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Return a list of unique items in the list provided, preserving the order
in which they are found. | def _unique_with_order_preserved(items):
"""
Return a list of unique items in the list provided, preserving the order
in which they are found.
"""
new_items = []
for item in items:
if item not in new_items:
new_items.append(item)
return new_items |
Return a correlation matrix between the pixel coordinates and the
high level world coordinates, along with the list of high level world
coordinate classes.
The shape of the matrix is ``(n_world, n_pix)``, where ``n_world`` is the
number of high level world coordinates. | def _pixel_to_world_correlation_matrix(wcs):
"""
Return a correlation matrix between the pixel coordinates and the
high level world coordinates, along with the list of high level world
coordinate classes.
The shape of the matrix is ``(n_world, n_pix)``, where ``n_world`` is the
number of high level world coordinates.
"""
# We basically want to collapse the world dimensions together that are
# combined into the same high-level objects.
# Get the following in advance as getting these properties can be expensive
all_components = wcs.low_level_wcs.world_axis_object_components
all_classes = wcs.low_level_wcs.world_axis_object_classes
axis_correlation_matrix = wcs.low_level_wcs.axis_correlation_matrix
components = _unique_with_order_preserved([c[0] for c in all_components])
matrix = np.zeros((len(components), wcs.pixel_n_dim), dtype=bool)
for iworld in range(wcs.world_n_dim):
iworld_unique = components.index(all_components[iworld][0])
matrix[iworld_unique] |= axis_correlation_matrix[iworld]
classes = [all_classes[component][0] for component in components]
return matrix, classes |
Correlation matrix between the input and output pixel coordinates for a
pixel -> world -> pixel transformation specified by two WCS instances.
The first WCS specified is the one used for the pixel -> world
transformation and the second WCS specified is the one used for the world ->
pixel transformation. The shape of the matrix is
``(n_pixel_out, n_pixel_in)``. | def _pixel_to_pixel_correlation_matrix(wcs_in, wcs_out):
"""
Correlation matrix between the input and output pixel coordinates for a
pixel -> world -> pixel transformation specified by two WCS instances.
The first WCS specified is the one used for the pixel -> world
transformation and the second WCS specified is the one used for the world ->
pixel transformation. The shape of the matrix is
``(n_pixel_out, n_pixel_in)``.
"""
matrix1, classes1 = _pixel_to_world_correlation_matrix(wcs_in)
matrix2, classes2 = _pixel_to_world_correlation_matrix(wcs_out)
if len(classes1) != len(classes2):
raise ValueError("The two WCS return a different number of world coordinates")
# Check if classes match uniquely
unique_match = True
mapping = []
for class1 in classes1:
matches = classes2.count(class1)
if matches == 0:
raise ValueError("The world coordinate types of the two WCS do not match")
elif matches > 1:
unique_match = False
break
else:
mapping.append(classes2.index(class1))
if unique_match:
# Classes are unique, so we need to re-order matrix2 along the world
# axis using the mapping we found above.
matrix2 = matrix2[mapping]
elif classes1 != classes2:
raise ValueError(
"World coordinate order doesn't match and automatic matching is ambiguous"
)
matrix = np.matmul(matrix2.T, matrix1)
return matrix |
Given an axis correlation matrix from a WCS object, return information about
the individual WCS that can be split out.
The output is a list of tuples, where each tuple contains a list of
pixel dimensions and a list of world dimensions that can be extracted to
form a new WCS. For example, in the case of a spectral cube with the first
two world coordinates being the celestial coordinates and the third
coordinate being an uncorrelated spectral axis, the matrix would look like::
array([[ True, True, False],
[ True, True, False],
[False, False, True]])
and this function will return ``[([0, 1], [0, 1]), ([2], [2])]``. | def _split_matrix(matrix):
"""
Given an axis correlation matrix from a WCS object, return information about
the individual WCS that can be split out.
The output is a list of tuples, where each tuple contains a list of
pixel dimensions and a list of world dimensions that can be extracted to
form a new WCS. For example, in the case of a spectral cube with the first
two world coordinates being the celestial coordinates and the third
coordinate being an uncorrelated spectral axis, the matrix would look like::
array([[ True, True, False],
[ True, True, False],
[False, False, True]])
and this function will return ``[([0, 1], [0, 1]), ([2], [2])]``.
"""
pixel_used = []
split_info = []
for ipix in range(matrix.shape[1]):
if ipix in pixel_used:
continue
pixel_include = np.zeros(matrix.shape[1], dtype=bool)
pixel_include[ipix] = True
n_pix_prev, n_pix = 0, 1
while n_pix > n_pix_prev:
world_include = matrix[:, pixel_include].any(axis=1)
pixel_include = matrix[world_include, :].any(axis=0)
n_pix_prev, n_pix = n_pix, np.sum(pixel_include)
pixel_indices = list(np.nonzero(pixel_include)[0])
world_indices = list(np.nonzero(world_include)[0])
pixel_used.extend(pixel_indices)
split_info.append((pixel_indices, world_indices))
return split_info |
Transform pixel coordinates in a dataset with a WCS to pixel coordinates
in another dataset with a different WCS.
This function is designed to efficiently deal with input pixel arrays that
are broadcasted views of smaller arrays, and is compatible with any
APE14-compliant WCS.
Parameters
----------
wcs_in : `~astropy.wcs.wcsapi.BaseHighLevelWCS`
A WCS object for the original dataset which complies with the
high-level shared APE 14 WCS API.
wcs_out : `~astropy.wcs.wcsapi.BaseHighLevelWCS`
A WCS object for the target dataset which complies with the
high-level shared APE 14 WCS API.
*inputs :
Scalars or arrays giving the pixel coordinates to transform. | def pixel_to_pixel(wcs_in, wcs_out, *inputs):
"""
Transform pixel coordinates in a dataset with a WCS to pixel coordinates
in another dataset with a different WCS.
This function is designed to efficiently deal with input pixel arrays that
are broadcasted views of smaller arrays, and is compatible with any
APE14-compliant WCS.
Parameters
----------
wcs_in : `~astropy.wcs.wcsapi.BaseHighLevelWCS`
A WCS object for the original dataset which complies with the
high-level shared APE 14 WCS API.
wcs_out : `~astropy.wcs.wcsapi.BaseHighLevelWCS`
A WCS object for the target dataset which complies with the
high-level shared APE 14 WCS API.
*inputs :
Scalars or arrays giving the pixel coordinates to transform.
"""
# Shortcut for scalars
if np.isscalar(inputs[0]):
world_outputs = wcs_in.pixel_to_world(*inputs)
if not isinstance(world_outputs, (tuple, list)):
world_outputs = (world_outputs,)
return wcs_out.world_to_pixel(*world_outputs)
# Remember original shape
original_shape = inputs[0].shape
matrix = _pixel_to_pixel_correlation_matrix(wcs_in, wcs_out)
split_info = _split_matrix(matrix)
outputs = [None] * wcs_out.pixel_n_dim
for pixel_in_indices, pixel_out_indices in split_info:
pixel_inputs = []
for ipix in range(wcs_in.pixel_n_dim):
if ipix in pixel_in_indices:
pixel_inputs.append(unbroadcast(inputs[ipix]))
else:
pixel_inputs.append(inputs[ipix].flat[0])
pixel_inputs = np.broadcast_arrays(*pixel_inputs)
world_outputs = wcs_in.pixel_to_world(*pixel_inputs)
if not isinstance(world_outputs, (tuple, list)):
world_outputs = (world_outputs,)
pixel_outputs = wcs_out.world_to_pixel(*world_outputs)
if wcs_out.pixel_n_dim == 1:
pixel_outputs = (pixel_outputs,)
for ipix in range(wcs_out.pixel_n_dim):
if ipix in pixel_out_indices:
outputs[ipix] = np.broadcast_to(pixel_outputs[ipix], original_shape)
return outputs[0] if wcs_out.pixel_n_dim == 1 else outputs |
Return a matrix of shape ``(world_n_dim, pixel_n_dim)`` where each entry
``[i, j]`` is the partial derivative d(world_i)/d(pixel_j) at the requested
pixel position.
Parameters
----------
wcs : `~astropy.wcs.WCS`
The WCS transformation to evaluate the derivatives for.
*pixel : float
The scalar pixel coordinates at which to evaluate the derivatives.
normalize_by_world : bool
If `True`, the matrix is normalized so that for each world entry
the derivatives add up to 1. | def local_partial_pixel_derivatives(wcs, *pixel, normalize_by_world=False):
"""
Return a matrix of shape ``(world_n_dim, pixel_n_dim)`` where each entry
``[i, j]`` is the partial derivative d(world_i)/d(pixel_j) at the requested
pixel position.
Parameters
----------
wcs : `~astropy.wcs.WCS`
The WCS transformation to evaluate the derivatives for.
*pixel : float
The scalar pixel coordinates at which to evaluate the derivatives.
normalize_by_world : bool
If `True`, the matrix is normalized so that for each world entry
the derivatives add up to 1.
"""
# Find the world coordinates at the requested pixel
pixel_ref = np.array(pixel)
world_ref = np.array(wcs.pixel_to_world_values(*pixel_ref))
# Set up the derivative matrix
derivatives = np.zeros((wcs.world_n_dim, wcs.pixel_n_dim))
for i in range(wcs.pixel_n_dim):
pixel_off = pixel_ref.copy()
pixel_off[i] += 1
world_off = np.array(wcs.pixel_to_world_values(*pixel_off))
derivatives[:, i] = world_off - world_ref
if normalize_by_world:
derivatives /= derivatives.sum(axis=0)[:, np.newaxis]
return derivatives |
Objective function for fitting linear terms.
Parameters
----------
params : array
6 element array. First 4 elements are PC matrix, last 2 are CRPIX.
lon, lat: array
Sky coordinates.
x, y: array
Pixel coordinates
w_obj: `~astropy.wcs.WCS`
WCS object | def _linear_wcs_fit(params, lon, lat, x, y, w_obj):
"""
Objective function for fitting linear terms.
Parameters
----------
params : array
6 element array. First 4 elements are PC matrix, last 2 are CRPIX.
lon, lat: array
Sky coordinates.
x, y: array
Pixel coordinates
w_obj: `~astropy.wcs.WCS`
WCS object
"""
cd = params[0:4]
crpix = params[4:6]
w_obj.wcs.cd = ((cd[0], cd[1]), (cd[2], cd[3]))
w_obj.wcs.crpix = crpix
lon2, lat2 = w_obj.wcs_pix2world(x, y, 0)
lat_resids = lat - lat2
lon_resids = lon - lon2
# In case the longitude has wrapped around
lon_resids = np.mod(lon_resids - 180.0, 360.0) - 180.0
resids = np.concatenate((lon_resids * np.cos(np.radians(lat)), lat_resids))
return resids |
Objective function for fitting SIP.
Parameters
----------
params : array
Fittable parameters. First 4 elements are PC matrix, last 2 are CRPIX.
lon, lat: array
Sky coordinates.
u, v: array
Pixel coordinates
w_obj: `~astropy.wcs.WCS`
WCS object | def _sip_fit(params, lon, lat, u, v, w_obj, order, coeff_names):
"""Objective function for fitting SIP.
Parameters
----------
params : array
Fittable parameters. First 4 elements are PC matrix, last 2 are CRPIX.
lon, lat: array
Sky coordinates.
u, v: array
Pixel coordinates
w_obj: `~astropy.wcs.WCS`
WCS object
"""
from astropy.modeling.models import SIP # here to avoid circular import
# unpack params
crpix = params[0:2]
cdx = params[2:6].reshape((2, 2))
a_params = params[6 : 6 + len(coeff_names)]
b_params = params[6 + len(coeff_names) :]
# assign to wcs, used for transformations in this function
w_obj.wcs.cd = cdx
w_obj.wcs.crpix = crpix
a_coeff, b_coeff = {}, {}
for i in range(len(coeff_names)):
a_coeff["A_" + coeff_names[i]] = a_params[i]
b_coeff["B_" + coeff_names[i]] = b_params[i]
sip = SIP(
crpix=crpix, a_order=order, b_order=order, a_coeff=a_coeff, b_coeff=b_coeff
)
fuv, guv = sip(u, v)
xo, yo = np.dot(cdx, np.array([u + fuv - crpix[0], v + guv - crpix[1]]))
# use all pix2world in case `projection` contains distortion table
x, y = w_obj.all_world2pix(lon, lat, 0)
x, y = np.dot(w_obj.wcs.cd, (x - w_obj.wcs.crpix[0], y - w_obj.wcs.crpix[1]))
resids = np.concatenate((x - xo, y - yo))
return resids |
Given two matching sets of coordinates on detector and sky,
compute the WCS.
