def _get_simba_property(self,ptype,prop):
from readgadget import readsnap
snapfile = ('%s/%s'%(self.ds.fullpath,self.ds.basename))
# set up units coming out of pygr
prop_unit = {'mass':'Msun', 'pos':'kpccm', 'vel':'km/s', 'pot':'Msun * kpccm**2 / s**2', 'rho':'g / cm**3', 'sfr':'Msun / yr', 'u':'K', 'Dust_Masses':'Msun', 'bhmass':'Msun', 'bhmdot':'Msun / yr', 'hsml':'kpccm'}
# damn you little h!
if prop == 'mass' or prop == 'pos':
hfact = 1./self.ds.hubble_constant
elif prop == 'rho':
hfact = self.ds.hubble_constant**2
else:
hfact = 1.
# deal with differences in pygr vs. yt/caesar naming
if ptype == 'bh': ptype = 'bndry'
if prop == 'temperature': prop = 'u'
if prop == 'haloid' or prop == 'dustmass' or prop == 'aform' or prop == 'bhmass' or prop == 'bhmdot': prop = self.get_property_name(ptype, prop)
# read in the data
data = readsnap(snapfile, prop, ptype, units=1, suppress=1) * hfact
# set to doubles
if prop == 'HaloID' or prop == 'particle_index': # this fixes a bug in our Gizmo, that HaloID is output as a float!
data = data.astype(np.int64)
else:
data = data.astype(np.float32)
if prop in prop_unit.keys():
data = self.ds.arr(data, prop_unit[prop])
else:
data = self.ds.arr(data, '')
return data
def collect_group_IDs(obj, data_type, part_type, snap_dir):
"""Collates list of particle and associated group IDs for all specified objects.
Returns particle and group ID lists, and a hash list of indexes for particle IDs
corresponding to the starting index of each group.
Parameters
----------
obj : :class:`main.CAESAR`
Caesar object for which to collect group IDs
data_type : str
'halo', 'galaxy', or 'cloud'
part_type : str
Particle type
snap_dir : str
Path where snapshot files are located; if None, uses obj.simulation.fullpath
"""
# read in particle IDs
from readgadget import readsnap
if snap_dir is None:
#snapfile = obj.simulation.fullpath.decode('utf-8')+'/'+obj.simulation.basename.decode('utf-8')
snapfile = obj.simulation.fullpath.decode(
'utf-8') + '/' + obj.simulation.basename.decode('utf-8')
else:
snapfile = snap_dir + '/' + obj.simulation.basename.decode('utf-8')
all_pids = np.array(readsnap(snapfile, 'pid', part_type, suppress=1),
dtype=np.uint64)
from caesar.fubar_halo import plist_dict
if data_type == 'halo':
part_list = 'obj.halos[i].%s' % plist_dict[part_type]
ngroups = len(obj.halos)
elif data_type == 'galaxy':
part_list = 'obj.galaxies[i].%s' % plist_dict[part_type]
ngroups = len(obj.galaxies)
elif data_type == 'cloud':
part_list = 'obj.clouds[i].%s' % plist_dict[part_type]
ngroups = len(obj.clouds)
# count number of total particles in groups
npart = 0
for i in range(ngroups):
mylist = eval(part_list)
npart += len(mylist)
# fill particle and group ID lists
pids = np.zeros(npart, dtype=np.int64)
gids = np.zeros(npart, dtype=np.int32)
pid_hash = np.zeros(ngroups, dtype=np.int64)
count = 0
for i in range(ngroups):
mylist = eval(part_list)
pids[count:count + len(mylist)] = all_pids[mylist]
gids[count:count + len(mylist)] = np.full(len(mylist), i)
pid_hash[i] = count
count += len(mylist)
pid_hash = np.append(pid_hash, npart + 1)
return ngroups, pids, gids, pid_hash
def info(obj, snapFile, top=None, savetxt=False):
"""
Customized version to print more info on the CAESAR extracted galaxies.
Parameters
----------
obj : :class:`main.CAESAR`
Main CAESAR object.
top : int
Number of objects to print.
