def __init__(
self, start_point, end_point, ds=None, field_parameters=None, data_source=None
):
validate_3d_array(start_point)
validate_3d_array(end_point)
validate_object(ds, Dataset)
validate_object(field_parameters, dict)
validate_object(data_source, YTSelectionContainer)
super(YTRay, self).__init__(ds, field_parameters, data_source)
if isinstance(start_point, YTArray):
self.start_point = self.ds.arr(start_point).to("code_length")
else:
self.start_point = self.ds.arr(start_point, "code_length", dtype="float64")
if isinstance(end_point, YTArray):
self.end_point = self.ds.arr(end_point).to("code_length")
else:
self.end_point = self.ds.arr(end_point, "code_length", dtype="float64")
if (self.start_point < self.ds.domain_left_edge).any() or (
self.end_point > self.ds.domain_right_edge
).any():
mylog.warn(
"Ray start or end is outside the domain. "
+ "Returned data will only be for the ray section inside the domain."
)
self.vec = self.end_point - self.start_point
self._set_center(self.start_point)
self.set_field_parameter("center", self.start_point)
self._dts, self._ts = None, None
def __init__(
self,
base_region,
domain,
ds,
over_refine_factor=1,
num_ghost_zones=0,
base_grid=None,
):
super(RAMSESDomainSubset, self).__init__(
base_region, domain, ds, over_refine_factor, num_ghost_zones
)
self._base_grid = base_grid
if num_ghost_zones > 0:
if not all(ds.periodicity):
mylog.warn("Ghost zones will wrongly assume the domain to be periodic.")
# Create a base domain *with no self._base_domain.fwidth
base_domain = RAMSESDomainSubset(
ds.all_data(), domain, ds, over_refine_factor
)
self._base_domain = base_domain
elif num_ghost_zones < 0:
raise RuntimeError(
"Cannot initialize a domain subset with a negative number of ghost zones,"
" was called with num_ghost_zones=%s" % num_ghost_zones
)
def set_units(self):
super().set_units()
res = self.parameters["res"]
for i, ax in enumerate("xy"):
self.unit_registry.add(f"{ax}pixels", res[i], dimensions.length)
if res[0] == res[1]:
self.unit_registry.add("pixels", res[0], dimensions.length)
else:
mylog.warn("x and y pixels have different sizes.")
def add_default_quantities(self, field_type='halos'):
for field in ["particle_identifier", "particle_mass",
"particle_position_x", "particle_position_y",
"particle_position_z", "virial_radius"]:
field_name = (field_type, field)
if field_name not in self.halos_ds.field_list:
mylog.warn("Halo dataset %s has no field %s." %
(self.halos_ds, str(field_name)))
continue
self.add_quantity(field, field_type=field_type, prepend=True)
def save_spectrum(self, filename='spectrum.h5', format=None):
"""
Save the current spectrum data to an output file. Unless specified,
the output data format will be determined by the suffix of the filename
provided ("h5":HDF5, "fits":FITS, all other:ASCII).
ASCII data is stored as a tab-delimited text file.
**Parameters**
:filename: string, optional
Output filename for storing the data.
Default: 'spectrum.h5'
:format: string, optional
Data format of the output file. Valid examples are "HDF5",
"FITS", and "ASCII". If None is set, selects based on suffix
of filename.
Default: None
**Example**
Save a spectrum to disk, load it from disk, and plot it.
>>> import trident
>>> ray = trident.make_onezone_ray()
>>> sg = trident.SpectrumGenerator('COS')
>>> sg.make_spectrum(ray)
>>> sg.save_spectrum('temp.h5')
>>> sg.clear_spectrum()
>>> sg.load_spectrum('temp.h5')
>>> sg.plot_spectrum('temp.png')
"""
if format is None:
if filename.endswith('.h5') or filename.endswith('hdf5'):
self._write_spectrum_hdf5(filename)
elif filename.endswith('.fits') or filename.endswith('FITS'):
self._write_spectrum_fits(filename)
else:
self._write_spectrum_ascii(filename)
elif format == 'HDF5':
self._write_spectrum_hdf5(filename)
elif format == 'FITS':
self._write_spectrum_fits(filename)
elif format == 'ASCII':
self._write_spectrum_ascii(filename)
else:
mylog.warn(
"Invalid format. Must be 'HDF5', 'FITS', 'ASCII'. Defaulting to ASCII."
)
self._write_spectrum_ascii(filename)
def get_bbox(self, left, right):
"""
Given left and right indicies, return a mask and
set of offsets+lengths into the sdf data.
"""
ileft = np.floor((left - self.rmin) / self.domain_width * self.domain_dims)
iright = np.floor((right - self.rmin) / self.domain_width * self.domain_dims)
if np.any(iright-ileft) > self.domain_dims:
mylog.warn("Attempting to get data from bounding box larger than the domain. You may want to check your units.")
