sys.path.insert(0,
os.path.abspath(os.path.join(os.path.dirname(__file__), '..')))
import synthobs
from synthobs.sed import models
import flare
import flare.filters
import matplotlib.pyplot as plt
"This is an more efficient way of calculating the broadband luminosities of galaxies. It produces the same answer as generate_SED within ~0.05 dex"
model = models.define_model('BPASSv2.2.1.binary/ModSalpeter_300',
path_to_SPS_grid=flare.FLARE_dir +
'/data/SPS/nebular/3.0/') # DEFINE SED GRID -
# model = models.define_model('BPASSv2.2.1.binary/ModSalpeter_300', path_to_SPS_grid = flare.FLARE_dir + '/data/SPS/nebular/2.0/Z_refQ_wdust/') # DEFINE SED GRID -
model.dust_ISM = ('simple', {'slope': -1.0})
model.dust_BC = ('simple', {'slope': -1.0})
# --- read in test data
test = synthobs.test_data() # --- read in some test data
# --- create rest-frame luminosities
filters = [
'FAKE.TH.' + f for f in ['FUV', 'NUV', 'V']
] # --- define the filters. FAKE.FAKE are just top-hat filters using for extracting rest-frame quantities.
cosmo = flare.default_cosmo()
z = 8.
test = synthobs.test_data() # --- read in some test data
# --- calculate V-band (550nm) optical depth for each star particle
A = 5.2
test.tauVs = (10**A) * test.MetSurfaceDensities
model = models.define_model('BPASSv2.2.1.binary/ModSalpeter_300') # DEFINE SED GRID -
model.dust = {'slope': -1.0} # define dust curve
do_test = False
if do_test:
width_arcsec = 3.
f = 'Webb.NIRCam.F150W'
x=reg,
u=tag,
filt=filters[0]))
# exists = os.path.isfile("data/flares_sizes_highresproject"
# "_{}_{}_{}_{}_{}.hdf5".format(reg, tag, Type,
# orientation,
# filters[0].split(".")[-1]))
# if not exists:
# run = True
# else:
# run = False
run = True
model = models.define_model(
F'BPASSv2.2.1.binary/Chabrier_300') # DEFINE SED GRID -
model.dust_ISM = ('simple', {'slope': -1.}) # Define dust curve for ISM
model.dust_BC = ('simple', {
'slope': -1.
}) # Define dust curve for birth cloud component
# --- create rest-frame luminosities
F = flare.filters.add_filters(filters, new_lam=model.lam)
model.create_Lnu_grid(
F) # --- create new L grid for each filter. In units of erg/s/Hz
if run:
# Define radii
radii_fracs = (0.2, 0.5, 0.8)
def lum(sim,
kappa,
tag,
BC_fac,
inp='FLARES',
IMF='Chabrier_300',
LF=True,
filters=['FAKE.TH.FUV'],
Type='Total',
log10t_BC=7.,
extinction='default',
data_folder='data',
aperture='30'):
S_mass, S_Z, S_age, S_los, S_len, begin, end, S_ap, DTM = get_data(
sim, tag, inp, data_folder, aperture)
if np.isscalar(filters):
Lums = np.zeros(len(begin), dtype=np.float64)
else:
Lums = np.zeros((len(begin), len(filters)), dtype=np.float64)
model = models.define_model(
F'BPASSv2.2.1.binary/{IMF}') # DEFINE SED GRID -
if extinction == 'default':
model.dust_ISM = ('simple', {'slope': -1.}) #Define dust curve for ISM
model.dust_BC = ('simple', {
'slope': -1.
}) #Define dust curve for birth cloud component
elif extinction == 'Calzetti':
model.dust_ISM = ('Starburst_Calzetti2000', {''})
model.dust_BC = ('Starburst_Calzetti2000', {''})
elif extinction == 'SMC':
model.dust_ISM = ('SMC_Pei92', {''})
model.dust_BC = ('SMC_Pei92', {''})
elif extinction == 'MW':
model.dust_ISM = ('MW_Pei92', {''})
model.dust_BC = ('MW_Pei92', {''})
elif extinction == 'N18':
model.dust_ISM = ('MW_N18', {''})
model.dust_BC = ('MW_N18', {''})
else:
ValueError("Extinction type not recognised")
z = float(tag[5:].replace('p', '.'))