"""
from readgadget import readsnap
from yt2caesar import group_part_by_galaxy, get_partmasses_from_snapshot
group_list = obj.galaxies[:]
nobjs = len(group_list)
if top is None:
top = nobjs
elif top > nobjs:
top = nobjs
if obj.simulation.cosmological_simulation:
time = 'z=%0.3f' % obj.simulation.redshift
else:
time = 't=%0.3f' % obj.simulation.time
output = '##\n'
output += '## Largest %d Galaxies \n' % (top)
if hasattr(obj, 'data_file'): output += '## from: %s\n' % obj.data_file
output += '## %d @ %s' % (nobjs, time)
output += '##\n'
output += '##\n'
cnt = 1
# get molecular gas fraction of each particle from snapshot file
gfH2_p = readsnap(snapFile,'fH2','gas', units=1)
gas_p_m = get_partmasses_from_snapshot(snapFile, obj, ptype='gas')
output += '## ID Mstar Mgas MBH fedd SFR [Msun/yr] SFRSD [Msun/yr/kpc^2] SFRSD_r_stellar_half_mass [Msun/yr/kpc^2] gasSD [Msun/pc^2] r_baryon r_gas r_gas_half_mass r_stellar r_stellar_half_mass Z_sfrWeighted [/Zsun] Z_massWeighted [/Zsun] Z_stellar [/Zsun] T_gas_massWeighted T_gas_SFRWeighted fgas f_h2_fromSnap DGR nrho Central\t| Mhalo_parent HID\n'
output += '## ----------------------------------------------------------------------------------------\n'
h = obj.simulation.hubble_constant
bhmdot = readsnap(snapFile, 'BH_Mdot','bndry',suppress=1)*1.e10/h/3.08568e+16*3.155e7 # in Mo/yr
# debug mbh:
# mmm = [g.masses['bh'] for g in obj.galaxies]
# mmm[:10]
for ii, o in enumerate(group_list):
phm, phid = -1, -1
if o.halo is not None:
phm, phid = o.halo.masses['total'], o.halo.GroupID
try:
bhmdots = [bhmdot[k] for k in o.bhlist]
bm = o.masses['bh']
imax = np.argmax(bm)
try:
bm = bm[imax]
bmdot = bhmdots[imax] # only the massive BH particle matters.
except:
bm = bm
bmdot = bhmdots
frad = 0.1
mdot_edd = 4*np.pi*6.67e-8*1.673e-24/(frad*3.e10*6.65245e-25) * bm * 3.155e7 # in Mo/yr
fedd = bmdot / mdot_edd
fedd = fedd[0].value
except:
bm = 0
fedd = 0
# print bm, fedd
# import pdb; pdb.set_trace()
# Calculate mass-weighted f_h2 of each gal
gas_f_H2 = group_part_by_galaxy(gfH2_p, o, ptype='gas')
gas_m = group_part_by_galaxy(gas_p_m, o, ptype='gas')
output += ' %04d %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.2e %0.3f %0.3f %0.3f %0.2e %0.2e %0.3f %0.2e %.2e %.2e %s\t| %0.2e %d \n' % \
(o.GroupID, o.masses['stellar'], o.masses['gas'],
bm,
fedd,
o.sfr,
o.sfr/np.pi/o.radii['gas'].in_units('kpc')**2,
o.sfr/np.pi/o.radii['stellar_half_mass'].in_units('kpc')**2,
o.masses['gas']/np.pi/(o.radii['gas'].in_units('kpc')*1.e3)**2,
o.radii['baryon'].in_units('kpc'),
o.radii['gas'].in_units('kpc'),
o.radii['gas_half_mass'].in_units('kpc'),
o.radii['stellar'].in_units('kpc'),
o.radii['stellar_half_mass'].in_units('kpc'),
o.metallicities['sfr_weighted']/0.0134,
o.metallicities['mass_weighted']/0.0134,
o.metallicities['stellar']/0.0134,
o.temperatures['mass_weighted'],
o.temperatures['sfr_weighted'],
o.gas_fraction, # = Mgas / (Mg + Ms)
np.sum(gas_f_H2 * gas_m)/np.sum(gas_m), # mass-weighted f_h2
o.masses['gas']/o.masses['dust'],
o.local_number_density, o.central,
phm, phid)
cnt += 1
if cnt > top: break
# print(output)
if savetxt:
outputFileName = aux_filename(snapFile, top)
f = open(outputFileName, 'w')
f.write(output)
f.close()
return output, outputFileName
gal_sm = np.array([i.masses['stellar'].in_units('Msun') for i in sim.galaxies])
gal_sfr = np.array([i.sfr.in_units('Msun/yr') for i in sim.galaxies])
gal_ssfr = gal_sfr / gal_sm
gal_sm = np.log10(gal_sm)
gal_ssfr = np.log10(gal_ssfr)
with h5py.File(halflight_file, 'r') as f:
gal_rad = f['abs_' + model + '_' + wind + '_' +
snap][:] # these are in pkpc
gal_rad = np.sum(gal_rad, axis=0) / 3.
