def luminosity_correction(self):
"""
The galaxev templates are in L_sun/Angstrom, with L_sun = 3.826e26W
so we change to the appropriate flux at each relevent redshift. We
also multiply by 1e11, so that the flux is appropriate for a galaxy
of mass 1e11 M_sun.
Our SED code gives correct magnitudes if the SED is in units of
ergs/s/cm/cm/Angstrom, and our distance class gives distances in
Mpc/h, so we will need to use the conversion Mpc = 3.08568e24cm
and assume a value for h.
The conversion factor is conv = flux_density/luminosity_density and
the templates should therefore be multiplied by conv to get the
correct flux_density. The factor of (1+z) accounts for the fact that
these are _densities_.
1e11 3.826e33
conv = ----- ----------
(1+z) 4 pi Dl**2
"""
from stellarpop import distances
from math import pi
dist = distances.Distance()
dist.h = 0.7
dist.OMEGA_M = 0.3
dist.OMEGA_L = 0.7
cm_per_Mpc = 3.08568e24
corr = []
for z in self.redshifts:
if z == 0:
dl = 1e-5 * cm_per_Mpc
else:
dl = dist.Dl(z) * cm_per_Mpc
conv = 1 / (4 * pi * dl**2)
conv *= 3.826e33
corr.append(conv)
return corr
filtermag = tools.VegaFilterMagnitude(f1, SED, z1)
# vegatmp = tools.getSED('Vega')
# vegaAB = tools.ABFilterMagnitude(f1,vegatmp,0.)
else:
filtermag = tools.ABFilterMagnitude(f1, SED, z1)
magoffset = m1 - filtermag
#print magoffset
if vega:
m2 = tools.VegaFilterMagnitude(f2, SED, z2) + magoffset
else:
m2 = tools.ABFilterMagnitude(f2, SED, z2) + magoffset
if z1 != z2:
from stellarpop import distances
from math import log10
dist = distances.Distance()
dist.OMEGA_M = Om
dist.OMEGA_L = OL
dist.h = H0 / 100.
if z2 != 0.:
dimming = dist.Dl(z1) / dist.Dl(z2)
else:
dimming = dist.Dl(z1) / 1e-5
m2 -= 5. * log10(dimming)
if convert:
vegatmp = tools.getSED('Vega')
vegatmp = (vegatmp[0], vegatmp[1])
vegaAB = tools.ABFilterMagnitude(f2, vegatmp, 0.)
if vega:
m2 += vegaAB