# --- create rest-frame luminosities
F = flare.filters.add_filters(filters, new_lam=model.lam)
model.create_Lnu_grid(
F) # --- create new L grid for each filter. In units of erg/s/Hz
for jj in range(len(begin)):
Masses = S_mass[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
Ages = S_age[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
Metallicities = S_Z[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
MetSurfaceDensities = S_los[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
MetSurfaceDensities = DTM[jj] * MetSurfaceDensities
if Type == 'Total':
tauVs_ISM = kappa * MetSurfaceDensities # --- calculate V-band (550nm) optical depth for each star particle
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
elif Type == 'Pure-stellar':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 1.0
elif Type == 'Intrinsic':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 0.0
elif Type == 'Only-BC':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
else:
ValueError(F"Undefined Type {Type}")
Lnu = models.generate_Lnu(
model=model,
F=F,
Masses=Masses,
Ages=Ages,
Metallicities=Metallicities,
tauVs_ISM=tauVs_ISM,
tauVs_BC=tauVs_BC,
fesc=fesc,
log10t_BC=log10t_BC
) # --- calculate rest-frame Luminosity. In units of erg/s/Hz
Lums[jj] = list(Lnu.values())
return Lums
def get_SED(sim,
kappa,
tag,
BC_fac,
inp='FLARES',
IMF='Chabrier_300',
log10t_BC=7.,
extinction='default',
data_folder='data',
aperture='30'):
S_mass, S_Z, S_age, S_los, S_len, begin, end, S_ap, DTM = get_data(
sim, tag, inp, data_folder, aperture)
model = models.define_model(
F'BPASSv2.2.1.binary/{IMF}') # DEFINE SED GRID -
# --- calculate intrinsic quantities
if extinction == 'default':
model.dust_ISM = ('simple', {'slope': -1.}) #Define dust curve for ISM
model.dust_BC = ('simple', {
'slope': -1.
}) #Define dust curve for birth cloud component
elif extinction == 'Calzetti':
model.dust_ISM = ('Starburst_Calzetti2000', {''})
model.dust_BC = ('Starburst_Calzetti2000', {''})
elif extinction == 'SMC':
model.dust_ISM = ('SMC_Pei92', {''})
model.dust_BC = ('SMC_Pei92', {''})
elif extinction == 'MW':
model.dust_ISM = ('MW_Pei92', {''})
model.dust_BC = ('MW_Pei92', {''})
elif extinction == 'N18':
model.dust_ISM = ('MW_N18', {''})
model.dust_BC = ('MW_N18', {''})
else:
ValueError("Extinction type not recognised")
for jj in range(len(begin)):
Masses = S_mass[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
Ages = S_age[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
Metallicities = S_Z[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
MetSurfaceDensities = S_los[begin[jj]:end[jj]][S_ap[begin[jj]:end[jj]]]
MetSurfaceDensities = DTM[jj] * MetSurfaceDensities
tauVs_ISM = kappa * MetSurfaceDensities # --- calculate V-band (550nm) optical depth for each star particle
tauVs_BC = BC_fac * (Metallicities / 0.01)
o = models.generate_SED(model,
Masses,
Ages,
Metallicities,
tauVs_ISM=tauVs_ISM,
tauVs_BC=tauVs_BC,
fesc=0.0)
if jj == 0:
lam = np.zeros((len(begin), len(o.lam)),
dtype=np.float64) #in Angstrom
stellar = np.zeros((len(begin), len(o.lam)), dtype=np.float64)
intrinsic = np.zeros((len(begin), len(o.lam)), dtype=np.float64)
no_ism = np.zeros((len(begin), len(o.lam)), dtype=np.float64)
total = np.zeros((len(begin), len(o.lam)), dtype=np.float64)
lam[jj] = o.lam
stellar[jj] = o.stellar.lnu
intrinsic[jj] = o.intrinsic.lnu
no_ism[jj] = o.BC.lnu
total[jj] = o.total.lnu
return lam, stellar, intrinsic, no_ism, total
def flux(sim, kappa, tag, BC_fac, inp='FLARES', IMF='Chabrier_300',
filters=flare.filters.NIRCam_W, Type='Total', log10t_BC=7.,
extinction='default', orientation="sim"):
kinp = np.load('/cosma/home/dp004/dc-rope1/cosma7/FLARES/'
'flares/los_extinction/kernel_sph-anarchy.npz',
allow_pickle=True)
lkernel = kinp['kernel']
header = kinp['header']
kbins = header.item()['bins']
S_mass, S_Z, S_age, S_los, G_Z, S_len, \
G_len, G_sml, S_sml, G_mass, S_coords, G_coords, \
S_vels, G_vels, cops, \
begin, end, gbegin, gend = get_data(sim, tag, inp)
Fnus = {f: np.zeros(len(S_mass), dtype=np.float64) for f in filters}
model = models.define_model(
F'BPASSv2.2.1.binary/{IMF}') # DEFINE SED GRID -
if extinction == 'default':
model.dust_ISM = (
'simple', {'slope': -1.}) # Define dust curve for ISM
model.dust_BC = ('simple', {
'slope': -1.}) # Define dust curve for birth cloud component
elif extinction == 'Calzetti':
model.dust_ISM = ('Starburst_Calzetti2000', {''})
model.dust_BC = ('Starburst_Calzetti2000', {''})
elif extinction == 'SMC':
model.dust_ISM = ('SMC_Pei92', {''})
model.dust_BC = ('SMC_Pei92', {''})
elif extinction == 'MW':
model.dust_ISM = ('MW_Pei92', {''})
model.dust_BC = ('MW_Pei92', {''})
elif extinction == 'N18':
model.dust_ISM = ('MW_N18', {''})
model.dust_BC = ('MW_N18', {''})
else:
ValueError("Extinction type not recognised")
z = float(tag[5:].replace('p', '.'))
