def test_sfrd():
""" Check conversion of Lmin -> SFRD.
At z=7:
Lmin = 0.2 L*z=6 -> Mmin=-18.5 -> log(rho/erg/s/Hz/Mpc^3)=25.5 ->
SFRD = 10^-2.32 Msun/yr^-1/Mpc^-3.
From Oesch et al (2009 ApJ 690 1350).
"""
cosmo = cparam.WMAP7_BAO_H0_mean(flat=True)
# # From Bouwens 2008ApJ...686..230B
# lfhist = luminosityfunction.LFHistory(params=luminosityfunction.B2008,
# **cosmo)
# mStarz6 = lfhist.params_z(6.0)['MStar']
alpha = -1.74
mStarz6 = -20.24
mStarz7 = -19.7
phiStar = 1.4e-3
lStarz6 = magnitudes.L_nu_from_magAB(mStarz6)
lmin = 0.2 * lStarz6
magmin = magnitudes.magnitude_AB_from_L_nu(lmin)
ltot = luminosityfunction.schechterCumuLM(magnitudeAB=magmin,
MStar=mStarz7,
phiStar=phiStar,
alpha=alpha)
sfrd = luminosityfunction.sfr_from_L_nu(ltot)
print """Lmin = 0.2 L*z=6 -> Lmin/erg/s/Hz = %.3g -> Mmin = %.3g ->
log(rho/(erg/s/Hz/Mpc^3)) = %.3g -> log(SFRD/(MSun/yr)) = %.3g"""\
% (lmin, magmin, numpy.log10(ltot), numpy.log10(sfrd))
ltotz6 = luminosityfunction.schechterCumuLM(magnitudeAB=magmin,
MStar=mStarz6,
phiStar=phiStar,
alpha=alpha)
print "luminosity density increase from z=7 to z=6 is %.2g percent." \
% (100 * (1. - ltot/ltotz6))
assert numpy.abs(numpy.round(1. - ltot/ltotz6, 1) - 0.5) < 0.1
assert numpy.round(magmin, 1) == -18.5
assert numpy.abs(numpy.round(numpy.log10(ltot), 1) - 25.5) < 0.2
assert numpy.abs(numpy.round(numpy.log10(sfrd), 1) - -2.32) < 0.05
def test_tau_instant():
"""Check the optical depth we get using the WMAP z_reion.
"""
dz = 0.1
z = numpy.arange(80., 0. - 1.5 * dz, -1. * dz)
# Can't match WMAP7 optical depths exactly. Need to look into new
# treatment in CAMB as mentioned in the WMAP7 paper (see
# parameters.py).
cosmos = [
cparam.WMAP7_BAO_H0_mean(flat=True),
cparam.WMAP7_ML(flat=True),
cparam.WMAP5_BAO_SN_mean(flat=True),
cparam.WMAP5_ML(flat=True),
cparam.WMAP5_mean(flat=True)
]
# The WMAP5 numbers apparently assume He is neutral, while WMAP7
# includes simultaneous singly ionized He plus Helium (double)
# reionization at z=3.5.
x_ionHe_list = [1.0, 1.0, 0, 0, 0]
z_rHe_list = [3.5, 3.5, None, None, None] #[3.5, None, None, None]
for cosmo in cosmos:
# Fully ionized H
x_ionH = 1.0
# He ionization with H?
x_ionHe = x_ionHe_list.pop(0)
# Redshift for Helium double reionization?
z_rHe = z_rHe_list.pop(0)
zr = cosmo['z_reion']
tau_zr = cosmo['tau']
tau_calc = cr.optical_depth_instant(zr,
x_ionH=x_ionH,
x_ionHe=x_ionHe,
z_rHe=z_rHe,
verbose=1,
**cosmo)
print "z_r = %f, testing tau:" % zr,
print tu.fractional_diff_string(tau_zr, tau_calc, 3)
ntest.assert_approx_equal(tau_calc,
tau_zr,
significant=2,
err_msg="Optical depth doesn't match WMAP")
def test_t_0():
"""Check the age of the universe we get using WMAP cosmologies.
We only find agreement to 3 sig figs, not the 4 specified in the
WMAP paper.
The results of test_age.py show that we're doing the integral
correctly, so I think the problem is that we're not taking into
account some of the higher-order effects included in the WMAP
numbers.
"""
dz = 0.1
z = numpy.arange(80., 0. - 1.5 * dz, -1. * dz)
flat = True
cosmos = [
cparam.WMAP7_BAO_H0_mean(flat=True),
cparam.WMAP7_ML(flat=True),
cparam.WMAP5_BAO_SN_mean(flat=True),
cparam.WMAP5_ML(flat=True),
cparam.WMAP5_mean(flat=True)
]
for cosmo in cosmos:
age = cd.age(0.0, **cosmo)
age_flat = cd.age_flat(0.0, **cosmo)
gyr = 1e9 * cc.yr_s
age /= gyr
age_flat /= gyr
print "integrated age: ",
print tu.fractional_diff_string(age, cosmo['t_0'], 4)
ntest.assert_approx_equal(age,
cosmo['t_0'],
significant=3,
err_msg="Integrated age doesn't match WMAP")
print "analytical age: ",
print tu.fractional_diff_string(age_flat, cosmo['t_0'], 4)
ntest.assert_approx_equal(age_flat,
cosmo['t_0'],
significant=3,
err_msg="Analytical age doesn't match WMAP")
def plotLFevo(
hist=None,
params=B2008,
extrap_var='t',
#maglim = -21.07 - 2.5 * numpy.log10(0.2)):
maglim=-21. - 2.5 * numpy.log10(0.2),
z_max=20.0,
skipIon=True):
"""Plot evolution of luminosity function params and total luminsity.
