def test_absorption_spectrum_non_cosmo(self):
"""
This test generates an absorption spectrum from a simple light ray on a
grid dataset
"""
lr = LightRay(COSMO_PLUS_SINGLE)
ray_start = [0,0,0]
ray_end = [1,1,1]
lr.make_light_ray(start_position=ray_start, end_position=ray_end,
fields=[('gas', 'temperature'),
('gas', 'density'),
('gas', 'H_p0_number_density')],
data_filename='lightray.h5')
sp = AbsorptionSpectrum(1200.0, 1300.0, 10001)
my_label = 'HI Lya'
field = ('gas', 'H_p0_number_density')
wavelength = 1215.6700 # Angstromss
f_value = 4.164E-01
gamma = 6.265e+08
mass = 1.00794
sp.add_line(my_label, field, wavelength, f_value,
gamma, mass, label_threshold=1.e10)
filename = "spectrum.h5"
wavelength, flux = sp.make_spectrum('lightray.h5',
output_file=filename,
output_absorbers_file='lines.txt',
use_peculiar_velocity=True)
return filename
def test_absorption_spectrum_with_continuum(self):
"""
This test generates an absorption spectrum from a simple light ray on a
grid dataset and adds Lyman alpha and Lyman continuum to it
"""
ds = load(ISO_GALAXY)
lr = LightRay(ds)
ray_start = ds.domain_left_edge
ray_end = ds.domain_right_edge
lr.make_light_ray(
start_position=ray_start,
end_position=ray_end,
fields=['temperature', 'density', 'H_number_density'],
data_filename='lightray.h5')
sp = AbsorptionSpectrum(800.0, 1300.0, 5001)
my_label = 'HI Lya'
field = 'H_number_density'
wavelength = 1215.6700 # Angstromss
f_value = 4.164E-01
gamma = 6.265e+08
mass = 1.00794
sp.add_line(my_label,
field,
wavelength,
f_value,
gamma,
mass,
label_threshold=1.e10)
my_label = 'Ly C'
field = 'H_number_density'
wavelength = 912.323660 # Angstroms
normalization = 1.6e17
index = 3.0
sp.add_continuum(my_label, field, wavelength, normalization, index)
filename = "spectrum.h5"
wavelength, flux = sp.make_spectrum('lightray.h5',
output_file=filename,
line_list_file='lines.txt',
use_peculiar_velocity=True)
return filename
def test_absorption_spectrum_cosmo(self):
"""
This test generates an absorption spectrum from a compound light ray on a
grid dataset
"""
lr = LightRay(COSMO_PLUS, 'Enzo', 0.0, 0.03)
lr.make_light_ray(
seed=1234567,
fields=['temperature', 'density', 'H_number_density'],
data_filename='lightray.h5')
sp = AbsorptionSpectrum(900.0, 1800.0, 10000)
my_label = 'HI Lya'
field = 'H_number_density'
wavelength = 1215.6700 # Angstromss
f_value = 4.164E-01
gamma = 6.265e+08
mass = 1.00794
sp.add_line(my_label,
field,
wavelength,
f_value,
gamma,
mass,
label_threshold=1.e10)
my_label = 'HI Lya'
field = 'H_number_density'
wavelength = 912.323660 # Angstroms
normalization = 1.6e17
index = 3.0
sp.add_continuum(my_label, field, wavelength, normalization, index)
filename = "spectrum.h5"
wavelength, flux = sp.make_spectrum('lightray.h5',
output_file=filename,
line_list_file='lines.txt',
use_peculiar_velocity=True)
return filename
def test_absorption_spectrum_fits(self):
"""
This test generates an absorption spectrum and saves it as a fits file.
"""
lr = LightRay(COSMO_PLUS_SINGLE)
ray_start = [0, 0, 0]
ray_end = [1, 1, 1]
lr.make_light_ray(
start_position=ray_start,
end_position=ray_end,
fields=['temperature', 'density', 'H_number_density'],
data_filename='lightray.h5')
sp = AbsorptionSpectrum(900.0, 1800.0, 10000)
my_label = 'HI Lya'
field = 'H_number_density'
wavelength = 1215.6700 # Angstromss
f_value = 4.164E-01
gamma = 6.265e+08
mass = 1.00794
sp.add_line(my_label,
field,
wavelength,
f_value,
gamma,
mass,
label_threshold=1.e10)
my_label = 'HI Lya'
field = 'H_number_density'
wavelength = 912.323660 # Angstroms
normalization = 1.6e17
index = 3.0
sp.add_continuum(my_label, field, wavelength, normalization, index)
wavelength, flux = sp.make_spectrum('lightray.h5',
output_file='spectrum.fits',
line_list_file='lines.txt',
use_peculiar_velocity=True)
def test_equivalent_width_conserved(self):
"""
This tests that the equivalent width of the optical depth is conserved
regardless of the bin width employed in wavelength space.