F = flare.filters.add_filters(filters, new_lam=model.lam * (1. + z))
cosmo = flare.default_cosmo()
# --- create new Fnu grid for each filter. In units of nJy/M_sol
model.create_Fnu_grid(F, z, cosmo)
for jj in range(len(begin)):
# Extract values for this galaxy
Masses = S_mass[begin[jj]: end[jj]]
Ages = S_age[begin[jj]: end[jj]]
Metallicities = S_Z[begin[jj]: end[jj]]
gasMetallicities = G_Z[begin[jj]: end[jj]]
gasSML = G_sml[begin[jj]: end[jj]]
gasMasses = G_mass[begin[jj]: end[jj]]
if orientation == "sim":
starCoords = S_coords[:, begin[jj]: end[jj]].T - cops[:, jj]
S_coords[:, begin[jj]: end[jj]] = starCoords.T
MetSurfaceDensities = S_los[begin[jj]:end[jj]]
elif orientation == "face-on":
starCoords = S_coords[:, begin[jj]: end[jj]].T - cops[:, jj]
gasCoords = G_coords[:, begin[jj]: end[jj]].T - cops[:, jj]
gasVels = G_vels[:, begin[jj]: end[jj]].T
# Get angular momentum vector
ang_vec = util.ang_mom_vector(gasMasses, gasCoords, gasVels)
# Rotate positions
starCoords = util.get_rotated_coords(ang_vec, starCoords)
gasCoords = util.get_rotated_coords(ang_vec, gasCoords)
S_coords[:, begin[jj]: end[jj]] = starCoords.T
MetSurfaceDensities = util.get_Z_LOS(starCoords, gasCoords,
gasMasses, gasMetallicities,
gasSML, (0, 1, 2),
lkernel, kbins)
elif orientation == "side-on":
starCoords = S_coords[:, begin[jj]: end[jj]].T - cops[:, jj]
gasCoords = G_coords[:, begin[jj]: end[jj]].T - cops[:, jj]
gasVels = G_vels[:, begin[jj]: end[jj]].T
# Get angular momentum vector
ang_vec = util.ang_mom_vector(gasMasses, gasCoords, gasVels)
# Rotate positions
starCoords = util.get_rotated_coords(ang_vec, starCoords)
gasCoords = util.get_rotated_coords(ang_vec, gasCoords)
S_coords[:, begin[jj]: end[jj]] = starCoords.T
MetSurfaceDensities = util.get_Z_LOS(starCoords, gasCoords,
gasMasses, gasMetallicities,
gasSML, (2, 0, 1),
lkernel, kbins)
else:
MetSurfaceDensities = None
print(orientation,
"is not an recognised orientation. "
"Accepted types are 'sim', 'face-on', or 'side-on'")
Mage = np.nansum(Masses * Ages) / np.nansum(Masses)
Z = np.nanmean(gasMetallicities)
MetSurfaceDensities = DTM_fit(Z, Mage) * MetSurfaceDensities
if Type == 'Total':
# --- calculate V-band (550nm) optical depth for each star particle
tauVs_ISM = kappa * MetSurfaceDensities
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
elif Type == 'Pure-stellar':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 1.0
elif Type == 'Intrinsic':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 0.0
elif Type == 'Only-BC':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
else:
tauVs_ISM = None
tauVs_BC = None
fesc = None
ValueError(F"Undefined Type {Type}")
# --- calculate rest-frame Luminosity. In units of erg/s/Hz
for f in filters:
# --- calculate rest-frame flux of each object in nJy
Fnu = models.generate_Fnu_array(model, Masses, Ages, Metallicities,
tauVs_ISM, tauVs_BC, F, f,
fesc=fesc, log10t_BC=log10t_BC)
Fnus[f][begin[jj]: end[jj]] = Fnu
Fnus["coords"] = S_coords
Fnus["smls"] = S_sml
Fnus["begin"] = begin
Fnus["end"] = end
return Fnus
def lum(sim, kappa, tag, BC_fac, inp='FLARES', IMF='Chabrier_300', LF=True,