gal_ids = np.array([True for i in range(len(sim.galaxies))])
gal_ids = np.arange(len(gal_ids))[gal_ids]
# load in star particle data with readsnap
star_pos = readsnap(snapfile, 'pos', 'star', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
star_mass = readsnap(snapfile, 'mass', 'star', suppress=1,
units=1) / h # in Mo
star_vels = readsnap(snapfile, 'vel', 'star', suppress=1, units=0) # in km/s
star_tform = readsnap(snapfile, 'age', 'star', suppress=1,
units=1) # expansion times at time of formation
gas_pos = readsnap(snapfile, 'pos', 'gas', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
gas_mass = readsnap(snapfile, 'mass', 'gas', suppress=1, units=1) / h # in Mo
gas_sfr = readsnap(snapfile, 'sfr', 'gas', suppress=1, units=1) # in Mo/yr
gas_h1 = readsnap(snapfile,
'NeutralHydrogenAbundance',
'gas',
suppress=1,
xmin = -20. # [kpc]
xmax = 20. # [kpc]
Npixels = 100 #512
DR = 1. # kpc
z = obj.simulation.redshift
masses = np.array([i.masses['stellar'] for i in obj.galaxies])
sfr = np.array([i.sfr for i in obj.galaxies])
mask_mass = (masses > 4e10) & (masses < 6e10)
mask_sfr = (sfr > 0.5) & (sfr < 2.5)
#mw_gal_no = np.arange(0, len(masses))[mask_mass*mask_sfr]
mw_gal_no = np.arange(0, len(masses))[mask_mass]
star_positions = readsnap(snap, 'pos', 'star', suppress=1, units=1) / (1.+z)
star_vels = readsnap(snap, 'vel', 'star', suppress=1, units=0)
star_mass = readsnap(snap, 'mass', 'star', suppress=1, units=1) / (h*10**7.)
names = ['edge_on', 'face_on']
vecs = [np.array([0,1,0]), np.array([0,0,1])]
faceon = np.zeros((len(obj.galaxies), 5))
edgeon = np.zeros((len(obj.galaxies), 5))
b_t = np.zeros(len(obj.galaxies))
for i in mw_gal_no:
print 'galaxy: ' + str(i)
slist = obj.galaxies[i].slist
gal_mass = obj.galaxies[i].masses['stellar'].in_units('Msun')
gal_pos = obj.galaxies[i].pos.in_units('kpc/h')
def simba_to_pd(galnames,
raw_sim_dir,
raw_sim_name_prefix,
caesar_dir,
name_prefix,
redshiftFile,
d_data,
startGAL=None,
endGAL=None,
debugplotgas=False,
R_max=20.0,
verbose=False,
debug=False):
"""
Write out useful fields gas, stars, DM particles of the selected galaxies into DataFrames
Parameters
----------
galnames: str or list of string
if it's a simple str, it's a file that stores the output from return from select_SFgal_from_simba()
if it's a list of str, it's output from select_SFgal_from_simba()
raw_sim_dir: string
where to look for raw snapshot files
raw_sim_name_prefix: string
prefix to the speciifc volume and resolution of snapshots we are looking
caesar_dir: str
path to the caesar output files
name_prefix: str
predix to file of caesar outputs
redshiftFile: str
where to look for the redshift info for this particular set of snapshots
d_data: str
directory location to save dataframe files
startGAL: None or int
snapshot number to begin extraction. Use to pseudo-parallelized things
startGAL <= GAL < endGAL
endGAL: None or int
snapshot number to end extraction. Use to pseudo-parallelized things
plotgas: bool
whether or not to plot gas distribution of galaxy. Uesful for e.g., looking at the galaxy position and see if it might be the COM of two overlapping galaxies - see Romeel's email on Apr 4th, 2019.