Unresolved lines should still deposit optical depth into the spectrum.
"""
lr = LightRay(COSMO_PLUS_SINGLE)
ray_start = [0, 0, 0]
ray_end = [1, 1, 1]
lr.make_light_ray(
start_position=ray_start,
end_position=ray_end,
fields=['temperature', 'density', 'H_number_density'],
data_filename='lightray.h5')
my_label = 'HI Lya'
field = 'H_number_density'
wave = 1215.6700 # Angstromss
f_value = 4.164E-01
gamma = 6.265e+08
mass = 1.00794
lambda_min = 1200
lambda_max = 1300
lambda_bin_widths = [1e-3, 1e-2, 1e-1, 1e0, 1e1]
total_tau = []
for lambda_bin_width in lambda_bin_widths:
n_lambda = ((lambda_max - lambda_min) / lambda_bin_width) + 1
sp = AbsorptionSpectrum(lambda_min=lambda_min,
lambda_max=lambda_max,
n_lambda=n_lambda)
sp.add_line(my_label, field, wave, f_value, gamma, mass)
wavelength, flux = sp.make_spectrum('lightray.h5')
total_tau.append((lambda_bin_width * sp.tau_field).sum())
# assure that the total tau values are all within 1e-3 of each other
for tau in total_tau:
assert_almost_equal(tau, total_tau[0], 3)
def test_absorption_spectrum_with_zero_field(self):
"""
This test generates an absorption spectrum with some
particle dataset
"""
ds = load(FIRE)
lr = LightRay(ds)
# Define species and associated parameters to add to continuum
# Parameters used for both adding the transition to the spectrum
# and for fitting
# Note that for single species that produce multiple lines
# (as in the OVI doublet), 'numLines' will be equal to the number
# of lines, and f,gamma, and wavelength will have multiple values.
HI_parameters = {
'name': 'HI',
'field': 'H_number_density',
'f': [.4164],
'Gamma': [6.265E8],
'wavelength': [1215.67],
'mass': 1.00794,
'numLines': 1,
'maxN': 1E22,
'minN': 1E11,
'maxb': 300,
'minb': 1,
'maxz': 6,
'minz': 0,
'init_b': 30,
'init_N': 1E14
}
species_dicts = {'HI': HI_parameters}
# Get all fields that need to be added to the light ray
fields = [('gas', 'temperature')]
for s, params in species_dicts.items():
fields.append(params['field'])
# With a single dataset, a start_position and
# end_position or trajectory must be given.
# Trajectory should be given as (r, theta, phi)
lr.make_light_ray(start_position=ds.arr([0., 0., 0.], 'unitary'),
end_position=ds.arr([1., 1., 1.], 'unitary'),
solution_filename='test_lightraysolution.txt',
data_filename='test_lightray.h5',
fields=fields)
# Create an AbsorptionSpectrum object extending from
# lambda = 900 to lambda = 1800, with 10000 pixels
sp = AbsorptionSpectrum(900.0, 1400.0, 50000)
# Iterate over species
for s, params in species_dicts.items():
# Iterate over transitions for a single species
for i in range(params['numLines']):
# Add the lines to the spectrum
sp.add_line(s,
params['field'],
params['wavelength'][i],
params['f'][i],
params['Gamma'][i],
params['mass'],
label_threshold=1.e10)
# Make and save spectrum
wavelength, flux = sp.make_spectrum('test_lightray.h5',
output_file='test_spectrum.h5',
line_list_file='test_lines.txt',
use_peculiar_velocity=True)
def make_spectrum(self,
ray,
lines='all',
output_file=None,
use_peculiar_velocity=True,
observing_redshift=0.0,
ly_continuum=True,
store_observables=False,
min_tau=1e-3,
njobs="auto"):
"""
Make a spectrum from ray data depositing the desired lines. Make sure
to pass this function a LightRay object and potentially also a list of
strings representing what lines you'd like to actually have be
deposited in your final spectrum.
**Parameters**
:ray: string or dataset
Ray dataset filename or a loaded ray dataset
:lines: list of strings
List of strings that determine which lines will be added
to the spectrum. List can include things like "C", "O VI",
or "Mg II ####", where #### would be the integer wavelength
value of the desired line. If set to 'all', includes all lines
in LineDatabase set in SpectrumGenerator.
Default: 'all'
:output_file: optional, string
Filename of output if you wish to save the spectrum immediately
without any further processing. File formats are chosen based on the
filename extension. ".h5" for HDF5, ".fits" for FITS,
and everything else is ASCII. Equivalent of calling
:class:`~trident.SpectrumGenerator.save_spectrum`.
Default: None
:use_peculiar_velocity: optional, bool
If True, include the effects of doppler redshift of the gas
in shifting lines in the final spectrum.