Fits a WCS object to matched set of input detector and sky coordinates.
Optionally, a SIP can be fit to account for geometric
distortion. Returns an `~astropy.wcs.WCS` object with the best fit
parameters for mapping between input pixel and sky coordinates.
The projection type (default 'TAN') can passed in as a string, one of
the valid three-letter projection codes - or as a WCS object with
projection keywords already set. Note that if an input WCS has any
non-polynomial distortion, this will be applied and reflected in the
fit terms and coefficients. Passing in a WCS object in this way essentially
allows it to be refit based on the matched input coordinates and projection
point, but take care when using this option as non-projection related
keywords in the input might cause unexpected behavior.
Notes
-----
- The fiducial point for the spherical projection can be set to 'center'
to use the mean position of input sky coordinates, or as an
`~astropy.coordinates.SkyCoord` object.
- Units in all output WCS objects will always be in degrees.
- If the coordinate frame differs between `~astropy.coordinates.SkyCoord`
objects passed in for ``world_coords`` and ``proj_point``, the frame for
``world_coords`` will override as the frame for the output WCS.
- If a WCS object is passed in to ``projection`` the CD/PC matrix will
be used as an initial guess for the fit. If this is known to be
significantly off and may throw off the fit, set to the identity matrix
(for example, by doing wcs.wcs.pc = [(1., 0.,), (0., 1.)])
Parameters
----------
xy : (`numpy.ndarray`, `numpy.ndarray`) tuple
x & y pixel coordinates. These should be in FITS convention, starting
from (1,1) as the center of the bottom-left pixel.
world_coords : `~astropy.coordinates.SkyCoord`
Skycoord object with world coordinates.
proj_point : 'center' or ~astropy.coordinates.SkyCoord`
Defaults to 'center', in which the geometric center of input world
coordinates will be used as the projection point. To specify an exact
point for the projection, a Skycoord object with a coordinate pair can
be passed in. For consistency, the units and frame of these coordinates
will be transformed to match ``world_coords`` if they don't.
projection : str or `~astropy.wcs.WCS`
Three letter projection code, of any of standard projections defined
in the FITS WCS standard. Optionally, a WCS object with projection
keywords set may be passed in.
sip_degree : None or int
If set to a non-zero integer value, will fit SIP of degree
``sip_degree`` to model geometric distortion. Defaults to None, meaning
no distortion corrections will be fit.
Returns
-------
wcs : `~astropy.wcs.WCS`
The best-fit WCS to the points given. | def fit_wcs_from_points(
xy, world_coords, proj_point="center", projection="TAN", sip_degree=None
):
"""
Given two matching sets of coordinates on detector and sky,
compute the WCS.
Fits a WCS object to matched set of input detector and sky coordinates.
Optionally, a SIP can be fit to account for geometric
distortion. Returns an `~astropy.wcs.WCS` object with the best fit
parameters for mapping between input pixel and sky coordinates.
The projection type (default 'TAN') can passed in as a string, one of
the valid three-letter projection codes - or as a WCS object with
projection keywords already set. Note that if an input WCS has any
non-polynomial distortion, this will be applied and reflected in the
fit terms and coefficients. Passing in a WCS object in this way essentially
allows it to be refit based on the matched input coordinates and projection
point, but take care when using this option as non-projection related
keywords in the input might cause unexpected behavior.
Notes
-----
- The fiducial point for the spherical projection can be set to 'center'
to use the mean position of input sky coordinates, or as an
`~astropy.coordinates.SkyCoord` object.
- Units in all output WCS objects will always be in degrees.
- If the coordinate frame differs between `~astropy.coordinates.SkyCoord`
objects passed in for ``world_coords`` and ``proj_point``, the frame for
``world_coords`` will override as the frame for the output WCS.
- If a WCS object is passed in to ``projection`` the CD/PC matrix will
be used as an initial guess for the fit. If this is known to be
significantly off and may throw off the fit, set to the identity matrix
(for example, by doing wcs.wcs.pc = [(1., 0.,), (0., 1.)])
Parameters
----------
xy : (`numpy.ndarray`, `numpy.ndarray`) tuple
x & y pixel coordinates. These should be in FITS convention, starting
from (1,1) as the center of the bottom-left pixel.
world_coords : `~astropy.coordinates.SkyCoord`
Skycoord object with world coordinates.
proj_point : 'center' or ~astropy.coordinates.SkyCoord`
Defaults to 'center', in which the geometric center of input world
coordinates will be used as the projection point. To specify an exact
point for the projection, a Skycoord object with a coordinate pair can
be passed in. For consistency, the units and frame of these coordinates
will be transformed to match ``world_coords`` if they don't.
projection : str or `~astropy.wcs.WCS`
Three letter projection code, of any of standard projections defined
in the FITS WCS standard. Optionally, a WCS object with projection
keywords set may be passed in.
sip_degree : None or int
If set to a non-zero integer value, will fit SIP of degree
``sip_degree`` to model geometric distortion. Defaults to None, meaning
no distortion corrections will be fit.
Returns
-------
wcs : `~astropy.wcs.WCS`
The best-fit WCS to the points given.
"""
from scipy.optimize import least_squares
import astropy.units as u
from astropy.coordinates import SkyCoord # here to avoid circular import
from .wcs import Sip
xp, yp = xy
try:
lon, lat = world_coords.data.lon.deg, world_coords.data.lat.deg
except AttributeError:
unit_sph = world_coords.unit_spherical
lon, lat = unit_sph.lon.deg, unit_sph.lat.deg
# verify input
if (type(proj_point) != type(world_coords)) and (proj_point != "center"):
raise ValueError(
"proj_point must be set to 'center', or an"
"`~astropy.coordinates.SkyCoord` object with "
"a pair of points."
)
use_center_as_proj_point = str(proj_point) == "center"
if not use_center_as_proj_point:
assert proj_point.size == 1
proj_codes = [
"AZP",
"SZP",
"TAN",
"STG",
"SIN",
"ARC",
"ZEA",
"AIR",
"CYP",
"CEA",
"CAR",
"MER",
"SFL",
"PAR",
"MOL",
"AIT",
"COP",
"COE",
"COD",
"COO",
"BON",
"PCO",
"TSC",
"CSC",
"QSC",
"HPX",
"XPH",
]
if type(projection) == str:
if projection not in proj_codes:
raise ValueError(
"Must specify valid projection code from list of supported types: ",
", ".join(proj_codes),
)
# empty wcs to fill in with fit values
wcs = celestial_frame_to_wcs(frame=world_coords.frame, projection=projection)
else: # if projection is not string, should be wcs object. use as template.
wcs = copy.deepcopy(projection)
wcs.wcs.cdelt = (1.0, 1.0) # make sure cdelt is 1
wcs.sip = None
# Change PC to CD, since cdelt will be set to 1
if wcs.wcs.has_pc():
wcs.wcs.cd = wcs.wcs.pc
wcs.wcs.__delattr__("pc")
if (type(sip_degree) != type(None)) and (type(sip_degree) != int):
raise ValueError("sip_degree must be None, or integer.")
# compute bounding box for sources in image coordinates:
xpmin, xpmax, ypmin, ypmax = xp.min(), xp.max(), yp.min(), yp.max()
# set pixel_shape to span of input points
wcs.pixel_shape = (
1 if xpmax <= 0.0 else int(np.ceil(xpmax)),
1 if ypmax <= 0.0 else int(np.ceil(ypmax)),
)
# determine CRVAL from input
close = lambda l, p: p[np.argmin(np.abs(l))]
if use_center_as_proj_point: # use center of input points
sc1 = SkyCoord(lon.min() * u.deg, lat.max() * u.deg)
sc2 = SkyCoord(lon.max() * u.deg, lat.min() * u.deg)
pa = sc1.position_angle(sc2)
sep = sc1.separation(sc2)
midpoint_sc = sc1.directional_offset_by(pa, sep / 2)
wcs.wcs.crval = (midpoint_sc.data.lon.deg, midpoint_sc.data.lat.deg)
wcs.wcs.crpix = ((xpmax + xpmin) / 2.0, (ypmax + ypmin) / 2.0)
else: # convert units, initial guess for crpix
proj_point.transform_to(world_coords)
wcs.wcs.crval = (proj_point.data.lon.deg, proj_point.data.lat.deg)
wcs.wcs.crpix = (
close(lon - wcs.wcs.crval[0], xp + 1),
close(lon - wcs.wcs.crval[1], yp + 1),
)
# fit linear terms, assign to wcs
# use (1, 0, 0, 1) as initial guess, in case input wcs was passed in
# and cd terms are way off.
# Use bounds to require that the fit center pixel is on the input image
if xpmin == xpmax:
xpmin, xpmax = xpmin - 0.5, xpmax + 0.5
if ypmin == ypmax:
ypmin, ypmax = ypmin - 0.5, ypmax + 0.5
p0 = np.concatenate([wcs.wcs.cd.flatten(), wcs.wcs.crpix.flatten()])
fit = least_squares(
_linear_wcs_fit,
p0,
args=(lon, lat, xp, yp, wcs),
bounds=[
[-np.inf, -np.inf, -np.inf, -np.inf, xpmin + 1, ypmin + 1],
[np.inf, np.inf, np.inf, np.inf, xpmax + 1, ypmax + 1],
],
)
wcs.wcs.crpix = np.array(fit.x[4:6])
wcs.wcs.cd = np.array(fit.x[0:4].reshape((2, 2)))
# fit SIP, if specified. Only fit forward coefficients
if sip_degree:
degree = sip_degree
if "-SIP" not in wcs.wcs.ctype[0]:
wcs.wcs.ctype = [x + "-SIP" for x in wcs.wcs.ctype]
coef_names = [
f"{i}_{j}"
for i in range(degree + 1)
for j in range(degree + 1)
if (i + j) < (degree + 1) and (i + j) > 1
]
p0 = np.concatenate(
(
np.array(wcs.wcs.crpix),
wcs.wcs.cd.flatten(),
np.zeros(2 * len(coef_names)),
)
)
fit = least_squares(
_sip_fit,
p0,
args=(lon, lat, xp, yp, wcs, degree, coef_names),
bounds=[
[xpmin + 1, ypmin + 1] + [-np.inf] * (4 + 2 * len(coef_names)),
[xpmax + 1, ypmax + 1] + [np.inf] * (4 + 2 * len(coef_names)),
],
)
coef_fit = (
list(fit.x[6 : 6 + len(coef_names)]),
list(fit.x[6 + len(coef_names) :]),
)
# put fit values in wcs
wcs.wcs.cd = fit.x[2:6].reshape((2, 2))
wcs.wcs.crpix = fit.x[0:2]
a_vals = np.zeros((degree + 1, degree + 1))
b_vals = np.zeros((degree + 1, degree + 1))
for coef_name in coef_names:
a_vals[int(coef_name[0])][int(coef_name[2])] = coef_fit[0].pop(0)
b_vals[int(coef_name[0])][int(coef_name[2])] = coef_fit[1].pop(0)
wcs.sip = Sip(
a_vals,
b_vals,
np.zeros((degree + 1, degree + 1)),
np.zeros((degree + 1, degree + 1)),
wcs.wcs.crpix,
)
return wcs |
Convert a WCS obsgeo property into an ITRS coordinate frame.
Parameters
----------
obsgeo : array-like
A shape ``(6, )`` array representing ``OBSGEO-[XYZ], OBSGEO-[BLH]`` as
returned by ``WCS.wcs.obsgeo``.
obstime : time-like
The time associated with the coordinate, will be passed to
`~astropy.coordinates.ITRS` as the obstime keyword.
Returns
-------
~astropy.coordinates.ITRS
An `~astropy.coordinates.ITRS` coordinate frame
representing the coordinates.
Notes
-----
The obsgeo array as accessed on a `.WCS` object is a length 6 numpy array
where the first three elements are the coordinate in a cartesian
representation and the second 3 are the coordinate in a spherical
representation.
This function priorities reading the cartesian coordinates, and will only
read the spherical coordinates if the cartesian coordinates are either all
zero or any of the cartesian coordinates are non-finite.
In the case where both the spherical and cartesian coordinates have some
non-finite values the spherical coordinates will be returned with the
non-finite values included. | def obsgeo_to_frame(obsgeo, obstime):
"""
Convert a WCS obsgeo property into an ITRS coordinate frame.
Parameters
----------
obsgeo : array-like
A shape ``(6, )`` array representing ``OBSGEO-[XYZ], OBSGEO-[BLH]`` as
returned by ``WCS.wcs.obsgeo``.
obstime : time-like
The time associated with the coordinate, will be passed to
`~astropy.coordinates.ITRS` as the obstime keyword.
Returns
-------
~astropy.coordinates.ITRS
An `~astropy.coordinates.ITRS` coordinate frame
representing the coordinates.