R_max: float
physical kpc for projection plot
Returns
-------
galnames_selected: list of string
galaxies names indicating the halo ID, snapshot number, and galaxy ID (numbered based on some predefined criterion)
zreds_selected: numpy array of float
redshifts of galaxies
"""
try:
import cPickle as pickle
except:
import _pickle as pickle
import caesar
import yt
import numpy as np
import pandas as pd
import os
from readgadget import readsnap
kpc2m = 3.085677580666e19
resort = False
# Save the names and redshift for the galaxies that we finally decide to save in DataFrames:
galnames_selected = []
zreds_selected = np.array([])
if type(galnames) is str:
try:
with open(galnames, 'r') as f:
galnames = pickle.load(f)
except:
pass
try:
print(galnames['halo'].values, galnames['snap'].values,
galnames['GAL'].values, galnames['SFR'].values)
except TypeError:
galnames = galnames[0]
if (sorted(galnames['snap'].values) == galnames['snap'].values
).all() == False:
# then we have to sort galnames by 'snap'
galnames = galnames.sort_values(
['snap', 'SFR'], ascending=[False, False]).reset_index(
drop=False) # drop: avoid old index being added as a column
resort = True
snap_hold = []
for num, (halo, snap, GAL, sfr) in enumerate(
zip(galnames['halo'].values, galnames['snap'].values,
galnames['GAL'].values, galnames['SFR'].values)):
if num == 0:
snap_hold = snap
s, h, obj, ds, zred = define_ds(snap, raw_sim_dir,
raw_sim_name_prefix, caesar_dir,
name_prefix, redshiftFile)
# get H2 fraction from snapfile, instead of from YT sphere - faster way to weed out galaxies that are too small/with too few dense gas particles.
snapFile = raw_sim_dir + raw_sim_name_prefix + '{:0>3}'.format(
int(snap)) + '.hdf5'
gfH2 = readsnap(snapFile, 'fH2', 'gas')
gas_p_m = get_partmasses_from_snapshot(snapFile, obj, ptype='gas')
else:
if snap != snap_hold:
s, h, obj, ds, zred = define_ds(snap, raw_sim_dir,
raw_sim_name_prefix,
caesar_dir, name_prefix,
redshiftFile)
snap_hold = snap
# if we have sorted galnames by ('snap', SFR of each snap), we have to do so for obj too.
if resort:
gal = obj.galaxies
obj.galaxies = [gal[i] for i in galnames.index.values]
# if we want to split up exection of this script into multiple nodes.
if startGAL is None:
startGAL = 0
else:
startGAL = int(startGAL)
if endGAL is None:
endGAL = len(galnames.index)
else:
endGAL = int(endGAL)
assert startGAL < len(galnames.index)
assert endGAL <= len(galnames.index)
assert startGAL < endGAL
if startGAL <= GAL < endGAL:
print(
'\nNow looking at galaxy # %s with parent halo ID %s in snapshot %s at z = %s'
% (int(GAL), int(halo), int(snap), zred))
print('Creating galaxy name:')
galname = 'h' + str(int(halo)) + '_s' + \
str(int(snap)) + '_G' + str(int(GAL))
print(galname)
galaxy = obj.galaxies[GAL]
# Exclude galaxies based on global properties to speed things up. TO BE IMPLEMENTED
if galaxy.sfr < 0.1:
print("SFR too low.. Skipping")
continue
galaxy_fH2 = np.array([gfh2[k] for k in obj.galaxies.glist])
assert len(galaxy_fH2) == len(galaxy.masses['gas'])
if (galaxy.masses['gas'] * galaxy_fH2).sum() <= 1.e5:
print("Dense gas mass less than 10^5 Msun.. Skipping")
continue
if len(galaxy.slist) < 64 or len(galaxy.glist) < 64:
print(
"Too few star particles or gas particles, unlikely to be real galaxy or useful for our purpose"
)
continue
if galaxy.masses['gas'] == 0.0 or galaxy.masses['stellar'] == 0.0:
# then don't bother getting any info on this galaxy
if galaxy.masses['gas'] == 0.0:
print("Don't bother with this galaxy, it has no gas mass.")
elif galaxy.masses['stellar'] == 0.0:
print(
"Don't bother with this galaxy, it has no stellar mass."
)
continue
simgas_path = (d_data +
'particle_data/sim_data/z' + '{:.2f}').format(
float(zred)) + '_' + galname + '_sim.gas'
simstar_path = (d_data +
'particle_data/sim_data/z' + '{:.2f}').format(
float(zred)) + '_' + galname + '_sim.star'
simdm_path = (d_data +
'particle_data/sim_data/z' + '{:.2f}').format(
float(zred)) + '_' + galname + '_sim.dm'
if not os.path.exists(simgas_path) and not os.path.exists(
simstar_path) and not os.path.exists(simdm_path):
# Get location and radius for each galaxy belonging to this haloID:
loc = galaxy.pos # .in_units('unitary')
R_gal = galaxy.radius # kpccm, i.e., co-moving
# print(galaxy.radii)
print('Cut out a sphere with radius %s, %s' %
(R_gal, R_gal.in_units('kpc')))
sphere = ds.sphere(loc, R_gal)
gas_pos = sphere['PartType0', 'Coordinates'].in_units('kpc')
print('%s SPH particles' % len(gas_pos))
star_pos_all = sphere['PartType4',
'Coordinates'].in_units('kpc')
print('%s Star particles' % len(star_pos_all))
if debug:
print("List all stuff inside the raw sim .hdf5")
rawSim = raw_sim_dir + raw_sim_name_prefix + \
'{:>03}'.format(int(snap)) + '.hdf5'
os.system('h5ls -r ' + rawSim)
print("")
print(ds.field_list)
if len(gas_pos) > 0 and len(star_pos_all) > 0:
print('Extracting all gas particle properties...')
