def calc_emline(stars_list):
print('[SED_gen/calc_emline]: Calculating Emission Line Fluxes')
#this function is awful and redundant. itloops over just the new
#stars in the box and calculates the SEDs for the ones smaller
#than cfg.par.HII_max_age. its a bit wasteful since we already
#calculate these SEDs, but its difficult to get the file to save
#in a nice format without incl
global sp
if sp is None:
sp = fsps.StellarPopulation()
#set up arrays
#first how many young stars are there?
newstars_idx = []
for counter, star in enumerate(stars_list):
if star.age <= cfg.par.HII_max_age:
newstars_idx.append(counter)
num_newstars = len(newstars_idx)
#set up a dummy sps model just to get number of wavelengths
sp.params["tage"] = stars_list[0].age
sp.params["zmet"] = stars_list[0].fsps_zmet
sp.params["add_neb_emission"] = True
wav, spec = sp.get_spectrum()
n_emlines = len(sp.emline_wavelengths)
#now set up the actual arrays
master_emline_wavelength = np.zeros([n_emlines])
master_emline_lum = np.zeros([num_newstars, n_emlines])
#loop through the newstars now and save the emlines
for counter, i in enumerate(newstars_idx):
num_HII_clusters = int(
np.floor((stars_list[i].mass / constants.M_sun.cgs.value) /
(cfg.par.stellar_cluster_mass)))
#first we calculate the spectrum without lines on to get logU
sp.params["tage"] = stars_list[i].age
sp.params["imf_type"] = cfg.par.imf_type
sp.params["pagb"] = cfg.par.pagb
sp.params["sfh"] = 0
sp.params["zmet"] = stars_list[i].fsps_zmet
sp.params["add_neb_emission"] = False
sp.params["add_agb_dust_model"] = cfg.par.add_agb_dust_model
sp.params['gas_logu'] = cfg.par.gas_logu
if cfg.par.FORCE_gas_logz == False:
sp.params['gas_logz'] = np.log10(stars_list[i].metals /
cfg.par.solar)
else:
sp.params['gas_logz'] = cfg.par.gas_logz
if cfg.par.CF_on == True:
sp.params["dust_type"] = 0
sp.params["dust1"] = 1
sp.params["dust2"] = 0
sp.params["dust_tesc"] = tesc_age
#sp = fsps.StellarPopulation(tage=stars_list[i].age,imf_type=2,sfh=0,zmet=stars_list[i].fsps_zmet)
spec = sp.get_spectrum(tage=stars_list[i].age,
zmet=stars_list[i].fsps_zmet)
num_HII_clusters = int(
np.floor((stars_list[i].mass / constants.M_sun.cgs.value) /
(cfg.par.stellar_cluster_mass)))
neb_file_output = False
sp.params["add_neb_emission"] = False
spec = sp.get_spectrum(tage=stars_list[i].age,
zmet=stars_list[i].fsps_zmet)
#now we know logU, so recalculate the lines
if cfg.par.FORCE_gas_logu:
LogU = cfg.par.gas_logu
else:
LogQ, Rin, LogU = calc_LogU(1.e8 * constants.c.cgs.value / spec[0],
spec[1] * constants.L_sun.cgs.value,
cfg.par.HII_nh,
cfg.par.HII_T,
mstar=cfg.par.stellar_cluster_mass)
sp.params['gas_logu'] = LogU
sp.params["add_neb_emission"] = True
spec = sp.get_spectrum(tage=stars_list[i].age,
zmet=stars_list[i].fsps_zmet)
f = spec[1] * num_HII_clusters
emline_luminosity = sp.emline_luminosity * num_HII_clusters
emline_wavelength = sp.emline_wavelengths
#the stellar population returns the calculation in units of Lsun/1 Msun: https://github.com/dfm/python-fsps/issues/117#issuecomment-546513619
master_emline_lum[counter, :] = emline_luminosity * (
(stars_list[i].mass * u.g).to(u.Msun).value)
if counter == 0:
master_emline_wavelength = emline_wavelength
#set up the emline output file as new, and insert the wavelengths
dump_emline(master_emline_wavelength, None, append=False)
#write the remainder of the emline file
dump_emline(master_emline_wavelength, master_emline_lum, append=True)
def newstars_gen(stars_list):
global sp
if sp is None:
sp = fsps.StellarPopulation()
#the newstars (particle type 4; so, for cosmological runs, this is all
#stars) are calculated in a separate function with just one argument so that it is can be fed
#into pool.map for multithreading.