Notes
-----
The obsgeo array as accessed on a `.WCS` object is a length 6 numpy array
where the first three elements are the coordinate in a cartesian
representation and the second 3 are the coordinate in a spherical
representation.
This function priorities reading the cartesian coordinates, and will only
read the spherical coordinates if the cartesian coordinates are either all
zero or any of the cartesian coordinates are non-finite.
In the case where both the spherical and cartesian coordinates have some
non-finite values the spherical coordinates will be returned with the
non-finite values included.
"""
if (
obsgeo is None
or len(obsgeo) != 6
or np.all(np.array(obsgeo) == 0)
or np.all(~np.isfinite(obsgeo))
):
raise ValueError(
f"Can not parse the 'obsgeo' location ({obsgeo}). "
"obsgeo should be a length 6 non-zero, finite numpy array"
)
# If the cartesian coords are zero or have NaNs in them use the spherical ones
if np.all(obsgeo[:3] == 0) or np.any(~np.isfinite(obsgeo[:3])):
data = SphericalRepresentation(*(obsgeo[3:] * (u.deg, u.deg, u.m)))
# Otherwise we assume the cartesian ones are valid
else:
data = CartesianRepresentation(*obsgeo[:3] * u.m)
return ITRS(data, obstime=obstime) |
Unpickles a WCS object from a serialized FITS string. | def __WCS_unpickle__(cls, dct, fits_data):
"""
Unpickles a WCS object from a serialized FITS string.
"""
self = cls.__new__(cls)
buffer = io.BytesIO(fits_data)
hdulist = fits.open(buffer)
naxis = dct.pop("naxis", None)
if naxis:
hdulist[0].header["naxis"] = naxis
naxes = dct.pop("_naxis", [])
for k, na in enumerate(naxes):
hdulist[0].header[f"naxis{k + 1:d}"] = na
kwargs = dct.pop("_init_kwargs", {})
self.__dict__.update(dct)
wcskey = dct.pop("_alt_wcskey", " ")
WCS.__init__(self, hdulist[0].header, hdulist, key=wcskey, **kwargs)
self.pixel_bounds = dct.get("_pixel_bounds", None)
return self |
Find all the WCS transformations in the given header.
Parameters
----------
header : str or `~astropy.io.fits.Header` object.
relax : bool or int, optional
Degree of permissiveness:
- `True` (default): Admit all recognized informal extensions of the
WCS standard.
- `False`: Recognize only FITS keywords defined by the
published WCS standard.
- `int`: a bit field selecting specific extensions to accept.
See :ref:`astropy:relaxread` for details.
keysel : sequence of str, optional
A list of flags used to select the keyword types considered by
wcslib. When ``None``, only the standard image header
keywords are considered (and the underlying wcspih() C
function is called). To use binary table image array or pixel
list keywords, *keysel* must be set.
Each element in the list should be one of the following strings:
- 'image': Image header keywords
- 'binary': Binary table image array keywords
- 'pixel': Pixel list keywords
Keywords such as ``EQUIna`` or ``RFRQna`` that are common to
binary table image arrays and pixel lists (including
``WCSNna`` and ``TWCSna``) are selected by both 'binary' and
'pixel'.
fix : bool, optional
When `True` (default), call `~astropy.wcs.Wcsprm.fix` on
the resulting objects to fix any non-standard uses in the
header. `FITSFixedWarning` warnings will be emitted if any
changes were made.
translate_units : str, optional
Specify which potentially unsafe translations of non-standard
unit strings to perform. By default, performs none. See
`WCS.fix` for more information about this parameter. Only
effective when ``fix`` is `True`.
Returns
-------
wcses : list of `WCS` | def find_all_wcs(
header, relax=True, keysel=None, fix=True, translate_units="", _do_set=True
):
"""
Find all the WCS transformations in the given header.
Parameters
----------
header : str or `~astropy.io.fits.Header` object.
relax : bool or int, optional
Degree of permissiveness:
- `True` (default): Admit all recognized informal extensions of the
WCS standard.
- `False`: Recognize only FITS keywords defined by the
published WCS standard.
- `int`: a bit field selecting specific extensions to accept.
See :ref:`astropy:relaxread` for details.
keysel : sequence of str, optional
A list of flags used to select the keyword types considered by
wcslib. When ``None``, only the standard image header
keywords are considered (and the underlying wcspih() C
function is called). To use binary table image array or pixel
list keywords, *keysel* must be set.
Each element in the list should be one of the following strings:
- 'image': Image header keywords
- 'binary': Binary table image array keywords
- 'pixel': Pixel list keywords
Keywords such as ``EQUIna`` or ``RFRQna`` that are common to
binary table image arrays and pixel lists (including
``WCSNna`` and ``TWCSna``) are selected by both 'binary' and
'pixel'.
fix : bool, optional
When `True` (default), call `~astropy.wcs.Wcsprm.fix` on
the resulting objects to fix any non-standard uses in the
header. `FITSFixedWarning` warnings will be emitted if any
changes were made.
translate_units : str, optional
Specify which potentially unsafe translations of non-standard
unit strings to perform. By default, performs none. See
`WCS.fix` for more information about this parameter. Only
effective when ``fix`` is `True`.
Returns
-------
wcses : list of `WCS`
"""
if isinstance(header, (str, bytes)):
header_string = header
elif isinstance(header, fits.Header):
header_string = header.tostring()
else:
raise TypeError("header must be a string or astropy.io.fits.Header object")
keysel_flags = _parse_keysel(keysel)
if isinstance(header_string, str):
header_bytes = header_string.encode("ascii")
else:
header_bytes = header_string
wcsprms = _wcs.find_all_wcs(header_bytes, relax, keysel_flags)
result = []
for wcsprm in wcsprms:
subresult = WCS(fix=False, _do_set=False)
subresult.wcs = wcsprm
result.append(subresult)
if fix:
subresult.fix(translate_units)
if _do_set:
subresult.wcs.set()
return result |
Prints a WCS validation report for the given FITS file.
Parameters
----------
source : str or file-like or `~astropy.io.fits.HDUList`
The FITS file to validate.
Returns
-------
results : list subclass instance
The result is returned as nested lists. The first level
corresponds to the HDUs in the given file. The next level has
an entry for each WCS found in that header. The special
subclass of list will pretty-print the results as a table when
printed. | def validate(source):
"""
Prints a WCS validation report for the given FITS file.
Parameters
----------
source : str or file-like or `~astropy.io.fits.HDUList`
The FITS file to validate.
Returns
-------
results : list subclass instance
The result is returned as nested lists. The first level
corresponds to the HDUs in the given file. The next level has
an entry for each WCS found in that header. The special
subclass of list will pretty-print the results as a table when
printed.
"""
class _WcsValidateWcsResult(list):
def __init__(self, key):
self._key = key
def __repr__(self):
result = [f" WCS key '{self._key or ' '}':"]
if len(self):
for entry in self:
for i, line in enumerate(entry.splitlines()):
if i == 0:
initial_indent = " - "
else:
initial_indent = " "
result.extend(
textwrap.wrap(
line,
initial_indent=initial_indent,
subsequent_indent=" ",
)
)
else:
result.append(" No issues.")
return "\n".join(result)
class _WcsValidateHduResult(list):
def __init__(self, hdu_index, hdu_name):
self._hdu_index = hdu_index
self._hdu_name = hdu_name
list.__init__(self)
def __repr__(self):
if len(self):
if self._hdu_name:
hdu_name = f" ({self._hdu_name})"
else:
hdu_name = ""
result = [f"HDU {self._hdu_index}{hdu_name}:"]
for wcs in self:
result.append(repr(wcs))
return "\n".join(result)
return ""
class _WcsValidateResults(list):
def __repr__(self):
result = []
for hdu in self:
content = repr(hdu)
if len(content):
result.append(content)
return "\n\n".join(result)
global __warningregistry__
if isinstance(source, fits.HDUList):
hdulist = source
close_file = False
else:
hdulist = fits.open(source)
close_file = True
results = _WcsValidateResults()
for i, hdu in enumerate(hdulist):
hdu_results = _WcsValidateHduResult(i, hdu.name)
results.append(hdu_results)
with warnings.catch_warnings(record=True) as warning_lines:
wcses = find_all_wcs(
hdu.header, relax=_wcs.WCSHDR_reject, fix=False, _do_set=False
)
for wcs in wcses:
wcs_results = _WcsValidateWcsResult(wcs.wcs.alt)
hdu_results.append(wcs_results)
try:
del __warningregistry__
except NameError:
pass
with warnings.catch_warnings(record=True) as warning_lines:
warnings.resetwarnings()
warnings.simplefilter("always", FITSFixedWarning, append=True)
try:
WCS(
hdu.header,
hdulist,
key=wcs.wcs.alt or " ",
relax=_wcs.WCSHDR_reject,
fix=True,
_do_set=False,
)
except WcsError as e:
wcs_results.append(str(e))
wcs_results.extend([str(x.message) for x in warning_lines])
if close_file:
hdulist.close()
return results |
Get the path to astropy.wcs's C header files. | def get_include():
"""
Get the path to astropy.wcs's C header files.
"""
import os
return os.path.join(os.path.dirname(__file__), "include") |
Test selection of a specific pixel list WCS using ``colsel``. See #11412. | def test_pixlist_wcs_colsel():
"""
Test selection of a specific pixel list WCS using ``colsel``. See #11412.
"""
hdr_file = get_pkg_data_filename("data/chandra-pixlist-wcs.hdr")
hdr = fits.Header.fromtextfile(hdr_file)
with pytest.warns(wcs.FITSFixedWarning):
w0 = wcs.WCS(hdr, keysel=["image", "pixel"], colsel=[11, 12])
with pytest.warns(wcs.FITSFixedWarning):
w = pickle.loads(pickle.dumps(w0))
assert w.naxis == 2
assert list(w.wcs.ctype) == ["RA---TAN", "DEC--TAN"]
assert np.allclose(w.wcs.crval, [229.38051931869, -58.81108068885])
assert np.allclose(w.wcs.pc, [[1, 0], [0, 1]])
assert np.allclose(w.wcs.cdelt, [-0.00013666666666666, 0.00013666666666666])
assert np.allclose(w.wcs.lonpole, 180.0) |
This WCS has an almost linear correlation between the pixel and world axes
close to the reference pixel. | def spatial_wcs_2d_small_angle():
"""
This WCS has an almost linear correlation between the pixel and world axes
close to the reference pixel.
"""
wcs = WCS(naxis=2)
wcs.wcs.ctype = ["HPLN-TAN", "HPLT-TAN"]
wcs.wcs.crpix = [3.0] * 2
wcs.wcs.cdelt = [0.002] * 2
wcs.wcs.crval = [0] * 2
wcs.wcs.set()
return wcs |
Regression test for https://github.com/astropy/astropy/pull/9609 | def test_pixel_to_world_itrs(x_in, y_in):
"""Regression test for https://github.com/astropy/astropy/pull/9609"""
if Version(_wcs.__version__) >= Version("7.4"):
ctx = pytest.warns(
FITSFixedWarning,
match=(
r"'datfix' made the change 'Set MJD-OBS to 57982\.528524 from"
r" DATE-OBS'\."