gas_pos = gas_pos - loc
# rotation to ensure that the galaxies lie in the xy-plane. That makes it easier to visualize later, and you can always add random viewing angles later as well.
gas_pos = caesar.utils.rotator(
gas_pos, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
gas_posx, gas_posy, gas_posz = gas_pos[:,
0].d, gas_pos[:,
1].d, gas_pos[:,
2].d
gas_vel = sphere['PartType0', 'Velocities'].in_cgs() / 1.e5
gas_vel = caesar.utils.rotator(
gas_vel, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
gas_velx, gas_vely, gas_velz = gas_vel[:,
0].d, gas_vel[:,
1].d, gas_vel[:,
2].d
print("gas_velx length: ", len(gas_velx))
gas_densities = sphere['PartType0', 'Density'].in_cgs()
gas_f_H2 = sphere['PartType0', 'FractionH2']
gas_f_neu = sphere['PartType0', 'NeutralHydrogenAbundance']
gas_m = sphere['PartType0', 'Masses'].in_units('Msun')
# electrons per Hydrogen atom (max: 1.15)
gas_x_e = sphere['PartType0', 'ElectronAbundance']
# ionized gas mass fraction (because we don't trust
# NeutralHydrogenAbundance -- which only includes atomic gas but not moleuclar)
# At the end, calculated from
gas_f_ion = gas_x_e / max(gas_x_e)
gas_f_HI = 1 - gas_f_ion
print(
'\nChecking molecular gas mass fraction from simulation:'
)
print('%.3s %% \n' %
(np.sum(gas_m * gas_f_H2) / np.sum(gas_m) * 100.))
# Tk
gas_Tk = sphere['PartType0', 'Temperature']
gas_h = sphere['PartType0',
'SmoothingLength'].in_units('kpc') # Tk
# Msun/yr
gas_SFR = sphere['PartType0', 'StarFormationRate']
# gas_SFR = galaxy.sfr
gas_Z = sphere['PartType0', 'Metallicity_00'].d / \
0.0134 # from RD
gas_a_He = sphere['PartType0', 'Metallicity_01'].d
gas_a_C = sphere['PartType0', 'Metallicity_02'].d
gas_a_N = sphere['PartType0', 'Metallicity_03'].d
gas_a_O = sphere['PartType0', 'Metallicity_04'].d
gas_a_Ne = sphere['PartType0', 'Metallicity_05'].d
gas_a_Mg = sphere['PartType0', 'Metallicity_06'].d
gas_a_Si = sphere['PartType0', 'Metallicity_07'].d
gas_a_S = sphere['PartType0', 'Metallicity_08'].d
gas_a_Ca = sphere['PartType0', 'Metallicity_09'].d
gas_a_Fe = sphere['PartType0', 'Metallicity_10'].d
print('Extracting all star particle properties...')