#sp = fsps.StellarPopulation()
sp.params["tage"] = stars_list[0].age
sp.params["imf_type"] = cfg.par.imf_type
sp.params["pagb"] = cfg.par.pagb
sp.params["sfh"] = 0
sp.params["zmet"] = stars_list[0].fsps_zmet
sp.params["add_neb_emission"] = False
sp.params["add_agb_dust_model"] = cfg.par.add_agb_dust_model
sp.params['gas_logu'] = cfg.par.gas_logu
if cfg.par.FORCE_gas_logz == False:
sp.params['gas_logz'] = np.log10(stars_list[0].metals / cfg.par.solar)
else:
sp.params['gas_logz'] = cfg.par.gas_logz
#first figure out how many wavelengths there are
spec = sp.get_spectrum(tage=stars_list[0].age,
zmet=stars_list[0].fsps_zmet)
nu = 1.e8 * constants.c.cgs.value / spec[0]
nlam = len(nu)
stellar_nu = np.zeros([nlam])
stellar_fnu = np.zeros([len(stars_list), nlam])
minage = 13 #Gyr
for i in range(len(stars_list)):
if stars_list[i].age < minage:
minage = stars_list[i].age
tesc_age = np.log10((minage + cfg.par.birth_cloud_clearing_age) * 1.e9)
# Get the number of ionizing photons from SED
#calculate the SEDs for new stars
for i in range(len(stars_list)):
sp.params["tage"] = stars_list[i].age
sp.params["imf_type"] = cfg.par.imf_type
sp.params["pagb"] = cfg.par.pagb
sp.params["sfh"] = 0
sp.params["zmet"] = stars_list[i].fsps_zmet
sp.params["add_neb_emission"] = False
sp.params["add_agb_dust_model"] = cfg.par.add_agb_dust_model
if cfg.par.FORCE_gas_logz == False:
LogZ = np.log10(stars_list[i].metals / cfg.par.solar)
else:
LogZ = cfg.par.gas_logz
if cfg.par.CF_on == True:
sp.params["dust_type"] = 0
sp.params["dust1"] = 1
sp.params["dust2"] = 0
sp.params["dust_tesc"] = tesc_age
#sp = fsps.StellarPopulation(tage=stars_list[i].age,imf_type=2,sfh=0,zmet=stars_list[i].fsps_zmet)
spec = sp.get_spectrum(tage=stars_list[i].age,
zmet=stars_list[i].fsps_zmet)
f = spec[1]
#Only including particles below the maximum age limit for calulating nebular emission
if cfg.par.add_neb_emission and stars_list[
i].age <= cfg.par.HII_max_age:
num_HII_clusters = int(
np.floor((stars_list[i].mass / constants.M_sun.cgs.value) /
(cfg.par.stellar_cluster_mass)))
f = np.zeros(nlam)
neb_file_output = cfg.par.neb_file_output
sp.params["add_neb_emission"] = False
spec = sp.get_spectrum(tage=stars_list[i].age,
zmet=stars_list[i].fsps_zmet)
if cfg.par.FORCE_gas_logu:
alpha = 2.5e-13 * ((cfg.par.HII_T / (10**4))**(-0.85))
LogU = cfg.par.gas_logu
LogQ = np.log10((10**(3 * LogU)) *
(36 * np.pi * (constants.c.cgs.value**3)) /
((alpha**2) * cfg.par.HII_nh))
Rin = ((3 * (10**LogQ)) /
(4 * np.pi * (cfg.par.HII_nh**2) * alpha))**(1. / 3.)
else:
LogQ, Rin, LogU = calc_LogU(
1.e8 * constants.c.cgs.value / spec[0],
spec[1] * constants.L_sun.cgs.value,
cfg.par.HII_nh,
cfg.par.HII_T,
mstar=cfg.par.stellar_cluster_mass)
if cfg.par.FORCE_logq:
LogQ = cfg.par.source_logq
if cfg.par.FORCE_inner_radius:
Rin = cfg.par.inner_radius
if neb_file_output:
logu_diagnostic(LogQ,
Rin,
LogU,
cfg.par.stellar_cluster_mass,
stars_list[i].age,
stars_list[i].fsps_zmet,
append=True)
neb_file_output = False
sp.params['gas_logu'] = LogU
sp.params['gas_logz'] = LogZ
sp.params["add_neb_emission"] = True
if cfg.par.use_cloudy_tables:
lam_neb, spec_neb = sp.get_spectrum(
tage=stars_list[i].age, zmet=stars_list[i].fsps_zmet)
else:
try:
# Calculating ionizing photons again but for 1 Msun in order to scale the output for FSPS
LogQ_1, Rin_1, LogU_1 = calc_LogU(
1.e8 * constants.c.cgs.value / spec[0],
spec[1] * constants.L_sun.cgs.value, cfg.par.HII_nh,
cfg.par.HII_T)
spec_neb = get_nebular(spec[0],
spec[1],
cfg.par.HII_nh,
LogQ,
Rin,
LogU,
LogZ,
LogQ_1,
abund=cfg.par.neb_abund,
useq=cfg.par.use_Q,
clean_up=cfg.par.cloudy_cleanup)
except ValueError as err:
lam_neb, spec_neb = sp.get_spectrum(
tage=stars_list[i].age, zmet=stars_list[i].fsps_zmet)
f = spec_neb * num_HII_clusters
stellar_nu[:] = 1.e8 * constants.c.cgs.value / spec[0]
stellar_fnu[i, :] = f
return stellar_fnu