filters=('FAKE.TH.FUV',), Type='Total', log10t_BC=7.,
extinction='default', orientation="sim", masslim=None, nlim=None):
kinp = np.load('/cosma7/data/dp004/dc-payy1/my_files/'
'los/kernel_sph-anarchy.npz',
allow_pickle=True)
lkernel = kinp['kernel']
header = kinp['header']
kbins = header.item()['bins']
S_mass_ini, S_Z, S_age, S_los, G_Z, S_len, \
G_len, G_sml, S_sml, G_mass, S_coords, G_coords, \
S_vels, G_vels, S_mass, cops, S_bool, G_bool, \
begin, end, gbegin, gend, grpid, subgrpid = get_data(sim, tag, inp)
print("Got data, there are ", len(begin), "galaxies")
Lums = {f: np.zeros(len(S_mass), dtype=np.float64) for f in filters}
for f in filters:
Lums[f + "tauVs_ISM"] = np.zeros(len(S_mass), dtype=np.float64)
Lums[f + "tauVs_BC"] = np.zeros(len(S_mass), dtype=np.float64)
Lums[f + "log10t_BC"] = np.zeros(len(begin), dtype=np.float64)
model = models.define_model(
F'BPASSv2.2.1.binary/{IMF}') # DEFINE SED GRID -
if extinction == 'default':
model.dust_ISM = (
'simple', {'slope': -1.}) # Define dust curve for ISM
model.dust_BC = ('simple', {
'slope': -1.}) # Define dust curve for birth cloud component
elif extinction == 'Calzetti':
model.dust_ISM = ('Starburst_Calzetti2000', {''})
model.dust_BC = ('Starburst_Calzetti2000', {''})
elif extinction == 'SMC':
model.dust_ISM = ('SMC_Pei92', {''})
model.dust_BC = ('SMC_Pei92', {''})
elif extinction == 'MW':
model.dust_ISM = ('MW_Pei92', {''})
model.dust_BC = ('MW_Pei92', {''})
elif extinction == 'N18':
model.dust_ISM = ('MW_N18', {''})
model.dust_BC = ('MW_N18', {''})
else:
ValueError("Extinction type not recognised")
z = float(tag[5:].replace('p', '.'))
# Convert coordinates to physical
S_coords = S_coords / (1 + z)
G_coords = G_coords / (1 + z)
cops = cops / (1 + z)
# --- create rest-frame luminosities
F = flare.filters.add_filters(filters, new_lam=model.lam)
model.create_Lnu_grid(
F) # --- create new L grid for each filter. In units of erg/s/Hz
for jj in range(len(begin)):
# Extract values for this galaxy
sbool = S_bool[begin[jj]: end[jj]]
gbool = G_bool[gbegin[jj]: gend[jj]]
Masses = S_mass_ini[begin[jj]: end[jj]][sbool]
Ages = S_age[begin[jj]: end[jj]][sbool]
Metallicities = S_Z[begin[jj]: end[jj]][sbool]
gasMetallicities = G_Z[gbegin[jj]: gend[jj]][gbool]
gasSML = G_sml[gbegin[jj]: gend[jj]][gbool]
gasMasses = G_mass[gbegin[jj]: gend[jj]][gbool]
if masslim != None:
if np.sum(Masses) < masslim:
for f in filters:
Lums[f][begin[jj]: end[jj]] = np.nan
continue
if nlim != None:
if (end[jj] - begin[jj]) < nlim:
for f in filters:
Lums[f][begin[jj]: end[jj]] = np.nan
continue
if orientation == "sim":
starCoords = S_coords[:, begin[jj]: end[jj]].T[sbool]
gasCoords = G_coords[:, gbegin[jj]: gend[jj]].T[gbool]
MetSurfaceDensities = util.get_Z_LOS(starCoords, gasCoords,
gasMasses, gasMetallicities,
gasSML, (0, 1, 2),
lkernel, kbins)
S_coords[:, begin[jj]: end[jj]][:, sbool] = (starCoords - cops[:, jj]).T
G_coords[:, gbegin[jj]: gend[jj]][:, gbool] = (gasCoords - cops[:, jj]).T
elif orientation == "face-on":
starCoords = S_coords[:, begin[jj]: end[jj]][:, sbool].T - cops[:, jj]