star_pos = star_pos_all - loc
star_pos = caesar.utils.rotator(
star_pos, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
star_posx, star_posy, star_posz = star_pos[:,
0].d, star_pos[:,
1].d, star_pos[:,
2].d
star_vel = sphere['PartType4', 'Velocities'].in_cgs() / 1e5
star_vel = caesar.utils.rotator(
star_vel, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
star_velx, star_vely, star_velz = star_vel[:,
0].d, star_vel[:,
1].d, star_vel[:,
2].d
star_m = sphere['PartType4', 'Masses'].in_units('Msun')
# star_m = galaxy.masses['stellar']
star_a_C = sphere['PartType4', 'Metallicity_02'].d
star_a_O = sphere['PartType4', 'Metallicity_04'].d
star_a_Si = sphere['PartType4', 'Metallicity_07'].d
star_a_Fe = sphere['PartType4', 'Metallicity_10'].d
star_Z = sphere['PartType4', 'Metallicity_00'].d / \
0.0134 # from RD
print('Info for this snapshot:')
omega_baryon = obj.simulation.omega_baryon
omega_matter = obj.simulation.omega_matter
hubble_constant = obj.simulation.hubble_constant
print('Omega baryon: %s' % omega_baryon)
print('Omega matter: %s' % omega_matter)
print('Hubble constant: %s' % hubble_constant)
print('XH: %s' % obj.simulation.XH)
current_time = ds.current_time.in_units('yr') / 1.e6 # Myr
# in scale factors, do as with Illustris
star_formation_a = sphere['PartType4',
'StellarFormationTime'].d
star_formation_z = 1. / star_formation_a - 1
# Code from yt project (yt.utilities.cosmology)
star_formation_t = 2.0 / 3.0 / np.sqrt(
1 - omega_matter) * np.arcsinh(
np.sqrt((1 - omega_matter) / omega_matter) /
np.power(1 + star_formation_z, 1.5)) / (
hubble_constant) # Mpc*s/(100*km)
star_formation_t *= kpc2m / 100. / (1e6 * 365.25 * 86400
) # Myr
star_age = current_time.d - star_formation_t
print('Extracting all DM particle properties...')
dm_pos_all = sphere['PartType1',
'Coordinates'].in_units('kpc')
dm_pos = dm_pos_all - loc
dm_pos = caesar.utils.rotator(
dm_pos, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
dm_posx, dm_posy, dm_posz = dm_pos[:,
0].d, dm_pos[:,
1].d, dm_pos[:,
2].d
dm_vel = sphere['PartType1', 'Velocities'].in_cgs() / 1e5
dm_vel = caesar.utils.rotator(
dm_vel, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
dm_velx, dm_vely, dm_velz = dm_vel[:,
0].d, dm_vel[:,
1].d, dm_vel[:,
2].d
dm_m = sphere['PartType1', 'Masses'].in_units('Msun')
print('Extracting all BH particle properties...')
BH_pos = sphere['PartType5',
'Coordinates'].in_units('kpc') - loc
print('%s BH particles' % len(BH_pos))
if len(BH_pos) > 0:
BH_pos = caesar.utils.rotator(
BH_pos, galaxy.rotation_angles['ALPHA'],
galaxy.rotation_angles['BETA'])
BH_posx, BH_posy, BH_posz = BH_pos[:,
0].d, BH_pos[:,
1].d, BH_pos[:,
2].d
# BH mass
# which grows through accretion and mergers w/ other BHs
BH_m = sphere['PartType5', 'BH_Mass'].in_units('Msun')
# dynamical mass, which enters into gravity calculation
BH_m2 = sphere['PartType5', 'Masses'].in_units('Msun')
BH_mdot = sphere['PartType5', 'BH_Mdot']
# the one that actually matters is the most massive BH particle
idx = np.where(BH_m == BH_m.max())
BH_m = BH_m[idx]
BH_mdot = BH_mdot[idx]
print(BH_m, BH_mdot)
simbh = pd.DataFrame({
'mBH_Msun': BH_m,
'mdot': BH_mdot
})
simbh.to_pickle(d_data + 'particle_data/sim_data/z' +
'{:.2f}'.format(float(zred)) + '_' +
galname + '_sim.bh')
# Put into dataframes:
simgas = pd.DataFrame({
'x': gas_posx,
'y': gas_posy,
'z': gas_posz,
'vx': gas_velx,
'vy': gas_vely,
'vz': gas_velz,
'SFR': gas_SFR,
'Z': gas_Z,
'nH': gas_densities,
'Tk': gas_Tk,
'h': gas_h,
'f_HI1': gas_f_HI, # atomic and molecular H
'f_neu': gas_f_neu, # atomic H
'f_H21': gas_f_H2,