),
)
else:
ctx = nullcontext()
with ctx:
wcs = WCS(
{
"NAXIS": 2,
"CTYPE1": "TLON-CAR",
"CTYPE2": "TLAT-CAR",
"RADESYS": "ITRS ",
"DATE-OBS": "2017-08-17T12:41:04.444",
}
)
# This shouldn't raise an exception.
coord = wcs.pixel_to_world(x_in, y_in)
# Check round trip transformation.
x, y = wcs.world_to_pixel(coord)
np.testing.assert_almost_equal(x, x_in)
np.testing.assert_almost_equal(y, y_in) |
From github issue #36 | def test_fixes():
"""
From github issue #36
"""
header = get_pkg_data_contents("data/nonstandard_units.hdr", encoding="binary")
with (
pytest.raises(wcs.InvalidTransformError),
pytest.warns(wcs.FITSFixedWarning) as w,
):
wcs.WCS(header, translate_units="dhs")
if Version("7.4") <= _WCSLIB_VER < Version("7.6"):
assert len(w) == 3
assert "'datfix' made the change 'Success'." in str(w.pop().message)
else:
assert len(w) == 2
first_wmsg = str(w[0].message)
assert "unitfix" in first_wmsg and "Hz" in first_wmsg and "M/S" in first_wmsg
assert "plane angle" in str(w[1].message) and "m/s" in str(w[1].message) |
From github issue #107 | def test_outside_sky():
"""
From github issue #107
"""
header = get_pkg_data_contents("data/outside_sky.hdr", encoding="binary")
w = wcs.WCS(header)
assert np.all(np.isnan(w.wcs_pix2world([[100.0, 500.0]], 0))) # outside sky
assert np.all(np.isnan(w.wcs_pix2world([[200.0, 200.0]], 0))) # outside sky
assert not np.any(np.isnan(w.wcs_pix2world([[1000.0, 1000.0]], 0))) |
From github issue #1463 | def test_pix2world():
"""
From github issue #1463
"""
# TODO: write this to test the expected output behavior of pix2world,
# currently this just makes sure it doesn't error out in unexpected ways
# (and compares `wcs.pc` and `result` values?)
filename = get_pkg_data_filename("data/sip2.fits")
with pytest.warns(wcs.FITSFixedWarning) as caught_warnings:
# this raises a warning unimportant for this testing the pix2world
# FITSFixedWarning(u'The WCS transformation has more axes (2) than
# the image it is associated with (0)')
ww = wcs.WCS(filename)
# might as well monitor for changing behavior
if Version("7.4") <= _WCSLIB_VER < Version("7.6"):
assert len(caught_warnings) == 2
else:
assert len(caught_warnings) == 1
n = 3
pixels = (np.arange(n) * np.ones((2, n))).T
result = ww.wcs_pix2world(pixels, 0, ra_dec_order=True)
# Catch #2791
ww.wcs_pix2world(pixels[..., 0], pixels[..., 1], 0, ra_dec_order=True)
# assuming that the data of sip2.fits doesn't change
answer = np.array([[0.00024976, 0.00023018], [0.00023043, -0.00024997]])
assert np.allclose(ww.wcs.pc, answer, atol=1.0e-8)
answer = np.array(
[
[202.39265216, 47.17756518],
[202.39335826, 47.17754619],
[202.39406436, 47.1775272],
]
)
assert np.allclose(result, answer, atol=1.0e-8, rtol=1.0e-10) |
Test that WCS can be initialized with a dict-like object | def test_dict_init():
"""
Test that WCS can be initialized with a dict-like object
"""
# Dictionary with no actual WCS, returns identity transform
with ctx_for_v71_dateref_warnings():
w = wcs.WCS({})
xp, yp = w.wcs_world2pix(41.0, 2.0, 1)
assert_array_almost_equal_nulp(xp, 41.0, 10)
assert_array_almost_equal_nulp(yp, 2.0, 10)
# Valid WCS
hdr = {
"CTYPE1": "GLON-CAR",
"CTYPE2": "GLAT-CAR",
"CUNIT1": "deg",
"CUNIT2": "deg",
"CRPIX1": 1,
"CRPIX2": 1,
"CRVAL1": 40.0,
"CRVAL2": 0.0,
"CDELT1": -0.1,
"CDELT2": 0.1,
}
if _WCSLIB_VER >= Version("7.1"):
hdr["DATEREF"] = "1858-11-17"
if _WCSLIB_VER >= Version("7.4"):
ctx = pytest.warns(
wcs.wcs.FITSFixedWarning,
match=r"'datfix' made the change 'Set MJDREF to 0\.000000 from DATEREF'\.",
)
else:
ctx = nullcontext()
with ctx:
w = wcs.WCS(hdr)
xp, yp = w.wcs_world2pix(41.0, 2.0, 0)
assert_array_almost_equal_nulp(xp, -10.0, 10)
assert_array_almost_equal_nulp(yp, 20.0, 10) |
Issue #444 | def test_extra_kwarg():
"""
Issue #444
"""
w = wcs.WCS()
with NumpyRNGContext(123456789):
data = np.random.rand(100, 2)
with pytest.raises(TypeError):
w.wcs_pix2world(data, origin=1) |
Issue #444 | def test_3d_shapes():
"""
Issue #444
"""
w = wcs.WCS(naxis=3)
with NumpyRNGContext(123456789):
data = np.random.rand(100, 3)
result = w.wcs_pix2world(data, 1)
assert result.shape == (100, 3)
result = w.wcs_pix2world(data[..., 0], data[..., 1], data[..., 2], 1)
assert len(result) == 3 |
Issue #1395 | def test_invalid_shape():
"""Issue #1395"""
MESSAGE = r"When providing two arguments, the array must be of shape [(]N, 2[)]"
w = wcs.WCS(naxis=2)
xy = np.random.random((2, 3))
with pytest.raises(ValueError, match=MESSAGE):
w.wcs_pix2world(xy, 1)
xy = np.random.random((2, 1))
with pytest.raises(ValueError, match=MESSAGE):
w.wcs_pix2world(xy, 1) |
Causes a double free without a recent fix in wcslib_wrap.C | def test_find_all_wcs_crash():
"""
Causes a double free without a recent fix in wcslib_wrap.C
"""
with open(get_pkg_data_filename("data/too_many_pv.hdr")) as fd:
header = fd.read()
# We have to set fix=False here, because one of the fixing tasks is to
# remove redundant SCAMP distortion parameters when SIP distortion
# parameters are also present.
with pytest.raises(wcs.InvalidTransformError), pytest.warns(wcs.FITSFixedWarning):
wcs.find_all_wcs(header, fix=False) |
Test all_world2pix, iterative inverse of all_pix2world | def test_all_world2pix(
fname=None,
ext=0,
tolerance=1.0e-4,
origin=0,
random_npts=25000,
adaptive=False,
maxiter=20,
detect_divergence=True,
):
"""Test all_world2pix, iterative inverse of all_pix2world"""
# Open test FITS file:
if fname is None:
fname = get_pkg_data_filename("data/j94f05bgq_flt.fits")
ext = ("SCI", 1)
if not os.path.isfile(fname):
raise OSError(f"Input file '{fname:s}' to 'test_all_world2pix' not found.")
h = fits.open(fname)
w = wcs.WCS(h[ext].header, h)
h.close()
del h
crpix = w.wcs.crpix
ncoord = crpix.shape[0]
# Assume that CRPIX is at the center of the image and that the image has
# a power-of-2 number of pixels along each axis. Only use the central
# 1/64 for this testing purpose:
naxesi_l = list((7.0 / 16 * crpix).astype(int))
naxesi_u = list((9.0 / 16 * crpix).astype(int))
# Generate integer indices of pixels (image grid):
img_pix = np.dstack(
[i.flatten() for i in np.meshgrid(*map(range, naxesi_l, naxesi_u))]
)[0]
# Generate random data (in image coordinates):
with NumpyRNGContext(123456789):
rnd_pix = np.random.rand(random_npts, ncoord)
# Scale random data to cover the central part of the image
mwidth = 2 * (crpix * 1.0 / 8)
rnd_pix = crpix - 0.5 * mwidth + (mwidth - 1) * rnd_pix
# Reference pixel coordinates in image coordinate system (CS):
test_pix = np.append(img_pix, rnd_pix, axis=0)
# Reference pixel coordinates in sky CS using forward transformation:
all_world = w.all_pix2world(test_pix, origin)
try:
runtime_begin = datetime.now()
# Apply the inverse iterative process to pixels in world coordinates
# to recover the pixel coordinates in image space.
all_pix = w.all_world2pix(
all_world,
origin,
tolerance=tolerance,
adaptive=adaptive,
maxiter=maxiter,
detect_divergence=detect_divergence,
)
runtime_end = datetime.now()
except wcs.wcs.NoConvergence as e:
runtime_end = datetime.now()
ndiv = 0
if e.divergent is not None:
ndiv = e.divergent.shape[0]
print(f"There are {ndiv} diverging solutions.")
print(f"Indices of diverging solutions:\n{e.divergent}")
print(f"Diverging solutions:\n{e.best_solution[e.divergent]}\n")
print(
"Mean radius of the diverging solutions:"
f" {np.mean(np.linalg.norm(e.best_solution[e.divergent], axis=1))}"
)
print(
"Mean accuracy of the diverging solutions:"
f" {np.mean(np.linalg.norm(e.accuracy[e.divergent], axis=1))}\n"
)
else:
print("There are no diverging solutions.")
nslow = 0
if e.slow_conv is not None:
nslow = e.slow_conv.shape[0]
print(f"There are {nslow} slowly converging solutions.")
print(f"Indices of slowly converging solutions:\n{e.slow_conv}")
print(f"Slowly converging solutions:\n{e.best_solution[e.slow_conv]}\n")
else:
print("There are no slowly converging solutions.\n")
print(
f"There are {e.best_solution.shape[0] - ndiv - nslow} converged solutions."
)
print(f"Best solutions (all points):\n{e.best_solution}")
print(f"Accuracy:\n{e.accuracy}\n")
print(
"\nFinished running 'test_all_world2pix' with errors.\n"
f"ERROR: {e.args[0]}\nRun time: {runtime_end - runtime_begin}\n"
)
raise e
# Compute differences between reference pixel coordinates and
# pixel coordinates (in image space) recovered from reference
# pixels in world coordinates:
errors = np.sqrt(np.sum(np.power(all_pix - test_pix, 2), axis=1))
meanerr = np.mean(errors)
maxerr = np.amax(errors)
print(
"\nFinished running 'test_all_world2pix'.\n"
f"Mean error = {meanerr:e} (Max error = {maxerr:e})\n"
f"Run time: {runtime_end - runtime_begin}\n"
)
assert maxerr < 2.0 * tolerance |
Test parsing of WCS parameters with redundant SIP and SCAMP distortion
parameters. | def test_scamp_sip_distortion_parameters():
"""
Test parsing of WCS parameters with redundant SIP and SCAMP distortion
parameters.
"""
header = get_pkg_data_contents("data/validate.fits", encoding="binary")
with pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(header)
# Just check that this doesn't raise an exception.
w.all_pix2world(0, 0, 0) |
From github issue #1854 | def test_fixes2():
"""
From github issue #1854
"""
header = get_pkg_data_contents("data/nonstandard_units.hdr", encoding="binary")
with pytest.raises(wcs.InvalidTransformError):
wcs.WCS(header, fix=False) |
From github issue #1918 | def test_unit_normalization():
"""
From github issue #1918
"""
header = get_pkg_data_contents("data/unit.hdr", encoding="binary")
w = wcs.WCS(header)
assert w.wcs.cunit[2] == "m/s" |
From github issue #1912 | def test_footprint_to_file(tmp_path):
"""
From github issue #1912
"""
# Arbitrary keywords from real data
hdr = {
"CTYPE1": "RA---ZPN",
"CRUNIT1": "deg",
"CRPIX1": -3.3495999e02,
"CRVAL1": 3.185790700000e02,
"CTYPE2": "DEC--ZPN",
"CRUNIT2": "deg",
"CRPIX2": 3.0453999e03,
"CRVAL2": 4.388538000000e01,
"PV2_1": 1.0,
"PV2_3": 220.0,
"NAXIS1": 2048,
"NAXIS2": 1024,
}
w = wcs.WCS(hdr)
testfile = tmp_path / "test.txt"
w.footprint_to_file(testfile)
with open(testfile) as f:
lines = f.readlines()
assert len(lines) == 4
assert lines[2] == "ICRS\n"
assert "color=green" in lines[3]
w.footprint_to_file(testfile, coordsys="FK5", color="red")
with open(testfile) as f:
lines = f.readlines()
assert len(lines) == 4
assert lines[2] == "FK5\n"
assert "color=red" in lines[3]
with pytest.raises(ValueError):
w.footprint_to_file(testfile, coordsys="FOO")
del hdr["NAXIS1"]
del hdr["NAXIS2"]
w = wcs.WCS(hdr)
with pytest.warns(AstropyUserWarning):
w.footprint_to_file(testfile) |
From github issue #2053 | def test_validate_faulty_wcs():
"""
From github issue #2053
"""
h = fits.Header()
# Illegal WCS:
h["RADESYSA"] = "ICRS"
h["PV2_1"] = 1.0
hdu = fits.PrimaryHDU([[0]], header=h)
hdulist = fits.HDUList([hdu])
# Check that this doesn't raise a NameError exception
wcs.validate(hdulist) |
Test calc_footprint without distortion. | def test_calc_footprint_2():
"""Test calc_footprint without distortion."""
fits = get_pkg_data_filename("data/sip.fits")
with pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(fits)
axes = (1000, 1051)
ref = np.array(
[
[202.39265216, 47.17756518],
[202.7469062, 46.91483312],
[203.11487481, 47.14359319],
[202.76092671, 47.40745948],
]
)
footprint = w.calc_footprint(axes=axes, undistort=False)
assert_allclose(footprint, ref) |
Test calc_footprint with corner of the pixel. | def test_calc_footprint_3():
"""Test calc_footprint with corner of the pixel."""