#iright[iright <= ileft+1] += 1
return self.get_ibbox(ileft, iright)
def read_namelist(self):
"""Read the namelist.txt file in the output folder, if present"""
namelist_file = os.path.join(self.root_folder, 'namelist.txt')
if os.path.exists(namelist_file):
try:
with open(namelist_file, 'r') as f:
nml = f90nml.read(f)
except ImportError as e:
nml = "An error occurred when reading the namelist: %s" % str(e)
except ValueError as e:
mylog.warn("Could not parse `namelist.txt` file as it was malformed: %s" % str(e))
return
self.parameters['namelist'] = nml
def get_bbox(self, left, right):
"""
Given left and right indicies, return a mask and
set of offsets+lengths into the sdf data.
"""
ileft = np.floor(
(left - self.rmin) / self.domain_width * self.domain_dims)
iright = np.floor(
(right - self.rmin) / self.domain_width * self.domain_dims)
if np.any(iright - ileft) > self.domain_dims:
mylog.warn(
"Attempting to get data from bounding box larger than the domain. You may want to check your units."
)
#iright[iright <= ileft+1] += 1
return self.get_ibbox(ileft, iright)
def subfind_field_list(fh, ptype, pcount):
fields = []
offset_fields = []
for field in fh.keys():
if "PartType" in field:
# These are halo member particles
continue
elif isinstance(fh[field], h5py.Group):
my_fields, my_offset_fields = \
subfind_field_list(fh[field], ptype, pcount)
fields.extend(my_fields)
my_offset_fields.extend(offset_fields)
else:
if not fh[field].size % pcount[ptype]:
my_div = fh[field].size / pcount[ptype]
fname = fh[field].name[fh[field].name.find(ptype) +
len(ptype) + 1:]
if my_div > 1:
for i in range(int(my_div)):
fields.append((ptype, "%s_%d" % (fname, i)))
else:
fields.append((ptype, fname))
elif ptype == "SUBFIND" and \
not fh[field].size % fh["/SUBFIND"].attrs["Number_of_groups"]:
# These are actually FOF fields, but they were written after
# a load balancing step moved halos around and thus they do not
# correspond to the halos stored in the FOF group.
my_div = fh[field].size / fh["/SUBFIND"].attrs[
"Number_of_groups"]
fname = fh[field].name[fh[field].name.find(ptype) +
len(ptype) + 1:]
if my_div > 1:
for i in range(int(my_div)):
fields.append(("FOF", "%s_%d" % (fname, i)))
else:
fields.append(("FOF", fname))
offset_fields.append(fname)
else:
mylog.warn("Cannot add field (%s, %s) with size %d." % \
(ptype, fh[field].name, fh[field].size))
continue
return fields, offset_fields
def __init__(self, function=None, width=None, filename=None):
self.kernel = []
self.filename = filename
self.function = function
self.width = width
# if filename is defined, use it
if filename is not None:
# Check to see if the file is in the local dir
if os.path.isfile(filename):
lsf_file = open(filename, 'r')
# otherwise use the file in the lsf_kernels dir
else:
filename2 = os.path.join(trident_path(), "data", \
"lsf_kernels", filename)
if os.path.isfile(filename2):
lsf_file = open(filename2, 'r')
else:
raise RuntimeError(
"LSF filename not found in current " +
"directory or in %s/data/lsf_kernels directory" %
trident_path())
for line in lsf_file:
self.kernel.append(float(line.split()[1]))
lsf_file.close()
self.kernel = np.array(self.kernel)
self.width = self.kernel.size
elif function is not None and width is not None:
if function == 'boxcar':
if width % 2 == 0:
mylog.warn(
"LSF kernel must have an odd length. Reducing kernel size by 1."
)
width -= 1
self.kernel = np.ones(width) / width
elif function == 'gaussian':
from astropy.convolution import Gaussian1DKernel
self.kernel = Gaussian1DKernel(width)
else:
raise RuntimeError(
"Either LSF filename OR function+width must be specified.")
def subfind_field_list(fh, ptype, pcount):
fields = []
offset_fields = []
for field in fh.keys():
if "PartType" in field:
# These are halo member particles
continue
elif isinstance(fh[field], h5py.Group):
my_fields, my_offset_fields = \
subfind_field_list(fh[field], ptype, pcount)
fields.extend(my_fields)
my_offset_fields.extend(offset_fields)
else:
if not fh[field].size % pcount[ptype]:
my_div = fh[field].size / pcount[ptype]
fname = fh[field].name[fh[field].name.find(ptype) + len(ptype) + 1:]
if my_div > 1:
for i in range(int(my_div)):
fields.append((ptype, "%s_%d" % (fname, i)))
else:
fields.append((ptype, fname))
elif ptype == "SUBFIND" and \
not fh[field].size % fh["/SUBFIND"].attrs["Number_of_groups"]:
# These are actually FOF fields, but they were written after
# a load balancing step moved halos around and thus they do not
# correspond to the halos stored in the FOF group.
my_div = fh[field].size / fh["/SUBFIND"].attrs["Number_of_groups"]
fname = fh[field].name[fh[field].name.find(ptype) + len(ptype) + 1:]
if my_div > 1:
for i in range(int(my_div)):
fields.append(("FOF", "%s_%d" % (fname, i)))
else:
fields.append(("FOF", fname))
offset_fields.append(fname)
else:
mylog.warn("Cannot add field (%s, %s) with size %d." % \
(ptype, fh[field].name, fh[field].size))
continue
return fields, offset_fields
def _parse_parameter_file(self):
# hard-coded -- not provided by headers
self.dimensionality = 3
self.refine_by = 2
self.parameters["HydroMethod"] = 'artio'
self.parameters["Time"] = 1. # default unit is 1...
# read header
self.unique_identifier = \
int(os.stat(self.parameter_filename)[stat.ST_CTIME])
self.num_grid = self._handle.num_grid
self.domain_dimensions = np.ones(3, dtype='int32') * self.num_grid
self.domain_left_edge = np.zeros(3, dtype="float64")
self.domain_right_edge = np.ones(3, dtype='float64') * self.num_grid
# TODO: detect if grid exists
self.min_level = 0 # ART has min_level=0
self.max_level = self.artio_parameters["grid_max_level"][0]
# TODO: detect if particles exist
if self._handle.has_particles:
self.num_species = self.artio_parameters["num_particle_species"][0]
self.particle_variables = [["PID", "SPECIES"]
for i in range(self.num_species)]
self.particle_types_raw = \
self.artio_parameters["particle_species_labels"]
self.particle_types = tuple(self.particle_types_raw)
for species in range(self.num_species):
# Mass would be best as a derived field,
# but wouldn't detect under 'all'
if self.artio_parameters["particle_species_labels"][species]\
== "N-BODY":
self.particle_variables[species].append("MASS")
if self.artio_parameters["num_primary_variables"][species] > 0:
self.particle_variables[species].extend(
self.artio_parameters[
"species_%02d_primary_variable_labels" %
(species, )])
if self.artio_parameters["num_secondary_variables"][
species] > 0:
self.particle_variables[species].extend(
self.artio_parameters[
"species_%02d_secondary_variable_labels" %
(species, )])
else:
self.num_species = 0
self.particle_variables = []
self.particle_types = ()
self.particle_types_raw = self.particle_types
self.current_time = self.quan(
self._handle.tphys_from_tcode(self.artio_parameters["tl"][0]),
"yr")
# detect cosmology
if "abox" in self.artio_parameters:
self.cosmological_simulation = True
abox = self.artio_parameters["abox"][0]
self.omega_lambda = self.artio_parameters["OmegaL"][0]
self.omega_matter = self.artio_parameters["OmegaM"][0]
self.hubble_constant = self.artio_parameters["hubble"][0]
self.current_redshift = 1.0 / self.artio_parameters["auni"][0] - 1.0
self.current_redshift_box = 1.0 / abox - 1.0
self.parameters["initial_redshift"] =\
1.0 / self.artio_parameters["auni_init"][0] - 1.0
self.parameters["CosmologyInitialRedshift"] =\
self.parameters["initial_redshift"]
self.parameters['unit_m'] = self.artio_parameters["mass_unit"][0]
self.parameters['unit_t'] =\
self.artio_parameters["time_unit"][0] * abox**2
self.parameters['unit_l'] =\
self.artio_parameters["length_unit"][0] * abox
if self.artio_parameters["DeltaDC"][0] != 0:
mylog.warn(
"DeltaDC != 0, which implies auni != abox. Be sure you understand which expansion parameter is appropriate for your use! (Gnedin, Kravtsov, & Rudd 2011)"
)
else:
self.cosmological_simulation = False
self.parameters['unit_l'] = self.artio_parameters["length_unit"][0]
self.parameters['unit_t'] = self.artio_parameters["time_unit"][0]
self.parameters['unit_m'] = self.artio_parameters["mass_unit"][0]
# hard coded assumption of 3D periodicity
self.periodicity = (True, True, True)
def make_light_ray(self, seed=None,
start_position=None, end_position=None,
trajectory=None,
fields=None, setup_function=None,
solution_filename=None, data_filename=None,
get_los_velocity=True, redshift=None,
njobs=-1):
"""
make_light_ray(seed=None, start_position=None, end_position=None,
trajectory=None, fields=None, setup_function=None,
solution_filename=None, data_filename=None,
get_los_velocity=True, redshift=None,
njobs=-1)
Create a light ray and get field values for each lixel. A light
ray consists of a list of field values for cells intersected by
the ray and the path length of the ray through those cells.