'm': gas_m,
'a_He': gas_a_He,
'a_C': gas_a_C,
'a_N': gas_a_N,
'a_O': gas_a_O,
'a_Ne': gas_a_Ne,
'a_Mg': gas_a_Mg,
'a_Si': gas_a_Si,
'a_S': gas_a_S,
'a_Ca': gas_a_Ca,
'a_Fe': gas_a_Fe
})
simstar = pd.DataFrame({
'x': star_posx,
'y': star_posy,
'z': star_posz,
'vx': star_velx,
'vy': star_vely,
'vz': star_velz,
'Z': star_Z,
'm': star_m,
'age': star_age
})
simdm = pd.DataFrame({
'x': dm_posx,
'y': dm_posy,
'z': dm_posz,
'vx': dm_velx,
'vy': dm_vely,
'vz': dm_velz,
'm': dm_m
})
# Calculate approximate 100 Myr average of SFR for this galaxy
m_star = simstar['m'].values
age_star = simstar['age'].values
SFR_avg = sum(m_star[age_star < 100]) / 100.e6
print(
'Estimated SFR for this galaxy averaged over past 100 Myr: '
+ str(SFR_avg))
print('SFR in simulation: %s' % galaxy.sfr)
print('SFR for parent halo: %s' % galaxy.halo.sfr)
print('Stellar mass: %s Msun' % np.sum(m_star))
print('Dark matter mass: %s ' % np.sum(dm_m))
print('Saving galaxy data as DataFrames in {}').format(
d_data)
# replace w/ this line if we decide to merge this func to load_module.py and call via parameters_zx.txt
# print('Saving galaxy data as DataFrames in {}, as defined in __init__.py').format(d_data)
savepath = d_data + 'particle_data/sim_data/'
if not os.path.exists(savepath):
os.makedirs(savepath)
simgas.to_pickle(simgas_path)
simstar.to_pickle(simstar_path)
simdm.to_pickle(simdm_path)
if plotgas:
import matplotlib.pyplot as plt
from mpl_toolkits.axes_grid1 import AxesGrid
# projection plot
plt.close('all')
savepath = 'plots/sims/'
if not os.path.exists(savepath):
os.makedirs(savepath)
ppp = yt.ProjectionPlot(
ds,
0,
[('gas', 'density')],
center=sphere.center.value,
width=(R_max, 'kpc'),
# center='c',
weight_field='density')
try:
ppp.annotate_timestamp(corner='upper_left',
redshift=True,
time=False,
draw_inset_box=True)
#p.annotate_scale(corner='upper_right')
ppp.annotate_particles((R_max, 'kpc'),
p_size=20,
ptype='PartType5',
minimum_mass=1.e7)
except:
pass
filename = 'z' + '{:.2f}'.format(
float(zred)) + '_' + galname + '_gas.pdf'
p.save(os.path.join(savepath, filename))
elif len(gas_pos) == 0 or len(star_pos_all) == 0:
if len(star_pos_all) == 0:
print(
"Not saving this galaxy {:} because it has no stellar mass..."
).format(galname)
elif len(gas_pos) == 0:
print(
"Not saving this galaxy {:} because it has no gas mass..."
).format(galname)
if debug:
import matplotlib.pyplot as plt
from mpl_toolkits.axes_grid1 import AxesGrid
# projection plot
plt.close('all')
savepath = 'plots/sims/'
if not os.path.exists(savepath):
os.makedirs(savepath)
filename = 'z' + '{:.2f}'.format(
float(zred)) + '_' + galname + '_gas.pdf'
if not os.path.isfile(filename):
print("Plotting gas particles...")
ppp = yt.ProjectionPlot(
ds,
0,
[('gas', 'density')],
center=sphere.center.value,
width=(R_max, 'kpc'),
# center='c',
weight_field='density')
try:
ppp.annotate_timestamp(corner='upper_left',
redshift=True,
time=False,
draw_inset_box=True)
#p.annotate_scale(corner='upper_right')
ppp.annotate_particles((R_max, 'kpc'),
p_size=20,
ptype='PartType5',
minimum_mass=1.e7)
except:
pass
ppp.save(os.path.join(savepath, filename))
continue
else:
print("Skipping... Already extracted...")
galnames_selected.append(galname)
zreds_selected = np.append(zreds_selected, float(zred))
return galnames_selected, zreds_selected
gal_sfr = np.array([i.sfr.in_units('Msun/yr') for i in sim.galaxies])
gal_ssfr = gal_sfr / gal_sm
with h5py.File(halflight_file, 'r') as f:
gal_rad = f[model + '_' + wind + '_' + snap +
'_halflight'][:] # these are in pkpc
gal_rad = np.sum(gal_rad, axis=0) / 3.
