def magnitudeAB_from_sfr(sfr):
"""Use Kennicutt (1998) conversion from UV luminosity to AB magnitude.
Convenience function: uses L_nu_from_sfr and
magnitudes.magnitude_AB_from_L_nu.
"""
lnu = L_nu_from_sfr(sfr)
return magnitudes.magnitude_AB_from_L_nu(lnu)
def magnitudeAB_from_sfr(sfr):
"""Use Kennicutt (1998) conversion from UV luminosity to AB magnitude.
Convenience function: uses L_nu_from_sfr and
magnitudes.magnitude_AB_from_L_nu.
"""
lnu = L_nu_from_sfr(sfr)
return magnitudes.magnitude_AB_from_L_nu(lnu)
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