Light ray data can be written out to an hdf5 file.
Parameters
----------
seed : optional, int
Seed for the random number generator.
Default: None.
start_position : optional, list of floats
Used only if creating a light ray from a single dataset.
The coordinates of the starting position of the ray.
Default: None.
end_position : optional, list of floats
Used only if creating a light ray from a single dataset.
The coordinates of the ending position of the ray.
Default: None.
trajectory : optional, list of floats
Used only if creating a light ray from a single dataset.
The (r, theta, phi) direction of the light ray. Use either
end_position or trajectory, not both.
Default: None.
fields : optional, list
A list of fields for which to get data.
Default: None.
setup_function : optional, callable, accepts a ds
This function will be called on each dataset that is loaded
to create the light ray. For, example, this can be used to
add new derived fields.
Default: None.
solution_filename : optional, string
Path to a text file where the trajectories of each
subray is written out.
Default: None.
data_filename : optional, string
Path to output file for ray data.
Default: None.
get_los_velocity : optional, bool
If True, the line of sight velocity is calculated for
each point in the ray.
Default: True.
redshift : optional, float
Used with light rays made from single datasets to specify a
starting redshift for the ray. If not used, the starting
redshift will be 0 for a non-cosmological dataset and
the dataset redshift for a cosmological dataset.
Default: None.
njobs : optional, int
The number of parallel jobs over which the segments will
be split. Choose -1 for one processor per segment.
Default: -1.
Examples
--------
Make a light ray from multiple datasets:
>>> import yt
>>> from yt.analysis_modules.cosmological_observation.light_ray.api import \
... LightRay
>>> my_ray = LightRay("enzo_tiny_cosmology/32Mpc_32.enzo", "Enzo",
... 0., 0.1, time_data=False)
...
>>> my_ray.make_light_ray(seed=12345,
... solution_filename="solution.txt",
... data_filename="my_ray.h5",
... fields=["temperature", "density"],
... get_los_velocity=True)
Make a light ray from a single dataset:
>>> import yt
>>> from yt.analysis_modules.cosmological_observation.light_ray.api import \
... LightRay
>>> my_ray = LightRay("IsolatedGalaxy/galaxy0030/galaxy0030")
...
>>> my_ray.make_light_ray(start_position=[0., 0., 0.],
... end_position=[1., 1., 1.],
... solution_filename="solution.txt",
... data_filename="my_ray.h5",
... fields=["temperature", "density"],
... get_los_velocity=True)
"""
# Calculate solution.
self._calculate_light_ray_solution(seed=seed,
start_position=start_position,
end_position=end_position,
trajectory=trajectory,
filename=solution_filename)
# Initialize data structures.
self._data = {}
if fields is None: fields = []
data_fields = fields[:]
all_fields = fields[:]
all_fields.extend(['dl', 'dredshift', 'redshift'])
if get_los_velocity:
all_fields.extend(['velocity_x', 'velocity_y',
'velocity_z', 'velocity_los'])
data_fields.extend(['velocity_x', 'velocity_y', 'velocity_z'])
all_ray_storage = {}
for my_storage, my_segment in parallel_objects(self.light_ray_solution,
storage=all_ray_storage,
njobs=njobs):
# Load dataset for segment.
ds = load(my_segment['filename'], **self.load_kwargs)
my_segment['unique_identifier'] = ds.unique_identifier
if redshift is not None:
if ds.cosmological_simulation and redshift != ds.current_redshift:
mylog.warn("Generating light ray with different redshift than " +
"the dataset itself.")
my_segment["redshift"] = redshift
if setup_function is not None:
setup_function(ds)
if start_position is not None:
my_segment["start"] = ds.arr(my_segment["start"], "code_length")
my_segment["end"] = ds.arr(my_segment["end"], "code_length")
else:
my_segment["start"] = ds.domain_width * my_segment["start"] + \
ds.domain_left_edge
my_segment["end"] = ds.domain_width * my_segment["end"] + \
ds.domain_left_edge
if not ds.cosmological_simulation:
next_redshift = my_segment["redshift"]
elif self.near_redshift == self.far_redshift:
next_redshift = my_segment["redshift"] - \
self._deltaz_forward(my_segment["redshift"],
ds.domain_width[0].in_units("Mpccm / h") *
my_segment["traversal_box_fraction"])
elif my_segment.get("next", None) is None:
next_redshift = self.near_redshift
else:
next_redshift = my_segment['next']['redshift']
mylog.info("Getting segment at z = %s: %s to %s." %
(my_segment['redshift'], my_segment['start'],
my_segment['end']))
# Break periodic ray into non-periodic segments.
sub_segments = periodic_ray(my_segment['start'], my_segment['end'],
left=ds.domain_left_edge,
right=ds.domain_right_edge)
