter=False,
halocat_file_type='npz',
intensity_unit='jy/sr'):
'''
Calculate luminosity for input parameters
'''
#low_mass_log=0.0
cellsize = boxsize / ngrid
V_cell = (cellsize)**3
halomass, halo_cm = lu.make_halocat(halocat_file,
filetype=halocat_file_type,
boxsize=boxsize)
nhalo = len(halomass)
x_halos = halo_cm[range(0, nhalo * 3, 3)]
y_halos = halo_cm[range(1, nhalo * 3, 3)]
z_halos = halo_cm[range(2, nhalo * 3, 3)]
print('Minimum halo mass:', halomass.min())
print('Maximum halo mass:', halomass.max())
#halomass_filter=halomass
#mh=halomass)
#logmh=np.array([int(logmh[key]) for key in range(nhalo)])
mass_cut = halomass >= halo_cutoff_mass
halomass = halomass[mass_cut]
x_halos_cut = x_halos[mass_cut]
y_halos_cut = y_halos[mass_cut]
z_halos_cut = z_halos[mass_cut]
halo_cm = np.concatenate([x_halos_cut, y_halos_cut, z_halos_cut])
hcut_len = len(halomass)
lcp = np.zeros(hcut_len)
for i in range(hcut_len):
lcp[i] = mhalo_to_lline(halomass[i],
halo_redshift,
line_name=line_name,
use_scatter=use_scatter)
grid_lum = lu.grid(halo_cm, lcp, boxsize, ngrid, ndim=3)
#print("shape of grid_lum", np.shape(grid_lum))
prefac = p.c_in_m / (4 * np.pi * p.nu_rest(line_name=line_name) *
p.Ghz_to_hz * p.cosmo.H_z(halo_redshift))
#print("shape of prefac", np.shape(prefac))
if (intensity_unit == "jy" or intensity_unit == "Jy"
or intensity_unit == "JY"):
grid_intensity = prefac * (
grid_lum * p.Lsun /
(V_cell * p.mpc_to_m**3)) / p.jy_unit #transformed to jansky unit
if (intensity_unit == "jy/sr" or intensity_unit == "Jy/sr"
or intensity_unit == "JY/sr"):
grid_intensity = prefac * (grid_lum * p.Lsun /
(V_cell * p.mpc_to_m**3)) / p.jy_unit / (
4 * np.pi) # JY/sr unit
return grid_intensity
def L_co_log(sfr, alpha, beta):
nu_co_line = p.nu_rest(line_name)
L_ir_sun = sfr * 1e10
L_coprime = (L_ir_sun * 10**(-beta))**(1 / alpha)
L_co = 4.9e-5 * (nu_co_line / 115.27)**3 * L_coprime
return np.log10(L_co)