w = wcs.WCS()
w.wcs.ctype = ["GLON-CAR", "GLAT-CAR"]
w.wcs.crpix = [1.5, 5.5]
w.wcs.cdelt = [-0.1, 0.1]
axes = (2, 10)
ref = np.array([[0.1, -0.5], [0.1, 0.5], [359.9, 0.5], [359.9, -0.5]])
footprint = w.calc_footprint(axes=axes, undistort=False, center=False)
assert_allclose(footprint, ref) |
Just make sure that it runs | def test_printwcs(capsys):
"""
Just make sure that it runs
"""
h = get_pkg_data_contents("data/spectra/orion-freq-1.hdr", encoding="binary")
with pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(h)
w.printwcs()
captured = capsys.readouterr()
assert "WCS Keywords" in captured.out
h = get_pkg_data_contents("data/3d_cd.hdr", encoding="binary")
w = wcs.WCS(h)
w.printwcs()
captured = capsys.readouterr()
assert "WCS Keywords" in captured.out |
Regression test for #3066 | def test_no_iteration():
"""Regression test for #3066"""
MESSAGE = "'{}' object is not iterable"
w = wcs.WCS(naxis=2)
with pytest.raises(TypeError, match=MESSAGE.format("WCS")):
iter(w)
class NewWCS(wcs.WCS):
pass
w = NewWCS(naxis=2)
with pytest.raises(TypeError, match=MESSAGE.format("NewWCS")):
iter(w) |
Regression test for https://github.com/astropy/astropy/issues/4612 | def test_no_truncate_crval():
"""
Regression test for https://github.com/astropy/astropy/issues/4612
"""
w = wcs.WCS(naxis=3)
w.wcs.crval = [50, 50, 2.12345678e11]
w.wcs.cdelt = [1e-3, 1e-3, 1e8]
w.wcs.ctype = ["RA---TAN", "DEC--TAN", "FREQ"]
w.wcs.set()
header = w.to_header()
for ii in range(3):
assert header[f"CRVAL{ii + 1}"] == w.wcs.crval[ii]
assert header[f"CDELT{ii + 1}"] == w.wcs.cdelt[ii] |
Regression test for https://github.com/astropy/astropy/issues/4612 | def test_no_truncate_crval_try2():
"""
Regression test for https://github.com/astropy/astropy/issues/4612
"""
w = wcs.WCS(naxis=3)
w.wcs.crval = [50, 50, 2.12345678e11]
w.wcs.cdelt = [1e-5, 1e-5, 1e5]
w.wcs.ctype = ["RA---SIN", "DEC--SIN", "FREQ"]
w.wcs.cunit = ["deg", "deg", "Hz"]
w.wcs.crpix = [1, 1, 1]
w.wcs.restfrq = 2.34e11
w.wcs.set()
header = w.to_header()
for ii in range(3):
assert header[f"CRVAL{ii + 1}"] == w.wcs.crval[ii]
assert header[f"CDELT{ii + 1}"] == w.wcs.cdelt[ii] |
Regression test for https://github.com/astropy/astropy/issues/5162 | def test_no_truncate_crval_p17():
"""
Regression test for https://github.com/astropy/astropy/issues/5162
"""
w = wcs.WCS(naxis=2)
w.wcs.crval = [50.1234567890123456, 50.1234567890123456]
w.wcs.cdelt = [1e-3, 1e-3]
w.wcs.ctype = ["RA---TAN", "DEC--TAN"]
w.wcs.set()
header = w.to_header()
assert header["CRVAL1"] != w.wcs.crval[0]
assert header["CRVAL2"] != w.wcs.crval[1]
header = w.to_header(relax=wcs.WCSHDO_P17)
assert header["CRVAL1"] == w.wcs.crval[0]
assert header["CRVAL2"] == w.wcs.crval[1] |
Regression test for https://github.com/astropy/astropy/issues/4612
This one uses WCS.wcs.compare and some slightly different values | def test_no_truncate_using_compare():
"""
Regression test for https://github.com/astropy/astropy/issues/4612
This one uses WCS.wcs.compare and some slightly different values
"""
w = wcs.WCS(naxis=3)
w.wcs.crval = [2.409303333333e02, 50, 2.12345678e11]
w.wcs.cdelt = [1e-3, 1e-3, 1e8]
w.wcs.ctype = ["RA---TAN", "DEC--TAN", "FREQ"]
w.wcs.set()
w2 = wcs.WCS(w.to_header())
w.wcs.compare(w2.wcs) |
Passing ImageHDU or PrimaryHDU and comparing it with
wcs initialized from header. For #4493. | def test_passing_ImageHDU():
"""
Passing ImageHDU or PrimaryHDU and comparing it with
wcs initialized from header. For #4493.
"""
path = get_pkg_data_filename("data/validate.fits")
with fits.open(path) as hdulist:
with pytest.warns(wcs.FITSFixedWarning):
wcs_hdu = wcs.WCS(hdulist[0])
wcs_header = wcs.WCS(hdulist[0].header)
assert wcs_hdu.wcs.compare(wcs_header.wcs)
wcs_hdu = wcs.WCS(hdulist[1])
wcs_header = wcs.WCS(hdulist[1].header)
assert wcs_hdu.wcs.compare(wcs_header.wcs) |
Test for #4814 | def test_inconsistent_sip():
"""
Test for #4814
"""
hdr = get_pkg_data_contents("data/sip-broken.hdr")
ctx = ctx_for_v71_dateref_warnings()
with ctx:
w = wcs.WCS(hdr)
with pytest.warns(AstropyWarning):
newhdr = w.to_header(relax=None)
# CTYPE should not include "-SIP" if relax is None
with ctx:
wnew = wcs.WCS(newhdr)
assert all(not ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype)
newhdr = w.to_header(relax=False)
assert "A_0_2" not in newhdr
# CTYPE should not include "-SIP" if relax is False
with ctx:
wnew = wcs.WCS(newhdr)
assert all(not ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype)
with pytest.warns(AstropyWarning):
newhdr = w.to_header(key="C")
assert "A_0_2" not in newhdr
# Test writing header with a different key
with ctx:
wnew = wcs.WCS(newhdr, key="C")
assert all(not ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype)
with pytest.warns(AstropyWarning):
newhdr = w.to_header(key=" ")
# Test writing a primary WCS to header
with ctx:
wnew = wcs.WCS(newhdr)
assert all(not ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype)
# Test that "-SIP" is kept into CTYPE if relax=True and
# "-SIP" was in the original header
newhdr = w.to_header(relax=True)
with ctx:
wnew = wcs.WCS(newhdr)
assert all(ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype)
assert "A_0_2" in newhdr
# Test that SIP coefficients are also written out.
assert wnew.sip is not None
# ######### broken header ###########
# Test that "-SIP" is added to CTYPE if relax=True and
# "-SIP" was not in the original header but SIP coefficients
# are present.
with ctx:
w = wcs.WCS(hdr)
w.wcs.ctype = ["RA---TAN", "DEC--TAN"]
newhdr = w.to_header(relax=True)
with ctx:
wnew = wcs.WCS(newhdr)
assert all(ctyp.endswith("-SIP") for ctyp in wnew.wcs.ctype) |
Test for #4957 | def test_bounds_check():
"""Test for #4957"""
w = wcs.WCS(naxis=2)
w.wcs.ctype = ["RA---CAR", "DEC--CAR"]
w.wcs.cdelt = [10, 10]
w.wcs.crval = [-90, 90]
w.wcs.crpix = [1, 1]
w.wcs.bounds_check(False, False)
ra, dec = w.wcs_pix2world(300, 0, 0)
assert_allclose(ra, -180)
assert_allclose(dec, -30) |
Test that when creating a WCS object using a key, CTYPE with
that key is looked at and not the primary CTYPE.
fix for #5443. | def test_sip_with_altkey():
"""
Test that when creating a WCS object using a key, CTYPE with
that key is looked at and not the primary CTYPE.
fix for #5443.
"""
with fits.open(get_pkg_data_filename("data/sip.fits")) as f:
with pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(f[0].header)
# create a header with two WCSs.
h1 = w.to_header(relax=True, key="A")
h2 = w.to_header(relax=False)
h1["CTYPE1A"] = "RA---SIN-SIP"
h1["CTYPE2A"] = "DEC--SIN-SIP"
h1.update(h2)
with ctx_for_v71_dateref_warnings():
w = wcs.WCS(h1, key="A")
assert (w.wcs.ctype == np.array(["RA---SIN-SIP", "DEC--SIN-SIP"])).all() |
Test to_fits() with LookupTable distortion. | def test_to_fits_1():
"""
Test to_fits() with LookupTable distortion.
"""
fits_name = get_pkg_data_filename("data/dist.fits")
if PYTEST_LT_8_0:
ctx = nullcontext()
else:
ctx = pytest.warns(
wcs.FITSFixedWarning, match="The WCS transformation has more axes"
)
with pytest.warns(AstropyDeprecationWarning), ctx:
w = wcs.WCS(fits_name)
wfits = w.to_fits()
assert isinstance(wfits, fits.HDUList)
assert isinstance(wfits[0], fits.PrimaryHDU)
assert isinstance(wfits[1], fits.ImageHDU) |
Test sip reading with extra key. | def test_keyedsip():
"""
Test sip reading with extra key.
"""
hdr_name = get_pkg_data_filename("data/sip-broken.hdr")
header = fits.Header.fromfile(hdr_name)
del header["CRPIX1"]
del header["CRPIX2"]
w = wcs.WCS(header=header, key="A")
assert isinstance(w.sip, wcs.Sip)
assert w.sip.crpix[0] == 2048
assert w.sip.crpix[1] == 1026 |
Issue #7845 | def test_scalar_inputs():
"""
Issue #7845
"""
wcsobj = wcs.WCS(naxis=1)
result = wcsobj.all_pix2world(2, 1)
assert_array_equal(result, [np.array(2.0)])
assert result[0].shape == ()
result = wcsobj.all_pix2world([2], 1)
assert_array_equal(result, [np.array([2.0])])
assert result[0].shape == (1,) |
Test WCS.footprint_contains(skycoord) | def test_footprint_contains():
"""
Test WCS.footprint_contains(skycoord)
"""
header = """
WCSAXES = 2 / Number of coordinate axes
CRPIX1 = 1045.0 / Pixel coordinate of reference point
CRPIX2 = 1001.0 / Pixel coordinate of reference point
PC1_1 = -0.00556448550786 / Coordinate transformation matrix element
PC1_2 = -0.001042120133257 / Coordinate transformation matrix element
PC2_1 = 0.001181477028705 / Coordinate transformation matrix element
PC2_2 = -0.005590809742987 / Coordinate transformation matrix element
CDELT1 = 1.0 / [deg] Coordinate increment at reference point
CDELT2 = 1.0 / [deg] Coordinate increment at reference point
CUNIT1 = 'deg' / Units of coordinate increment and value
CUNIT2 = 'deg' / Units of coordinate increment and value
CTYPE1 = 'RA---TAN' / TAN (gnomonic) projection + SIP distortions
CTYPE2 = 'DEC--TAN' / TAN (gnomonic) projection + SIP distortions
CRVAL1 = 250.34971683647 / [deg] Coordinate value at reference point
CRVAL2 = 2.2808772582495 / [deg] Coordinate value at reference point
LONPOLE = 180.0 / [deg] Native longitude of celestial pole
LATPOLE = 2.2808772582495 / [deg] Native latitude of celestial pole
RADESYS = 'ICRS' / Equatorial coordinate system
MJD-OBS = 58612.339199259 / [d] MJD of observation matching DATE-OBS
DATE-OBS= '2019-05-09T08:08:26.816Z' / ISO-8601 observation date matching MJD-OB
NAXIS = 2 / NAXIS
NAXIS1 = 2136 / length of first array dimension
NAXIS2 = 2078 / length of second array dimension
"""
header = fits.Header.fromstring(header.strip(), "\n")
test_wcs = wcs.WCS(header)
hasCoord = test_wcs.footprint_contains(SkyCoord(254, 2, unit="deg"))
assert hasCoord
hasCoord = test_wcs.footprint_contains(SkyCoord(240, 2, unit="deg"))
assert not hasCoord
hasCoord = test_wcs.footprint_contains(SkyCoord(24, 2, unit="deg"))
assert not hasCoord |
Test that plate distortion model is correctly described by `wcs.to_header()`
and preserved when creating a Cutout2D from the image, writing it to FITS,
and reading it back from the file. | def test_distortion_header(tmp_path):
"""
Test that plate distortion model is correctly described by `wcs.to_header()`
and preserved when creating a Cutout2D from the image, writing it to FITS,
and reading it back from the file.