# Prepare data structure for subsegment.
sub_data = {}
sub_data['segment_redshift'] = my_segment['redshift']
for field in all_fields:
sub_data[field] = []
# Get data for all subsegments in segment.
for sub_segment in sub_segments:
mylog.info("Getting subsegment: %s to %s." %
(list(sub_segment[0]), list(sub_segment[1])))
sub_ray = ds.ray(sub_segment[0], sub_segment[1])
asort = np.argsort(sub_ray["t"])
sub_data['dl'].extend(sub_ray['dts'][asort] *
vector_length(sub_ray.start_point,
sub_ray.end_point))
for field in data_fields:
sub_data[field].extend(sub_ray[field][asort])
if get_los_velocity:
line_of_sight = sub_segment[1] - sub_segment[0]
line_of_sight /= ((line_of_sight**2).sum())**0.5
sub_vel = ds.arr([sub_ray['velocity_x'],
sub_ray['velocity_y'],
sub_ray['velocity_z']])
sub_data['velocity_los'].extend((np.rollaxis(sub_vel, 1) *
line_of_sight).sum(axis=1)[asort])
del sub_vel
sub_ray.clear_data()
del sub_ray, asort
for key in sub_data:
sub_data[key] = ds.arr(sub_data[key]).in_cgs()
# Get redshift for each lixel. Assume linear relation between l and z.
sub_data['dredshift'] = (my_segment['redshift'] - next_redshift) * \
(sub_data['dl'] / vector_length(my_segment['start'],
my_segment['end']).in_cgs())
sub_data['redshift'] = my_segment['redshift'] - \
sub_data['dredshift'].cumsum() + sub_data['dredshift']
# Remove empty lixels.
sub_dl_nonzero = sub_data['dl'].nonzero()
for field in all_fields:
sub_data[field] = sub_data[field][sub_dl_nonzero]
del sub_dl_nonzero
# Add to storage.
my_storage.result = sub_data
del ds
# Reconstruct ray data from parallel_objects storage.
all_data = [my_data for my_data in all_ray_storage.values()]
# This is now a list of segments where each one is a dictionary
# with all the fields.
all_data.sort(key=lambda a:a['segment_redshift'], reverse=True)
# Flatten the list into a single dictionary containing fields
# for the whole ray.
all_data = _flatten_dict_list(all_data, exceptions=['segment_redshift'])
if data_filename is not None:
self._write_light_ray(data_filename, all_data)
self._data = all_data
return all_data
def _add_lines_to_spectrum(self, field_data, use_peculiar_velocity):
"""
Add the absorption lines to the spectrum.
"""
# Only make voigt profile for slice of spectrum that is 10 times the line width.
spectrum_bin_ratio = 5
# Widen wavelength window until optical depth reaches a max value at the ends.
max_tau = 0.001
for line in self.line_list:
column_density = field_data[line['field_name']] * field_data['dl']
delta_lambda = line['wavelength'] * field_data['redshift']
if use_peculiar_velocity:
# include factor of (1 + z) because our velocity is in proper frame.
delta_lambda += line['wavelength'] * (1 + field_data['redshift']) * \
field_data['velocity_los'] / speed_of_light_cgs
thermal_b = np.sqrt(
(2 * boltzmann_constant_cgs * field_data['temperature']) /
line['atomic_mass'])
center_bins = np.digitize((delta_lambda + line['wavelength']),
self.lambda_bins)
# ratio of line width to bin width
width_ratio = ((line['wavelength'] + delta_lambda) * \
thermal_b / speed_of_light_cgs / self.bin_width).in_units("").d
if (width_ratio < 1.0).any():
mylog.warn(("%d out of %d line components are unresolved, " +
"consider increasing spectral resolution.") %
((width_ratio < 1.0).sum(), width_ratio.size))
# do voigt profiles for a subset of the full spectrum
left_index = (center_bins -
spectrum_bin_ratio * width_ratio).astype(int).clip(
0, self.n_lambda)
right_index = (center_bins +
spectrum_bin_ratio * width_ratio).astype(int).clip(
0, self.n_lambda)
# loop over all lines wider than the bin width
valid_lines = np.where((width_ratio >= 1.0)
& (right_index - left_index > 1))[0]
pbar = get_pbar(
"Adding line - %s [%f A]: " %
(line['label'], line['wavelength']), valid_lines.size)
for i, lixel in enumerate(valid_lines):
my_bin_ratio = spectrum_bin_ratio
while True:
lambda_bins, line_tau = \
tau_profile(
line['wavelength'], line['f_value'],
line['gamma'], thermal_b[lixel].in_units("km/s"),
column_density[lixel],
delta_lambda=delta_lambda[lixel],
lambda_bins=self.lambda_bins[left_index[lixel]:right_index[lixel]])