Default: True
:observing_redshift: optional, float
This is the value of the redshift at which the observer of this
spectrum exists. In most cases, this will be a redshift of 0.
Default: 0.
:ly_continuum: optional, boolean
If any H I lines are used in the line list, this assures a
Lyman continuum will be included in the spectral generation.
Lyman continuum begins at final Lyman line deposited (Ly 39 =
912.32 A) not at formal Lyman Limit (911.76 A) so as to not have
a gap between final Lyman lines and continuum. Uses power law
of index 3 and normalization to match opacity of final Lyman lines.
Default: True
:store_observables: optional, boolean
If set to true, observable properties for each cell in the light
ray will be saved for each line in the line list. Properties
include the column density, tau, thermal b, and the wavelength
where tau was deposited. Best applied for a reasonable number
of lines.
Default: False
:min_tau: optional, float
This value determines size of the wavelength window used to
deposit lines or continua. The wavelength window is expanded
until the optical depth at the edge is below this value. If too
high, this will result in features appearing cut off at the edges.
Decreasing this will make features smoother but will also increase
run time. An increase by a factor of ten will result in roughly a
2x slow down.
Default: 1e-3.
:njobs: optional, int or "auto"
The number of process groups into which the loop over
absorption lines will be divided. If set to -1, each
absorption line will be deposited by exactly one processor.
If njobs is set to a value less than the total number of
available processors (N), then the deposition of an
individual line will be parallelized over (N / njobs)
processors. If set to "auto", it will first try to
parallelize over the list of lines and only parallelize
the line deposition if there are more processors than
lines. This is the optimal strategy for parallelizing
spectrum generation.
Default: "auto"
**Example**
Make a one zone ray and generate a COS spectrum for it including
only Oxygen VI, Mg II, and all Carbon lines, and plot to disk.
>>> import trident
>>> ray = trident.make_onezone_ray()
>>> sg = trident.SpectrumGenerator('COS')
>>> sg.make_spectrum(ray, lines=['O VI', 'Mg II', 'C'])
>>> sg.plot_spectrum('spec_raw.png')
"""
self.observing_redshift = observing_redshift
if isinstance(ray, str):
ray = load(ray)
ad = ray.all_data()
# Clear out any previous spectrum that existed first
self.clear_spectrum()
active_lines = self.line_database.parse_subset(lines)
# Make sure we've produced all the necessary
# derived fields if they aren't native to the data
for line in active_lines:
# if successful, means line.field is in ds.derived_field_list
try:
disk_field = ad._determine_fields(line.field)[0]
# otherwise we probably need to add the field to the dataset
except:
my_ion = \
line.field[:line.field.find("number_density")]
on_ion = my_ion.split("_")
# Add the field if greater than level 1 ionization
# because there is only one naming convention for these fields:
# X_pY_number_density
if on_ion[1]:
my_lev = int(on_ion[1][1:]) + 1
mylog.info("Creating %s from ray's density, "
"temperature, metallicity." % (line.field))
add_ion_number_density_field(
on_ion[0],
my_lev,
ray,
ionization_table=self.ionization_table)
# If level 1 ionization, check to see if other name for
# field is present in dataset
else:
my_lev = 1
alias_field = ('gas',
"".join([my_ion, 'p0_number_density']))
# Don't add the X_number_density if X_p0_number_density is
# in dataset already
if alias_field in ray.derived_field_list:
line.field = alias_field
# But add the field if neither X_number_density nor
# X_p0_number_density is in the dataset
else:
mylog.info("Creating %s from ray's density, "
"temperature, metallicity." % (line.field))
add_ion_number_density_field(
on_ion[0],
my_lev,
ray,
ionization_table=self.ionization_table)
self.add_line(line.identifier,
line.field,
float(line.wavelength),
float(line.f_value),
float(line.gamma),
atomic_mass[line.element],
label_threshold=1e3)
# If there are H I lines present, add a Lyman continuum source
# Lyman continuum source starts at wavelength where last Lyman line
# is deposited (Ly 40), as opposed to true Lyman Limit at 911.763 A
# so there won't be a gap between lines and continuum. Using
# power law of index 3.0 and normalization to match the opacity of
# the final Lyman line into the FUV.
H_lines = self.line_database.select_lines(source_list=active_lines,
element='H',
ion_state='I')
if (len(H_lines) > 0) and (ly_continuum == True):
self.add_continuum('Ly C', H_lines[0].field, 912.32336, 1.6e17,
3.0)
AbsorptionSpectrum.make_spectrum(
self,
ray,
output_file=None,
line_list_file=None,
use_peculiar_velocity=use_peculiar_velocity,
observing_redshift=observing_redshift,
store_observables=store_observables,
min_tau=min_tau,
njobs=njobs)