"""
path = get_pkg_data_filename("data/dss.14.29.56-62.41.05.fits.gz")
cen = np.array((50, 50))
siz = np.array((20, 20))
if PYTEST_LT_8_0:
ctx = nullcontext()
else:
ctx = pytest.warns(VerifyWarning)
with fits.open(path) as hdulist:
with ctx, pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(hdulist[0].header)
cut = Cutout2D(hdulist[0].data, position=cen, size=siz, wcs=w)
# This converts the DSS plate solution model with AMD[XY]n coefficients into a
# Template Polynomial Distortion model (TPD.FWD.n coefficients);
# not testing explicitly for the header keywords here.
if _WCSLIB_VER < Version("7.4"):
with pytest.warns(
AstropyWarning, match="WCS contains a TPD distortion model in CQDIS"
):
w0 = wcs.WCS(w.to_header_string())
with pytest.warns(
AstropyWarning, match="WCS contains a TPD distortion model in CQDIS"
):
w1 = wcs.WCS(cut.wcs.to_header_string())
if _WCSLIB_VER >= Version("7.1"):
pytest.xfail("TPD coefficients incomplete with WCSLIB >= 7.1 < 7.4")
else:
w0 = wcs.WCS(w.to_header_string())
w1 = wcs.WCS(cut.wcs.to_header_string())
assert w.pixel_to_world(0, 0).separation(w0.pixel_to_world(0, 0)) < 1.0e-3 * u.mas
assert w.pixel_to_world(*cen).separation(w0.pixel_to_world(*cen)) < 1.0e-3 * u.mas
assert (
w.pixel_to_world(*cen).separation(w1.pixel_to_world(*(siz / 2)))
< 1.0e-3 * u.mas
)
cutfile = tmp_path / "cutout.fits"
fits.writeto(cutfile, cut.data, cut.wcs.to_header())
with fits.open(cutfile) as hdulist:
w2 = wcs.WCS(hdulist[0].header)
assert (
w.pixel_to_world(*cen).separation(w2.pixel_to_world(*(siz / 2)))
< 1.0e-3 * u.mas
) |
Test selection of a specific pixel list WCS using ``colsel``. See #11412. | def test_pixlist_wcs_colsel():
"""
Test selection of a specific pixel list WCS using ``colsel``. See #11412.
"""
hdr_file = get_pkg_data_filename("data/chandra-pixlist-wcs.hdr")
hdr = fits.Header.fromtextfile(hdr_file)
with pytest.warns(wcs.FITSFixedWarning):
w = wcs.WCS(hdr, keysel=["image", "pixel"], colsel=[11, 12])
assert w.naxis == 2
assert list(w.wcs.ctype) == ["RA---TAN", "DEC--TAN"]
assert np.allclose(w.wcs.crval, [229.38051931869, -58.81108068885])
assert np.allclose(w.wcs.pc, [[1, 0], [0, 1]])
assert np.allclose(w.wcs.cdelt, [-0.00013666666666666, 0.00013666666666666])
assert np.allclose(w.wcs.lonpole, 180.0) |
Issue #1960 | def test_sub_segfault():
"""Issue #1960"""
header = fits.Header.fromtextfile(get_pkg_data_filename("data/sub-segfault.hdr"))
w = wcs.WCS(header)
w.sub([wcs.WCSSUB_CELESTIAL])
gc.collect() |
Issue #1587 | def test_wcs_sub_error_message():
"""Issue #1587"""
w = _wcs.Wcsprm()
with pytest.raises(TypeError, match="axes must None, a sequence or an integer$"):
w.sub("latitude") |
Issue #3356 | def test_wcs_sub():
"""Issue #3356"""
w = _wcs.Wcsprm()
w.sub(["latitude"])
w = _wcs.Wcsprm()
w.sub([b"latitude"]) |
Convert value to an int or an int array.
Input coordinates converted to integers
corresponding to the center of the pixel.
The convention is that the center of the pixel is
(0, 0), while the lower left corner is (-0.5, -0.5).
The outputs are used to index the mask.
Examples
--------
>>> _toindex(np.array([-0.5, 0.49999]))
array([0, 0])
>>> _toindex(np.array([0.5, 1.49999]))
array([1, 1])
>>> _toindex(np.array([1.5, 2.49999]))
array([2, 2]) | def _toindex(value):
"""Convert value to an int or an int array.
Input coordinates converted to integers
corresponding to the center of the pixel.
The convention is that the center of the pixel is
(0, 0), while the lower left corner is (-0.5, -0.5).
The outputs are used to index the mask.
Examples
--------
>>> _toindex(np.array([-0.5, 0.49999]))
array([0, 0])
>>> _toindex(np.array([0.5, 1.49999]))
array([1, 1])
>>> _toindex(np.array([1.5, 2.49999]))
array([2, 2])
"""
indx = np.asarray(np.floor(np.asarray(value) + 0.5), dtype=int)
return indx |
Convert the input high level object to low level values.
This function uses the information in ``wcs.world_axis_object_classes`` and
``wcs.world_axis_object_components`` to convert the high level objects
(such as `~.SkyCoord`) to low level "values" `~.Quantity` objects.
This is used in `.HighLevelWCSMixin.world_to_pixel`, but provided as a
separate function for use in other places where needed.
Parameters
----------
*world_objects: object
High level coordinate objects.
low_level_wcs: `.BaseLowLevelWCS`
The WCS object to use to interpret the coordinates. | def high_level_objects_to_values(*world_objects, low_level_wcs):
"""
Convert the input high level object to low level values.
This function uses the information in ``wcs.world_axis_object_classes`` and
``wcs.world_axis_object_components`` to convert the high level objects
(such as `~.SkyCoord`) to low level "values" `~.Quantity` objects.
This is used in `.HighLevelWCSMixin.world_to_pixel`, but provided as a
separate function for use in other places where needed.
Parameters
----------
*world_objects: object
High level coordinate objects.
low_level_wcs: `.BaseLowLevelWCS`
The WCS object to use to interpret the coordinates.
"""
# Cache the classes and components since this may be expensive
serialized_classes = low_level_wcs.world_axis_object_classes
components = low_level_wcs.world_axis_object_components
# Deserialize world_axis_object_classes using the default order
classes = OrderedDict()
for key in default_order(components):
if low_level_wcs.serialized_classes:
classes[key] = deserialize_class(serialized_classes[key], construct=False)
else:
classes[key] = serialized_classes[key]
# Check that the number of classes matches the number of inputs
if len(world_objects) != len(classes):
raise ValueError(
f"Number of world inputs ({len(world_objects)}) does not match expected"
f" ({len(classes)})"
)
# Determine whether the classes are uniquely matched, that is we check
# whether there is only one of each class.
world_by_key = {}
unique_match = True
for w in world_objects:
matches = []
for key, (klass, *_) in classes.items():
if isinstance(w, klass):
matches.append(key)
if len(matches) == 1:
world_by_key[matches[0]] = w
else:
unique_match = False
break
# If the match is not unique, the order of the classes needs to match,
# whereas if all classes are unique, we can still intelligently match
# them even if the order is wrong.
objects = {}
if unique_match:
for key, (klass, args, kwargs, *rest) in classes.items():
if len(rest) == 0:
klass_gen = klass
elif len(rest) == 1:
klass_gen = rest[0]
else:
raise ValueError(
"Tuples in world_axis_object_classes should have length 3 or 4"
)
# FIXME: For now SkyCoord won't auto-convert upon initialization
# https://github.com/astropy/astropy/issues/7689
from astropy.coordinates import SkyCoord
if isinstance(world_by_key[key], SkyCoord):
if "frame" in kwargs:
objects[key] = world_by_key[key].transform_to(kwargs["frame"])
else:
objects[key] = world_by_key[key]
else:
objects[key] = klass_gen(world_by_key[key], *args, **kwargs)
else:
for ikey, key in enumerate(classes):
klass, args, kwargs, *rest = classes[key]
if len(rest) == 0:
klass_gen = klass
elif len(rest) == 1:
klass_gen = rest[0]
else:
raise ValueError(
"Tuples in world_axis_object_classes should have length 3 or 4"
)
w = world_objects[ikey]
if not isinstance(w, klass):
raise ValueError(
"Expected the following order of world arguments:"
f" {', '.join([k.__name__ for (k, *_) in classes.values()])}"
)
# FIXME: For now SkyCoord won't auto-convert upon initialization
# https://github.com/astropy/astropy/issues/7689
from astropy.coordinates import SkyCoord
if isinstance(w, SkyCoord):
if "frame" in kwargs:
objects[key] = w.transform_to(kwargs["frame"])
else:
objects[key] = w
else:
objects[key] = klass_gen(w, *args, **kwargs)
# We now extract the attributes needed for the world values
world = []
for key, _, attr in components:
if callable(attr):
world.append(attr(objects[key]))
else:
world.append(rec_getattr(objects[key], attr))
return world |
Convert low level values into high level objects.
This function uses the information in ``wcs.world_axis_object_classes`` and
``wcs.world_axis_object_components`` to convert low level "values"
`~.Quantity` objects, to high level objects (such as `~.SkyCoord).
This is used in `.HighLevelWCSMixin.pixel_to_world`, but provided as a
separate function for use in other places where needed.
Parameters
----------
*world_values: object
Low level, "values" representations of the world coordinates.
low_level_wcs: `.BaseLowLevelWCS`
The WCS object to use to interpret the coordinates. | def values_to_high_level_objects(*world_values, low_level_wcs):
"""
Convert low level values into high level objects.
This function uses the information in ``wcs.world_axis_object_classes`` and
``wcs.world_axis_object_components`` to convert low level "values"
`~.Quantity` objects, to high level objects (such as `~.SkyCoord).
This is used in `.HighLevelWCSMixin.pixel_to_world`, but provided as a
separate function for use in other places where needed.
Parameters
----------
*world_values: object
Low level, "values" representations of the world coordinates.
low_level_wcs: `.BaseLowLevelWCS`
The WCS object to use to interpret the coordinates.
"""
# Cache the classes and components since this may be expensive
components = low_level_wcs.world_axis_object_components
classes = low_level_wcs.world_axis_object_classes
# Deserialize classes
if low_level_wcs.serialized_classes:
classes_new = {}
for key, value in classes.items():
classes_new[key] = deserialize_class(value, construct=False)
classes = classes_new
args = defaultdict(list)
kwargs = defaultdict(dict)
for i, (key, attr, _) in enumerate(components):
if isinstance(attr, str):
kwargs[key][attr] = world_values[i]
else:
while attr > len(args[key]) - 1:
args[key].append(None)
args[key][attr] = world_values[i]
result = []
for key in default_order(components):
klass, ar, kw, *rest = classes[key]
if len(rest) == 0:
klass_gen = klass
elif len(rest) == 1:
klass_gen = rest[0]
else:
raise ValueError(
"Tuples in world_axis_object_classes should have length 3 or 4"
)
result.append(klass_gen(*args[key], *ar, **kwargs[key], **kw))
return result |
Validate a list of physical types against the UCD1+ standard. | def validate_physical_types(physical_types):
"""
Validate a list of physical types against the UCD1+ standard.
"""
for physical_type in physical_types:
if (
physical_type is not None
and physical_type not in VALID_UCDS
and not physical_type.startswith("custom:")
):
raise ValueError(
f"'{physical_type}' is not a valid IOVA UCD1+ physical type. It must be"
" a string specified in the list"
" (http://www.ivoa.net/documents/latest/UCDlist.html) or if no"
" matching type exists it can be any string prepended with 'custom:'."
) |
Deserialize classes recursively. | def deserialize_class(tpl, construct=True):
"""
Deserialize classes recursively.
"""
if not isinstance(tpl, tuple) or len(tpl) != 3:
raise ValueError("Expected a tuple of three values")
module, klass = tpl[0].rsplit(".", 1)
module = importlib.import_module(module)
klass = getattr(module, klass)
args = tuple(
deserialize_class(arg) if isinstance(arg, tuple) else arg for arg in tpl[1]
)
kwargs = dict(
(key, deserialize_class(val)) if isinstance(val, tuple) else (key, val)
for (key, val) in tpl[2].items()
)
if construct:
return klass(*args, **kwargs)
else:
return klass, args, kwargs |
Test case for issue #11446
Since we can't define a target accuracy when plotting a WCS `all_world2pix`
should not error but only warn when the default accuracy can't be reached. | def test_non_convergence_warning():
"""Test case for issue #11446
Since we can't define a target accuracy when plotting a WCS `all_world2pix`
should not error but only warn when the default accuracy can't be reached.