# Widen wavelength window until optical depth reaches a max value at the ends.
if (line_tau[0] < max_tau and line_tau[-1] < max_tau) or \
(left_index[lixel] <= 0 and right_index[lixel] >= self.n_lambda):
break
my_bin_ratio *= 2
left_index[lixel] = (
center_bins[lixel] -
my_bin_ratio * width_ratio[lixel]).astype(int).clip(
0, self.n_lambda)
right_index[lixel] = (
center_bins[lixel] +
my_bin_ratio * width_ratio[lixel]).astype(int).clip(
0, self.n_lambda)
self.tau_field[
left_index[lixel]:right_index[lixel]] += line_tau
if line['label_threshold'] is not None and \
column_density[lixel] >= line['label_threshold']:
if use_peculiar_velocity:
peculiar_velocity = field_data['velocity_los'][
lixel].in_units("km/s")
else:
peculiar_velocity = 0.0
self.spectrum_line_list.append({
'label':
line['label'],
'wavelength':
(line['wavelength'] + delta_lambda[lixel]),
'column_density':
column_density[lixel],
'b_thermal':
thermal_b[lixel],
'redshift':
field_data['redshift'][lixel],
'v_pec':
peculiar_velocity
})
pbar.update(i)
pbar.finish()
del column_density, delta_lambda, thermal_b, \
center_bins, width_ratio, left_index, right_index
def _add_lines_to_spectrum(self, field_data, use_peculiar_velocity):
"""
Add the absorption lines to the spectrum.
"""
# Only make voigt profile for slice of spectrum that is 10 times the line width.
spectrum_bin_ratio = 5
# Widen wavelength window until optical depth reaches a max value at the ends.
max_tau = 0.001
for line in self.line_list:
column_density = field_data[line['field_name']] * field_data['dl']
delta_lambda = line['wavelength'] * field_data['redshift']
if use_peculiar_velocity:
# include factor of (1 + z) because our velocity is in proper frame.
delta_lambda += line['wavelength'] * (1 + field_data['redshift']) * \
field_data['velocity_los'] / speed_of_light_cgs
thermal_b = np.sqrt((2 * boltzmann_constant_cgs *
field_data['temperature']) /
line['atomic_mass'])
center_bins = np.digitize((delta_lambda + line['wavelength']),
self.lambda_bins)
# ratio of line width to bin width
width_ratio = ((line['wavelength'] + delta_lambda) * \
thermal_b / speed_of_light_cgs / self.bin_width).in_units("").d
if (width_ratio < 1.0).any():
mylog.warn(("%d out of %d line components are unresolved, " +
"consider increasing spectral resolution.") %
((width_ratio < 1.0).sum(), width_ratio.size))
# do voigt profiles for a subset of the full spectrum
left_index = (center_bins -
spectrum_bin_ratio * width_ratio).astype(int).clip(0, self.n_lambda)
right_index = (center_bins +
spectrum_bin_ratio * width_ratio).astype(int).clip(0, self.n_lambda)
# loop over all lines wider than the bin width
valid_lines = np.where((width_ratio >= 1.0) &
(right_index - left_index > 1))[0]
pbar = get_pbar("Adding line - %s [%f A]: " % (line['label'], line['wavelength']),
valid_lines.size)
for i, lixel in enumerate(valid_lines):
my_bin_ratio = spectrum_bin_ratio
while True:
lambda_bins, line_tau = \
tau_profile(
line['wavelength'], line['f_value'],
line['gamma'], thermal_b[lixel].in_units("km/s"),
column_density[lixel],
delta_lambda=delta_lambda[lixel],
lambda_bins=self.lambda_bins[left_index[lixel]:right_index[lixel]])
# Widen wavelength window until optical depth reaches a max value at the ends.
if (line_tau[0] < max_tau and line_tau[-1] < max_tau) or \
(left_index[lixel] <= 0 and right_index[lixel] >= self.n_lambda):
break
my_bin_ratio *= 2
left_index[lixel] = (center_bins[lixel] -
my_bin_ratio *
width_ratio[lixel]).astype(int).clip(0, self.n_lambda)
right_index[lixel] = (center_bins[lixel] +
my_bin_ratio *
width_ratio[lixel]).astype(int).clip(0, self.n_lambda)
self.tau_field[left_index[lixel]:right_index[lixel]] += line_tau
if line['label_threshold'] is not None and \
column_density[lixel] >= line['label_threshold']:
if use_peculiar_velocity:
peculiar_velocity = field_data['velocity_los'][lixel].in_units("km/s")
else:
peculiar_velocity = 0.0
self.spectrum_line_list.append({'label': line['label'],
'wavelength': (line['wavelength'] +
delta_lambda[lixel]),
'column_density': column_density[lixel],
'b_thermal': thermal_b[lixel],
'redshift': field_data['redshift'][lixel],
'v_pec': peculiar_velocity})
pbar.update(i)
pbar.finish()
del column_density, delta_lambda, thermal_b, \
center_bins, width_ratio, left_index, right_index
from yt.extern import \
six
from yt.funcs import \
is_root, mylog
from yt.utilities.parallel_tools.parallel_analysis_interface import \
ParallelAnalysisInterface, \
ProcessorPool
from yt.utilities.exceptions import \
YTRockstarMultiMassNotSupported
try:
from yt_astro_analysis.halo_finding.rockstar import \
rockstar_interface
except ImportError:
mylog.warn(
("Cannot import the rockstar interface. Rockstar will not run.\n" +
"If you need Rockstar, see the installation instructions at " +
"http://yt-astro-analysis.readthedocs.io/."))