gasCoords = G_coords[:, gbegin[jj]: gend[jj]][:, gbool].T - cops[:, jj]
gasVels = G_vels[gbegin[jj]: gend[jj], :][gbool]
# Get angular momentum vector
ang_vec = util.ang_mom_vector(gasMasses, gasCoords, gasVels)
# Rotate positions
starCoords = util.get_rotated_coords(ang_vec, starCoords)
gasCoords = util.get_rotated_coords(ang_vec, gasCoords)
S_coords[:, begin[jj]: end[jj]][:, sbool] = starCoords.T
MetSurfaceDensities = util.get_Z_LOS(starCoords, gasCoords,
gasMasses, gasMetallicities,
gasSML, (0, 1, 2),
lkernel, kbins)
elif orientation == "side-on":
starCoords = S_coords[:, begin[jj]: end[jj]][:, sbool].T - cops[:, jj]
gasCoords = G_coords[:, gbegin[jj]: gend[jj]][:, gbool].T - cops[:, jj]
gasVels = G_vels[gbegin[jj]: gend[jj], :][gbool]
# Get angular momentum vector
ang_vec = util.ang_mom_vector(gasMasses, gasCoords, gasVels)
# Rotate positions
starCoords = util.get_rotated_coords(ang_vec, starCoords)
gasCoords = util.get_rotated_coords(ang_vec, gasCoords)
S_coords[:, begin[jj]: end[jj]][:, sbool] = starCoords.T
MetSurfaceDensities = util.get_Z_LOS(starCoords, gasCoords,
gasMasses, gasMetallicities,
gasSML, (2, 0, 1),
lkernel, kbins)
else:
MetSurfaceDensities = None
print(orientation,
"is not an recognised orientation. "
"Accepted types are 'sim', 'face-on', or 'side-on'")
Mage = np.nansum(Masses * Ages) / np.nansum(Masses)
Z = np.nanmean(gasMetallicities)
MetSurfaceDensities = DTM_fit(Z, Mage) * MetSurfaceDensities
if Type == 'Total':
# --- calculate V-band (550nm) optical depth for each star particle
tauVs_ISM = kappa * MetSurfaceDensities
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
elif Type == 'Pure-stellar':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 1.0
elif Type == 'Intrinsic':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = np.zeros(len(Masses))
fesc = 0.0
elif Type == 'Only-BC':
tauVs_ISM = np.zeros(len(Masses))
tauVs_BC = BC_fac * (Metallicities / 0.01)
fesc = 0.0
else:
tauVs_ISM = None
tauVs_BC = None
fesc = None
ValueError(F"Undefined Type {Type}")
# --- calculate rest-frame Luminosity. In units of erg/s/Hz
for f in filters:
Lnu = models.generate_Lnu_array(model=model, Masses=Masses,
Ages=Ages,
Metallicities=Metallicities,
tauVs_ISM=tauVs_ISM,
tauVs_BC=tauVs_BC, F=F, f=f,
fesc=fesc, log10t_BC=log10t_BC)
Lums[f][begin[jj]: end[jj]][sbool] = Lnu
Lums[f + "tauVs_ISM"][begin[jj]: end[jj]][sbool] = tauVs_ISM
Lums[f + "tauVs_BC"][begin[jj]: end[jj]][sbool] = tauVs_BC
Lums[f + "log10t_BC"][jj] = log10t_BC
Lums[f][begin[jj]: end[jj]][~sbool] = np.nan
Lums[f + "tauVs_ISM"][begin[jj]: end[jj]][~sbool] = np.nan
Lums[f + "tauVs_BC"][begin[jj]: end[jj]][~sbool] = np.nan
Lums["coords"] = S_coords
Lums["gcoords"] = G_coords
Lums["grpid"] = grpid
Lums["subgrpid"] = subgrpid
Lums["smls"] = S_sml
Lums["masses"] = S_mass
Lums["gmasses"] = G_mass
Lums["S_age"] = S_age
Lums["S_Z"] = S_Z
Lums["G_Z"] = G_Z
Lums["nstar"] = S_len
Lums["begin"] = begin
Lums["end"] = end
Lums["gbegin"] = gbegin
Lums["gend"] = gend
Lums["S_bool"] = S_bool
Lums["G_bool"] = G_bool
return Lums # , S_len + G_len