"""
# define a minimal WCS where convergence fails for certain image positions
wcs = WCS(naxis=2)
crpix = [0, 0]
a = b = ap = bp = np.zeros((4, 4))
a[3, 0] = -1.20116753e-07
test_pos_x = [1000, 1]
test_pos_y = [0, 2]
wcs.sip = Sip(a, b, ap, bp, crpix)
# first make sure the WCS works when using a low accuracy
expected = wcs.all_world2pix(test_pos_x, test_pos_y, 0, tolerance=1e-3)
# then check that it fails when using the default accuracy
with pytest.raises(NoConvergence):
wcs.all_world2pix(test_pos_x, test_pos_y, 0)
# at last check that world_to_pixel_values raises a warning but returns
# the same 'low accuray' result
with pytest.warns(UserWarning):
assert_allclose(wcs.world_to_pixel_values(test_pos_x, test_pos_y), expected) |
This test is a regression test for https://github.com/astropy/astropy/issues/12095
It checks the following:
- If a spatial WCS isn't converted to units of deg by wcslib it still works.
- If TIMESYS is upper case we parse it correctly
- If a TIME CTYPE key has an algorithm code (in this case -TAB) it still works.
The file used here was generated by gWCS and then edited to add the TIMESYS key. | def test_fits_tab_time_and_units():
"""
This test is a regression test for https://github.com/astropy/astropy/issues/12095
It checks the following:
- If a spatial WCS isn't converted to units of deg by wcslib it still works.
- If TIMESYS is upper case we parse it correctly
- If a TIME CTYPE key has an algorithm code (in this case -TAB) it still works.
The file used here was generated by gWCS and then edited to add the TIMESYS key.
"""
with (
fits.open(get_pkg_data_filename("data/example_4d_tab.fits")) as hdul,
pytest.warns(FITSFixedWarning),
):
w = WCS(header=hdul[0].header, fobj=hdul)
with warnings.catch_warnings():
warnings.filterwarnings("ignore", message=r".*dubious year \(Note \d\)")
world = w.pixel_to_world(0, 0, 0, 0)
assert isinstance(world[0], SkyCoord)
assert world[0].data.lat.unit is u.arcsec
assert world[0].data.lon.unit is u.arcsec
assert u.allclose(world[0].l, 0.06475506 * u.deg)
assert u.allclose(world[0].b, -0.02430561 * u.deg)
assert isinstance(world[1], SpectralCoord)
assert u.allclose(world[1], 24.96 * u.Hz)
assert isinstance(world[2], Time)
assert world[2].scale == "utc"
assert u.allclose(world[2].mjd, 0.00032986111111110716) |
Given a slice as input sanitise it to an easier to parse format.format.
This function returns a list ``ndim`` long containing slice objects (or ints). | def sanitize_slices(slices, ndim):
"""
Given a slice as input sanitise it to an easier to parse format.format.
This function returns a list ``ndim`` long containing slice objects (or ints).
"""
if not isinstance(slices, (tuple, list)): # We just have a single int
slices = (slices,)
if len(slices) > ndim:
raise ValueError(
f"The dimensionality of the specified slice {slices} can not be greater "
f"than the dimensionality ({ndim}) of the wcs."
)
if any(isiterable(s) for s in slices):
raise IndexError(
"This slice is invalid, only integer or range slices are supported."
)
slices = list(slices)
if Ellipsis in slices:
if slices.count(Ellipsis) > 1:
raise IndexError("an index can only have a single ellipsis ('...')")
# Replace the Ellipsis with the correct number of slice(None)s
e_ind = slices.index(Ellipsis)
slices.remove(Ellipsis)
n_e = ndim - len(slices)
for i in range(n_e):
ind = e_ind + i
slices.insert(ind, slice(None))
for i in range(ndim):
if i < len(slices):
slc = slices[i]
if isinstance(slc, slice):
if slc.step and slc.step != 1:
raise IndexError("Slicing WCS with a step is not supported.")
elif not isinstance(slc, numbers.Integral):
raise IndexError("Only integer or range slices are accepted.")
else:
slices.append(slice(None))
return slices |
Given two slices that can be applied to a 1-d array, find the resulting
slice that corresponds to the combination of both slices. We assume that
slice2 can be an integer, but slice1 cannot. | def combine_slices(slice1, slice2):
"""
Given two slices that can be applied to a 1-d array, find the resulting
slice that corresponds to the combination of both slices. We assume that
slice2 can be an integer, but slice1 cannot.
"""
if isinstance(slice1, slice) and slice1.step is not None:
raise ValueError("Only slices with steps of 1 are supported")
if isinstance(slice2, slice) and slice2.step is not None:
raise ValueError("Only slices with steps of 1 are supported")
if isinstance(slice2, numbers.Integral):
if slice1.start is None:
return slice2
else:
return slice2 + slice1.start
if slice1.start is None:
if slice1.stop is None:
return slice2
else:
if slice2.stop is None:
return slice(slice2.start, slice1.stop)
else:
return slice(slice2.start, min(slice1.stop, slice2.stop))
else:
if slice2.start is None:
start = slice1.start
else:
start = slice1.start + slice2.start
if slice2.stop is None:
stop = slice1.stop
else:
if slice1.start is None:
stop = slice2.stop
else:
stop = slice2.stop + slice1.start
if slice1.stop is not None:
stop = min(slice1.stop, stop)
return slice(start, stop) |
Render pages as a jinja template to hide/show dev docs. | def rstjinja(app, docname, source):
"""Render pages as a jinja template to hide/show dev docs."""
# Make sure we're outputting HTML
if app.builder.format != "html":
return
files_to_render = ["index_dev", "install"]
if docname in files_to_render:
logger.info("Jinja rendering %s", docname)
rendered = app.builder.templates.render_string(
source[0], app.config.html_context
)
source[0] = rendered |
Reference targets for ``astropy:`` and ``astropy-dev:`` are special cases.
Documentation links in astropy can be set up as intersphinx links so that
affiliate packages do not have to override the docstrings when building
the docs.
If we are building the development docs it is a local ref targeting the
label ``astropy-dev:<label>``, but for stable docs it should be an
intersphinx resolution to the development docs.
See https://github.com/astropy/astropy/issues/11366 | def resolve_astropy_and_dev_reference(app, env, node, contnode):
"""
Reference targets for ``astropy:`` and ``astropy-dev:`` are special cases.
Documentation links in astropy can be set up as intersphinx links so that
affiliate packages do not have to override the docstrings when building
the docs.
If we are building the development docs it is a local ref targeting the
label ``astropy-dev:<label>``, but for stable docs it should be an
intersphinx resolution to the development docs.
See https://github.com/astropy/astropy/issues/11366
"""
# should the node be processed?
reftarget = node.get("reftarget") # str or None
if str(reftarget).startswith("astropy:"):
# This allows Astropy to use intersphinx links to itself and have
# them resolve to local links. Downstream packages will see intersphinx.
# TODO! deprecate this if sphinx-doc/sphinx/issues/9169 is implemented.
process, replace = True, "astropy:"
elif dev and str(reftarget).startswith("astropy-dev:"):
process, replace = True, "astropy-dev:"
else:
process, replace = False, ""
# make link local
if process:
reftype = node.get("reftype")
refdoc = node.get("refdoc", app.env.docname)
# convert astropy intersphinx targets to local links.
# there are a few types of intersphinx link patterns, as described in
# https://docs.readthedocs.io/en/stable/guides/intersphinx.html
reftarget = reftarget.replace(replace, "")
if reftype == "doc": # also need to replace the doc link
node.replace_attr("reftarget", reftarget)
# Delegate to the ref node's original domain/target (typically :ref:)
try:
domain = app.env.domains[node["refdomain"]]
return domain.resolve_xref(
app.env, refdoc, app.builder, reftype, reftarget, node, contnode
)
except Exception:
pass |
Run doctests in isolated tmp_path so outputs do not end up in repo. | def _docdir(request):
"""Run doctests in isolated tmp_path so outputs do not end up in repo."""
# Trigger ONLY for doctestplus
doctest_plugin = request.config.pluginmanager.getplugin("doctestplus")
if isinstance(request.node.parent, doctest_plugin._doctest_textfile_item_cls):
# Don't apply this fixture to io.rst. It reads files and doesn't write.
# Implementation from https://github.com/pytest-dev/pytest/discussions/10437
if "io.rst" not in request.node.name:
old_cwd = os.getcwd()
tmp_path = request.getfixturevalue("tmp_path")
os.chdir(tmp_path)
yield
os.chdir(old_cwd)
else:
yield
else:
yield |
Compute the Galactic spherical to heliocentric Sgr transformation matrix. | def galactic_to_sgr():
"""Compute the Galactic spherical to heliocentric Sgr transformation matrix."""
return SGR_MATRIX |
Compute the heliocentric Sgr to spherical Galactic transformation matrix. | def sgr_to_galactic():
"""Compute the heliocentric Sgr to spherical Galactic transformation matrix."""
return matrix_transpose(SGR_MATRIX) |
Transform a barycentric radial velocity to the Galactic Standard of Rest
(GSR).
The input radial velocity must be passed in as a
Parameters
----------
c : `~astropy.coordinates.BaseCoordinateFrame` subclass instance
The radial velocity, associated with a sky coordinates, to be
transformed.
v_sun : `~astropy.units.Quantity`, optional
The 3D velocity of the solar system barycenter in the GSR frame.
Defaults to the same solar motion as in the
`~astropy.coordinates.Galactocentric` frame.
Returns
-------
v_gsr : `~astropy.units.Quantity`
The input radial velocity transformed to a GSR frame. | def rv_to_gsr(c, v_sun=None):
"""Transform a barycentric radial velocity to the Galactic Standard of Rest
(GSR).
The input radial velocity must be passed in as a
Parameters
----------
c : `~astropy.coordinates.BaseCoordinateFrame` subclass instance
The radial velocity, associated with a sky coordinates, to be
transformed.
v_sun : `~astropy.units.Quantity`, optional
The 3D velocity of the solar system barycenter in the GSR frame.
Defaults to the same solar motion as in the
`~astropy.coordinates.Galactocentric` frame.
Returns
-------
v_gsr : `~astropy.units.Quantity`
The input radial velocity transformed to a GSR frame.
"""
if v_sun is None:
v_sun = coord.Galactocentric().galcen_v_sun.to_cartesian()
gal = c.transform_to(coord.Galactic)
cart_data = gal.data.to_cartesian()
unit_vector = cart_data / cart_data.norm()
v_proj = v_sun.dot(unit_vector)
return c.radial_velocity + v_proj |
Dummy function to make sure docstrings don't get rendered as text | def dummy() -> None:
"""Dummy function to make sure docstrings don't get rendered as text""" |
Convert primitive modules to float16. | def convert_module_to_f16(l):
"""
Convert primitive modules to float16.
"""
if isinstance(l, (nn.Conv1d, nn.Conv2d, nn.Conv3d)):
l.weight.data = l.weight.data.half()
if l.bias is not None:
l.bias.data = l.bias.data.half() |
Convert primitive modules to float32, undoing convert_module_to_f16(). | def convert_module_to_f32(l):
"""
Convert primitive modules to float32, undoing convert_module_to_f16().
"""
if isinstance(l, (nn.Conv1d, nn.Conv2d, nn.Conv3d)):
l.weight.data = l.weight.data.float()
if l.bias is not None:
l.bias.data = l.bias.data.float() |
Copy model parameters into a (differently-shaped) list of full-precision
parameters. | def make_master_params(param_groups_and_shapes):
"""
Copy model parameters into a (differently-shaped) list of full-precision
parameters.
"""
master_params = []
for param_group, shape in param_groups_and_shapes:
master_param = nn.Parameter(
_flatten_dense_tensors(
[param.detach().float() for (_, param) in param_group]
).view(shape)
)
master_param.requires_grad = True
master_params.append(master_param)
return master_params |
Copy the gradients from the model parameters into the master parameters
from make_master_params(). | def model_grads_to_master_grads(param_groups_and_shapes, master_params):
"""
Copy the gradients from the model parameters into the master parameters
from make_master_params().
"""
for master_param, (param_group, shape) in zip(
master_params, param_groups_and_shapes
):
master_param.grad = _flatten_dense_tensors(
[param_grad_or_zeros(param) for (_, param) in param_group]
).view(shape) |
Copy the master parameter data back into the model parameters. | def master_params_to_model_params(param_groups_and_shapes, master_params):
"""
Copy the master parameter data back into the model parameters.
"""
# Without copying to a list, if a generator is passed, this will
# silently not copy any parameters.
for master_param, (param_group, _) in zip(master_params, param_groups_and_shapes):
for (_, param), unflat_master_param in zip(
param_group, unflatten_master_params(param_group, master_param.view(-1))
):
param.detach().copy_(unflat_master_param) |
Get a pre-defined beta schedule for the given name.
The beta schedule library consists of beta schedules which remain similar
in the limit of num_diffusion_timesteps.
Beta schedules may be added, but should not be removed or changed once
they are committed to maintain backwards compatibility. | def get_named_beta_schedule(schedule_name, num_diffusion_timesteps, scale_betas=1.0):
"""
Get a pre-defined beta schedule for the given name.