rockstar_interface = None
import socket
import time
import os
import numpy as np
from os import path
class InlineRunner(ParallelAnalysisInterface):
def __init__(self):
# If this is being run inline, num_readers == comm.size, always.
psize = ytcfg.getint("yt", "__global_parallel_size")
self.num_readers = psize
def _add_lines_to_spectrum(self,
field_data,
use_peculiar_velocity,
output_absorbers_file,
subgrid_resolution=10,
observing_redshift=0.,
njobs=-1):
"""
Add the absorption lines to the spectrum.
"""
# Change the redshifts of individual absorbers to account for the
# redshift at which the observer sits
redshift, redshift_eff = self._apply_observing_redshift(
field_data, use_peculiar_velocity, observing_redshift)
# Widen wavelength window until optical depth falls below this tau
# value at the ends to assure that the wings of a line have been
# fully resolved.
min_tau = 1e-3
# step through each ionic transition (e.g. HI, HII, MgII) specified
# and deposit the lines into the spectrum
for line in parallel_objects(self.line_list, njobs=njobs):
column_density = field_data[line['field_name']] * field_data['dl']
if (column_density < 0).any():
mylog.warn(
"Setting negative densities for field %s to 0! Bad!" %
line['field_name'])
np.clip(column_density, 0, np.inf, out=column_density)
if (column_density == 0).all():
mylog.info("Not adding line %s: insufficient column density" %
line['label'])
continue
# redshift_eff field combines cosmological and velocity redshifts
# so delta_lambda gives the offset in angstroms from the rest frame
# wavelength to the observed wavelength of the transition
if use_peculiar_velocity:
delta_lambda = line['wavelength'] * redshift_eff
else:
delta_lambda = line['wavelength'] * redshift
# lambda_obs is central wavelength of line after redshift
lambda_obs = line['wavelength'] + delta_lambda
# the total number of absorbers per transition
n_absorbers = len(lambda_obs)
# we want to know the bin index in the lambda_field array
# where each line has its central wavelength after being
# redshifted. however, because we don't know a priori how wide
# a line will be (ie DLAs), we have to include bin indices
# *outside* the spectral range of the AbsorptionSpectrum
# object. Thus, we find the "equivalent" bin index, which
# may be <0 or >the size of the array. In the end, we deposit
# the bins that actually overlap with the AbsorptionSpectrum's
# range in lambda.
# this equation gives us the "equivalent" bin index for each line
# if it were placed into the self.lambda_field array
center_index = (lambda_obs.in_units('Angstrom').d - self.lambda_min) \
/ self.bin_width.d
center_index = np.ceil(center_index).astype('int')
# thermal broadening b parameter
thermal_b = np.sqrt(
(2 * boltzmann_constant_cgs * field_data['temperature']) /
line['atomic_mass'])
# the actual thermal width of the lines
thermal_width = (lambda_obs * thermal_b /
speed_of_light_cgs).convert_to_units("angstrom")
# Sanitize units for faster runtime of the tau_profile machinery.
lambda_0 = line['wavelength'].d # line's rest frame; angstroms
cdens = column_density.in_units("cm**-2").d # cm**-2
thermb = thermal_b.in_cgs().d # thermal b coefficient; cm / s
dlambda = delta_lambda.d # lambda offset; angstroms
if use_peculiar_velocity:
vlos = field_data['velocity_los'].in_units("km/s").d # km/s
else:
vlos = np.zeros(field_data['temperature'].size)