Schechter function at each redshift is integrated up to maglim to
find total luminsity.
"""
for (k, v) in params.iteritems():
params[k] = numpy.asarray(v)
if hist is None:
cosmo = cp.WMAP7_BAO_H0_mean(flat=True)
hist = LFHistory(params, extrap_var=extrap_var, **cosmo)
else:
params = hist.params
extrap_var = hist.extrap_var
cosmo = hist.cosmo
z = params['z']
t = cd.age(z, **cosmo)[0] / cc.yr_s
MStar = params['MStar']
phiStar = params['phiStar']
alpha = params['alpha']
if maglim is None:
ltot = schechterTotLM(MStar=MStar, phiStar=phiStar, alpha=alpha)
else:
ltot = schechterCumuLM(magnitudeAB=maglim,
MStar=MStar,
phiStar=phiStar,
alpha=alpha)
print(hist._MStarfunc.extrap_string())
zPlot = numpy.arange(z.min() - 0.1, z_max, 0.1)
tPlot = cd.age(zPlot, **cosmo)[0] / cc.yr_s
newparams = hist.params_z(zPlot)
MPlot = newparams['MStar']
phiPlot = newparams['phiStar']
alphaPlot = newparams['alpha']
if maglim is None:
ltotPlot = hist.schechterTotLM(zPlot)
else:
ltotPlot = hist.schechterCumuLM(zPlot, magnitudeAB=maglim)
# From Table 6 of 2008ApJ...686..230B
lB2008 = 10.**numpy.array([26.18, 25.85, 25.72, 25.32, 25.14])
iPhot = hist.iPhotonRateDensity_z(zPlot, maglim=maglim)
# iPhotFunc = lambda t1: cc.yr_s * hist.iPhotonRateDensity_t(t1,
# maglim=maglim)
if not skipIon:
xH = hist.ionization(zPlot, maglim)
import pylab
pylab.figure(1)
pylab.gcf().set_label('LFion_vs_z')
if skipIon:
pylab.subplot(111)
else:
pylab.subplot(211)
pylab.plot(zPlot, iPhot)
if not skipIon:
pylab.subplot(212)
pylab.plot(zPlot, xH)
pylab.ylim(0.0, 1.5)
pylab.figure(2)
pylab.gcf().set_label('LFparams_vs_z')
pylab.subplot(311)
pylab.plot(z, MStar, '-')
pylab.plot(z, MStar, 'o')
pylab.plot(zPlot, MPlot, ':')
pylab.subplot(312)
pylab.plot(z, phiStar, '-')
pylab.plot(z, phiStar, 'o')
pylab.plot(zPlot, phiPlot, ':')
pylab.subplot(313)
pylab.plot(z, alpha, '-')
pylab.plot(z, alpha, 'o')
pylab.plot(zPlot, alphaPlot, ':')
pylab.figure(3)
pylab.gcf().set_label('LFparams_vs_t')
pylab.subplot(311)
pylab.plot(t, MStar, '-')
pylab.plot(t, MStar, 'o')
pylab.plot(tPlot, MPlot, ':')
pylab.subplot(312)
pylab.plot(t, phiStar, '-')
pylab.plot(t, phiStar, '.')
pylab.plot(tPlot, phiPlot, ':')
pylab.subplot(313)
pylab.plot(t, alpha, '-')
pylab.plot(t, alpha, 'o')
pylab.plot(tPlot, alphaPlot, ':')
pylab.figure(4)
pylab.gcf().set_label('LFlum_vs_z')
pylab.subplot(121)
pylab.plot(z, ltot, 'o')
pylab.plot(z, lB2008, 'x')
pylab.plot(zPlot, ltotPlot)
pylab.subplot(122)
pylab.plot(t, ltot, 'o')
pylab.plot(t, lB2008, 'x')
pylab.plot(tPlot, ltotPlot)
... } >>> mass = cp.virial_mass(1e4, 6.0, **cosmo) >>> temp = cp.virial_temp(mass, 6.0, **cosmo) >>> print "Mass = %.3g M_sun" % mass Mass = 1.68e+08 M_sun >>> print round(temp, 4) 10000.0 Calculate the critical and matter densities: >>> from cosmolopy import * >>> 'rho_crit=%.3g Msun/Mpc^3, rho_0=%.3g Msun/Mpc^3' % cden.cosmo_densities(**fidcosmo) 'rho_crit=1.38e+11 Msun/Mpc^3, rho_0=3.75e+10 Msun/Mpc^3' Look in the tests/ and examples/ directories for more examples. """ import cosmolopy.constants as cc import cosmolopy.density as cden import cosmolopy.distance as cd import cosmolopy.perturbation as cp import cosmolopy.reionization as cr import cosmolopy.parameters as cparam import cosmolopy.magnitudes as cmag import cosmolopy.luminosity_function as cl import cosmolopy.transfer_function import cosmolopy.transfer_function_fit fidcosmo = cparam.WMAP7_BAO_H0_mean(flat=True, extras=True)