def predict_c_one(theta, age):
# Time, tq and tau are in units of Gyrs
t = N.linspace(0,14.0,100)
tq, tau = theta
sfr = expsfh(tau, tq, t)
nuv_u = N.zeros_like(sfr)
u_r = N.zeros_like(sfr)
# Work out total flux at each time given the sfh model of tau and tq (calls assign_fluxes function)
# The total_flux array has time_steps as the rows (y) and model_lambda along the columns(x)
total_flux = assign_fluxes.assign_total_flux(data[0,1:], data[1:,0], data[1:,1:], t*1E9, sfr)
# Calculate fluxes from the flux at all times then interpolate to get one colour for the age you are observing the galaxy at - if many galaxies are being observed, this also works with an array of ages to give back an array of colours
nuv_u, u_r = get_colours(t*1E9, total_flux, data)
nuv_u_age = N.interp(age, t, nuv_u)
u_r_age = N.interp(age, t, u_r)
return nuv_u_age, u_r_age
def predict_c_one(theta, age):
# Time, tq and tau are in units of Gyrs
time = N.arange(0, 0.01, 0.003)
t = N.linspace(0,14.0,100)
t = N.append(time, t[1:])
tq, tau = theta
sfr = expsfh(tau, tq, t)
nuv_u = N.zeros_like(sfr)
u_r = N.zeros_like(sfr)
# Work out total flux at each time given the sfh model of tau and tq (calls assign_fluxes function)
total_flux, masses = assign_fluxes.assign_total_flux(data[0,1:], data[1:,0], data[1:,1:], t*1E9, sfr)
# Calculate fluxes from the flux at all times then interpolate to get one colour for the age you are observing the galaxy at - if many galaxies are being observed, this also works with an array of ages to give back an array of colours
nuv_u, u_r, rmag = get_colours(t*1E9, total_flux, data)
nuv_u_age = N.interp(age, t, nuv_u)
u_r_age = N.interp(age, t, u_r)
rmag_age = N.interp(age, t, rmag)
mass = N.interp(age, t, masses)
return nuv_u_age, u_r_age, rmag_age, mass
def predict_colour_for_loop(tq, tau, z):
cosmo = FlatLambdaCDM(H0 = 71.0, Om0 = 0.26)
age = cosmo.age(z)
print age
#time = N.arange(0, 0.01, 0.003)
#t = N.arange(0, 13.7, 0.01)
#time = N.append(time, t[1:])
time = N.arange(28.0)/2.0
dir ='/Users/becky/Projects/Green-Valley-Project/bc03/models/Padova1994/chabrier/ASCII/'
model = 'extracted_bc2003_lr_m62_chab_ssp.ised_ASCII'
data = N.loadtxt(dir+model)
sfr = N.zeros(len(time)*len(tq)*len(tau)).reshape(len(time), len(tq), len(tau))
nuv_u = N.zeros_like(sfr)
u_r = N.zeros_like(sfr)
nuv_u_age = N.zeros(len(age)*len(tq)*len(tau)).reshape(len(age),len(tq), len(tau))
u_r_age = N.zeros_like(nuv_u_age)
for m in range(len(tq)):
for n in range(len(tau)):
sfr[:,m,n] = expsfh(tau[n], tq[m], time)
total_flux = assign_fluxes.assign_total_flux(data[0,1:], data[1:,0], data[1:,1:], time*1E9, sfr[:,m,n])
nuv_u[:,m,n], u_r[:,m,n] = get_colours(total_flux, data)
nuv_u_age[:,m,n] = N.interp(age, time, nuv_u[:,m,n])
u_r_age[:,m,n] = N.interp(age, time, u_r[:,m,n])
return nuv_u_age, u_r_age