# When we actually deposit the voigt profile, sometimes we will
# have underresolved lines (ie lines with smaller widths than
# the spectral bin size). Here, we create virtual wavelength bins
# small enough in width to well resolve each line, deposit the
# voigt profile into them, then numerically integrate their tau
# values and sum them to redeposit them into the actual spectral
# bins.
# virtual bins (vbins) will be:
# 1) <= the bin_width; assures at least as good as spectral bins
# 2) <= 1/10th the thermal width; assures resolving voigt profiles
# (actually 1/subgrid_resolution value, default is 1/10)
# 3) a bin width will be divisible by vbin_width times a power of
# 10; this will assure we don't get spikes in the deposited
# spectra from uneven numbers of vbins per bin
resolution = thermal_width / self.bin_width
n_vbins_per_bin = (10**(np.ceil(
np.log10(subgrid_resolution / resolution)).clip(
0, np.inf))).astype('int')
vbin_width = self.bin_width.d / n_vbins_per_bin
# a note to the user about which lines components are unresolved
if (thermal_width < self.bin_width).any():
mylog.info(
"%d out of %d line components will be " +
"deposited as unresolved lines.",
(thermal_width < self.bin_width).sum(), n_absorbers)
# provide a progress bar with information about lines processed
pbar = get_pbar("Adding line - %s [%f A]: " % \
(line['label'], line['wavelength']), n_absorbers)
# for a given transition, step through each location in the
# observed spectrum where it occurs and deposit a voigt profile
for i in parallel_objects(np.arange(n_absorbers), njobs=-1):
# if there is a ray element with temperature = 0 or column
# density = 0, skip it
if (thermal_b[i] == 0.) or (cdens[i] == 0.):
pbar.update(i)
continue
# the virtual window into which the line is deposited initially
# spans a region of 2 coarse spectral bins
# (one on each side of the center_index) but the window
# can expand as necessary.
# it will continue to expand until the tau value in the far
# edge of the wings is less than the min_tau value or it
# reaches the edge of the spectrum
window_width_in_bins = 2
while True:
left_index = (center_index[i] - window_width_in_bins // 2)
right_index = (center_index[i] + window_width_in_bins // 2)
n_vbins = (right_index - left_index) * n_vbins_per_bin[i]
# the array of virtual bins in lambda space
vbins = \
np.linspace(self.lambda_min + self.bin_width.d * left_index,
self.lambda_min + self.bin_width.d * right_index,
n_vbins, endpoint=False)
# the virtual bins and their corresponding opacities
vbins, vtau = \
tau_profile(
lambda_0, line['f_value'], line['gamma'],
thermb[i], cdens[i],
delta_lambda=dlambda[i], lambda_bins=vbins)
# If tau has not dropped below min tau threshold by the
# edges (ie the wings), then widen the wavelength
# window and repeat process.
if (vtau[0] < min_tau and vtau[-1] < min_tau):
break
window_width_in_bins *= 2
# numerically integrate the virtual bins to calculate a
# virtual equivalent width; then sum the virtual equivalent
# widths and deposit into each spectral bin
vEW = vtau * vbin_width[i]
EW = np.zeros(right_index - left_index)
EW_indices = np.arange(left_index, right_index)
for k, val in enumerate(EW_indices):
EW[k] = vEW[n_vbins_per_bin[i] * k: \
n_vbins_per_bin[i] * (k + 1)].sum()
EW = EW / self.bin_width.d
# only deposit EW bins that actually intersect the original
# spectral wavelength range (i.e. lambda_field)
# if EW bins don't intersect the original spectral range at all
# then skip the deposition
if ((left_index >= self.n_lambda) or \
(right_index < 0)):
pbar.update(i)
continue
# otherwise, determine how much of the original spectrum
# is intersected by the expanded line window to be deposited,
# and deposit the Equivalent Width data into that intersecting
# window in the original spectrum's tau
else:
intersect_left_index = max(left_index, 0)
intersect_right_index = min(right_index, self.n_lambda - 1)
self.tau_field[intersect_left_index:intersect_right_index] \
+= EW[(intersect_left_index - left_index): \
(intersect_right_index - left_index)]
# write out absorbers to file if the column density of
# an absorber is greater than the specified "label_threshold"
# of that absorption line
if output_absorbers_file and \
line['label_threshold'] is not None and \
cdens[i] >= line['label_threshold']:
if use_peculiar_velocity:
peculiar_velocity = vlos[i]
else:
peculiar_velocity = 0.0
self.absorbers_list.append({
'label':
line['label'],
'wavelength': (lambda_0 + dlambda[i]),
'column_density':
column_density[i],
'b_thermal':
thermal_b[i],
'redshift':
redshift[i],
'redshift_eff':
redshift_eff[i],
'v_pec':
peculiar_velocity
})
pbar.update(i)
pbar.finish()
del column_density, delta_lambda, lambda_obs, center_index, \
thermal_b, thermal_width, cdens, thermb, dlambda, \
vlos, resolution, vbin_width, n_vbins, n_vbins_per_bin
comm = _get_comm(())
self.tau_field = comm.mpi_allreduce(self.tau_field, op="sum")
if output_absorbers_file:
self.absorbers_list = comm.par_combine_object(self.absorbers_list,
"cat",
datatype="list")
def _count_particles(self, data_file):
pcount = self._handle['x'].size
if (pcount > 1e9):
mylog.warn("About to load %i particles into memory. " % (pcount) +
"You may want to consider a midx-enabled load")
return {'dark_matter': pcount}