#gal_rad = np.array([i.radii['stellar_half_mass'].in_units('kpc') for i in sim.galaxies])
gal_sm = np.log10(gal_sm[gal_ids * gal_cent])
gal_ssfr = np.log10(gal_ssfr[gal_ids * gal_cent])
gal_rad = gal_rad[gal_ids * gal_cent]
gal_ids = np.arange(len(gal_ids))[gal_ids * gal_cent]
# load in star particle data with readsnap
star_pos = readsnap(snapfile, 'pos', 'star', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
star_mass = readsnap(snapfile, 'mass', 'star', suppress=1,
units=1) / h # in Mo
gas_pos = readsnap(snapfile, 'pos', 'gas', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
gas_mass = readsnap(snapfile, 'mass', 'gas', suppress=1, units=1) / h # in Mo
gas_temp = readsnap(snapfile, 'u', 'gas', suppress=1, units=1)
bh_pos = readsnap(snapfile, 'pos', 'bndry', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
no_gals = np.zeros(len(bin_labels))
for j, m in enumerate(masks):
sim = caesar.load(infile,LoadHalo=False)
redshift = np.round(sim.simulation.redshift,3)
h = sim.simulation.hubble_constant
mygals = sim.galaxies
print('Doing z=',redshift,'snapshot',snapfile,'with',len(mygals),'galaxies.')
# read in galaxy info
ids = np.asarray([i.GroupID for i in mygals])
central = np.asarray([i.central for i in mygals])
ms = np.asarray([i.masses['stellar'] for i in mygals])
mbh = np.asarray([i.masses['bh'] for i in mygals])
sfr = np.asarray([i.sfr for i in mygals])
# read in particle info
sm = readsnap(snapfile,'mass','star',units=1,suppress=1)/h # Mo
sp = readsnap(snapfile,'pos','star',units=1,suppress=1)/(1+redshift)/h # pkpc
gm = readsnap(snapfile,'mass','gas',units=1,suppress=1)/h # Mo
gp = readsnap(snapfile,'pos','gas',units=1,suppress=1)/(1+redshift)/h # pkpc
gsfr = readsnap(snapfile,'sfr','gas',units=1,suppress=1) # Mo/yr
# compute rhalf
rhalf = np.zeros([3,len(mygals)])
if (MODEL == 'm100n1024') & (SNAP in ['105', '151']):
params, mags = get_mags_band(loserfile, mtype, band, only_mtype=True, verbose=True)
where = int(np.where(params['bands'] == band)[0])
mags = mags.transpose()[where]
else:
params, mags = get_mags_band(loserfile, mtype, band, verbose=True)
allL = absmag_to_lum(mags)
gal_sm = np.array(
[i.masses['stellar'].in_units('Msun') for i in sim.central_galaxies])
gal_sfr = np.array([i.sfr.in_units('Msun/yr') for i in sim.central_galaxies])
gal_ssfr = np.log10(gal_sfr / gal_sm)
gal_rad = np.array([
i.radii['stellar_half_mass'].in_units('kpc') for i in sim.central_galaxies
])
richness = np.log10(gal_h1m / gal_sm)
mass_mask = np.log10(gal_sm) > 9.
n_mask = np.array([(len(i.glist) > n_min) for i in sim.central_galaxies])
mask = mass_mask * n_mask * (gal_h1m > 0.)
mask = mass_mask * (gal_h1m > 0.)
gal_ids = np.arange(len(sim.central_galaxies))[mask]
gas_pos = readsnap(snapfile, 'pos', 'gas', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
gas_mass = readsnap(snapfile, 'mass', 'gas', suppress=1, units=1) / h # in Mo
gas_h1 = readsnap(snapfile,
'NeutralHydrogenAbundance',
'gas',
suppress=1,
units=1)
bh_pos = readsnap(snapfile, 'pos', 'bndry', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
h1_radii = np.zeros(len(gal_ids))
for i in range(len(gal_ids)):
print('\n')
gal_ssfr = gal_sfr / gal_sm
# load in half light radii:
with h5py.File(halflight_file, 'r') as f:
gal_rad = f[model + '_' + wind + '_' + snap +
'_halflight'][:] # these are in pkpc
gal_rad = np.sum(gal_rad, axis=0) / 3.
# select central galaxies:
gal_sm = np.log10(gal_sm[gal_ids * gal_cent])
gal_ssfr = np.log10(gal_ssfr[gal_ids * gal_cent])
gal_rad = gal_rad[gal_ids * gal_cent]
gal_ids = np.arange(len(gal_ids))[gal_ids * gal_cent]
# load in star particle data with readsnap
star_pos = readsnap(snapfile, 'pos', 'star', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
star_tform = readsnap(snapfile, 'age', 'star', suppress=1,
units=1) # expansion times at time of formation
star_mass = readsnap(snapfile, 'mass', 'star', suppress=1,
units=1) / h # in Mo
bh_pos = readsnap(snapfile, 'pos', 'bndry', suppress=1, units=1) / (
h * (1. + redshift)) # in kpc
no_gals = np.zeros(len(bin_labels))
for j, m in enumerate(masks):
# for each mass bin make a mass mask and select those galaxies:
print '\n'