The beta schedule library consists of beta schedules which remain similar
in the limit of num_diffusion_timesteps.
Beta schedules may be added, but should not be removed or changed once
they are committed to maintain backwards compatibility.
"""
if schedule_name == "linear":
# Linear schedule from Ho et al, extended to work for any number of
# diffusion steps.
scale = scale_betas * 1000 / num_diffusion_timesteps
beta_start = scale * 0.0001
beta_end = scale * 0.02
return np.linspace(
beta_start, beta_end, num_diffusion_timesteps, dtype=np.float64
)
elif schedule_name == "cosine":
return betas_for_alpha_bar(
num_diffusion_timesteps,
lambda t: math.cos((t + 0.008) / 1.008 * math.pi / 2) ** 2,
)
else:
raise NotImplementedError(f"unknown beta schedule: {schedule_name}") |
Create a beta schedule that discretizes the given alpha_t_bar function,
which defines the cumulative product of (1-beta) over time from t = [0,1].
:param num_diffusion_timesteps: the number of betas to produce.
:param alpha_bar: a lambda that takes an argument t from 0 to 1 and
produces the cumulative product of (1-beta) up to that
part of the diffusion process.
:param max_beta: the maximum beta to use; use values lower than 1 to
prevent singularities. | def betas_for_alpha_bar(num_diffusion_timesteps, alpha_bar, max_beta=0.999):
"""
Create a beta schedule that discretizes the given alpha_t_bar function,
which defines the cumulative product of (1-beta) over time from t = [0,1].
:param num_diffusion_timesteps: the number of betas to produce.
:param alpha_bar: a lambda that takes an argument t from 0 to 1 and
produces the cumulative product of (1-beta) up to that
part of the diffusion process.
:param max_beta: the maximum beta to use; use values lower than 1 to
prevent singularities.
"""
betas = []
for i in range(num_diffusion_timesteps):
t1 = i / num_diffusion_timesteps
t2 = (i + 1) / num_diffusion_timesteps
betas.append(min(1 - alpha_bar(t2) / alpha_bar(t1), max_beta))
return np.array(betas) |
Extract values from a 1-D numpy array for a batch of indices.
:param arr: the 1-D numpy array.
:param timesteps: a tensor of indices into the array to extract.
:param broadcast_shape: a larger shape of K dimensions with the batch
dimension equal to the length of timesteps.
:return: a tensor of shape [batch_size, 1, ...] where the shape has K dims. | def _extract_into_tensor(arr, timesteps, broadcast_shape):
"""
Extract values from a 1-D numpy array for a batch of indices.
:param arr: the 1-D numpy array.
:param timesteps: a tensor of indices into the array to extract.
:param broadcast_shape: a larger shape of K dimensions with the batch
dimension equal to the length of timesteps.
:return: a tensor of shape [batch_size, 1, ...] where the shape has K dims.
"""
res = th.from_numpy(arr).to(device=timesteps.device)[timesteps].float()
while len(res.shape) < len(broadcast_shape):
res = res[..., None]
return res.expand(broadcast_shape) |
Compute the KL divergence between two gaussians.
Shapes are automatically broadcasted, so batches can be compared to
scalars, among other use cases. | def normal_kl(mean1, logvar1, mean2, logvar2):
"""
Compute the KL divergence between two gaussians.
Shapes are automatically broadcasted, so batches can be compared to
scalars, among other use cases.
"""
tensor = None
for obj in (mean1, logvar1, mean2, logvar2):
if isinstance(obj, th.Tensor):
tensor = obj
break
assert tensor is not None, "at least one argument must be a Tensor"
# Force variances to be Tensors. Broadcasting helps convert scalars to
# Tensors, but it does not work for th.exp().
logvar1, logvar2 = [
x if isinstance(x, th.Tensor) else th.tensor(x).to(tensor)
for x in (logvar1, logvar2)
]
return 0.5 * (
-1.0
+ logvar2
- logvar1
+ th.exp(logvar1 - logvar2)
+ ((mean1 - mean2) ** 2) * th.exp(-logvar2)
) |
A fast approximation of the cumulative distribution function of the
standard normal. | def approx_standard_normal_cdf(x):
"""
A fast approximation of the cumulative distribution function of the
standard normal.
"""
return 0.5 * (1.0 + th.tanh(np.sqrt(2.0 / np.pi) * (x + 0.044715 * th.pow(x, 3)))) |
Compute the log-likelihood of a Gaussian distribution discretizing to a
given image.
:param x: the target images. It is assumed that this was uint8 values,
rescaled to the range [-1, 1].
:param means: the Gaussian mean Tensor.
:param log_scales: the Gaussian log stddev Tensor.
:return: a tensor like x of log probabilities (in nats). | def discretized_gaussian_log_likelihood(x, *, means, log_scales):
"""
Compute the log-likelihood of a Gaussian distribution discretizing to a
given image.
:param x: the target images. It is assumed that this was uint8 values,
rescaled to the range [-1, 1].
:param means: the Gaussian mean Tensor.
:param log_scales: the Gaussian log stddev Tensor.
:return: a tensor like x of log probabilities (in nats).
"""
assert x.shape == means.shape == log_scales.shape
centered_x = x - means
inv_stdv = th.exp(-log_scales)
plus_in = inv_stdv * (centered_x + 1.0 / 255.0)
cdf_plus = approx_standard_normal_cdf(plus_in)
min_in = inv_stdv * (centered_x - 1.0 / 255.0)
cdf_min = approx_standard_normal_cdf(min_in)
log_cdf_plus = th.log(cdf_plus.clamp(min=1e-12))
log_one_minus_cdf_min = th.log((1.0 - cdf_min).clamp(min=1e-12))
cdf_delta = cdf_plus - cdf_min
log_probs = th.where(
x < -0.999,
log_cdf_plus,
th.where(x > 0.999, log_one_minus_cdf_min, th.log(cdf_delta.clamp(min=1e-12))),
)
assert log_probs.shape == x.shape
return log_probs |
Create a 1D, 2D, or 3D convolution module. | def conv_nd(dims, *args, **kwargs):
"""
Create a 1D, 2D, or 3D convolution module.
"""
if dims == 1:
return nn.Conv1d(*args, **kwargs)
elif dims == 2:
return nn.Conv2d(*args, **kwargs)
elif dims == 3:
return nn.Conv3d(*args, **kwargs)
raise ValueError(f"unsupported dimensions: {dims}") |
Create a linear module. | def linear(*args, **kwargs):
"""
Create a linear module.
"""
return nn.Linear(*args, **kwargs) |
Create a 1D, 2D, or 3D average pooling module. | def avg_pool_nd(dims, *args, **kwargs):
"""
Create a 1D, 2D, or 3D average pooling module.
"""
if dims == 1:
return nn.AvgPool1d(*args, **kwargs)
elif dims == 2:
return nn.AvgPool2d(*args, **kwargs)
elif dims == 3:
return nn.AvgPool3d(*args, **kwargs)
raise ValueError(f"unsupported dimensions: {dims}") |
Update target parameters to be closer to those of source parameters using
an exponential moving average.
:param target_params: the target parameter sequence.
:param source_params: the source parameter sequence.
:param rate: the EMA rate (closer to 1 means slower). | def update_ema(target_params, source_params, rate=0.99):
"""
Update target parameters to be closer to those of source parameters using
an exponential moving average.
:param target_params: the target parameter sequence.
:param source_params: the source parameter sequence.
:param rate: the EMA rate (closer to 1 means slower).
"""
for targ, src in zip(target_params, source_params):
targ.detach().mul_(rate).add_(src, alpha=1 - rate) |
Zero out the parameters of a module and return it. | def zero_module(module):
"""
Zero out the parameters of a module and return it.
"""
for p in module.parameters():
p.detach().zero_()
return module |
Scale the parameters of a module and return it. | def scale_module(module, scale):
"""
Scale the parameters of a module and return it.
"""
for p in module.parameters():
p.detach().mul_(scale)
return module |
Take the mean over all non-batch dimensions. | def mean_flat(tensor):
"""
Take the mean over all non-batch dimensions.
"""
return tensor.mean(dim=list(range(1, len(tensor.shape)))) |
Take the sum over all non-batch dimensions. | def sum_flat(tensor):
"""
Take the sum over all non-batch dimensions.
"""
return tensor.sum(dim=list(range(1, len(tensor.shape)))) |
Make a standard normalization layer.
:param channels: number of input channels.
:return: an nn.Module for normalization. | def normalization(channels):
"""
Make a standard normalization layer.
:param channels: number of input channels.
:return: an nn.Module for normalization.
"""
return GroupNorm32(32, channels) |
Create sinusoidal timestep embeddings.
:param timesteps: a 1-D Tensor of N indices, one per batch element.
These may be fractional.
:param dim: the dimension of the output.
:param max_period: controls the minimum frequency of the embeddings.
:return: an [N x dim] Tensor of positional embeddings. | def timestep_embedding(timesteps, dim, max_period=10000):
"""
Create sinusoidal timestep embeddings.
:param timesteps: a 1-D Tensor of N indices, one per batch element.
These may be fractional.
:param dim: the dimension of the output.
:param max_period: controls the minimum frequency of the embeddings.
:return: an [N x dim] Tensor of positional embeddings.
"""
half = dim // 2
freqs = th.exp(
-math.log(max_period) * th.arange(start=0, end=half, dtype=th.float32) / half
).to(device=timesteps.device)
args = timesteps[:, None].float() * freqs[None]
embedding = th.cat([th.cos(args), th.sin(args)], dim=-1)
if dim % 2:
embedding = th.cat([embedding, th.zeros_like(embedding[:, :1])], dim=-1)
return embedding |
Evaluate a function without caching intermediate activations, allowing for
reduced memory at the expense of extra compute in the backward pass.
:param func: the function to evaluate.
:param inputs: the argument sequence to pass to `func`.
:param params: a sequence of parameters `func` depends on but does not
explicitly take as arguments.
:param flag: if False, disable gradient checkpointing. | def checkpoint(func, inputs, params, flag):
"""
Evaluate a function without caching intermediate activations, allowing for
reduced memory at the expense of extra compute in the backward pass.
:param func: the function to evaluate.
:param inputs: the argument sequence to pass to `func`.
:param params: a sequence of parameters `func` depends on but does not
explicitly take as arguments.
:param flag: if False, disable gradient checkpointing.
"""
if flag:
args = tuple(inputs) + tuple(params)
return CheckpointFunction.apply(func, len(inputs), *args)
else:
return func(*inputs) |
Create a ScheduleSampler from a library of pre-defined samplers.
:param name: the name of the sampler.
:param diffusion: the diffusion object to sample for. | def create_named_schedule_sampler(name, diffusion):
"""
Create a ScheduleSampler from a library of pre-defined samplers.
:param name: the name of the sampler.
:param diffusion: the diffusion object to sample for.
"""
if name == "uniform":
return UniformSampler(diffusion)
elif name == "loss-second-moment":
return LossSecondMomentResampler(diffusion)
else:
raise NotImplementedError(f"unknown schedule sampler: {name}") |
Create a list of timesteps to use from an original diffusion process,
given the number of timesteps we want to take from equally-sized portions
of the original process.
For example, if there's 300 timesteps and the section counts are [10,15,20]
then the first 100 timesteps are strided to be 10 timesteps, the second 100
are strided to be 15 timesteps, and the final 100 are strided to be 20.
If the stride is a string starting with "ddim", then the fixed striding
from the DDIM paper is used, and only one section is allowed.
:param num_timesteps: the number of diffusion steps in the original
process to divide up.
:param section_counts: either a list of numbers, or a string containing
comma-separated numbers, indicating the step count
per section. As a special case, use "ddimN" where N
is a number of steps to use the striding from the
DDIM paper.
:return: a set of diffusion steps from the original process to use. | def space_timesteps(num_timesteps, section_counts):
"""
Create a list of timesteps to use from an original diffusion process,
given the number of timesteps we want to take from equally-sized portions
of the original process.
For example, if there's 300 timesteps and the section counts are [10,15,20]
then the first 100 timesteps are strided to be 10 timesteps, the second 100
are strided to be 15 timesteps, and the final 100 are strided to be 20.
If the stride is a string starting with "ddim", then the fixed striding
from the DDIM paper is used, and only one section is allowed.
:param num_timesteps: the number of diffusion steps in the original
process to divide up.
:param section_counts: either a list of numbers, or a string containing
comma-separated numbers, indicating the step count
per section. As a special case, use "ddimN" where N
is a number of steps to use the striding from the
DDIM paper.
:return: a set of diffusion steps from the original process to use.
"""
if isinstance(section_counts, str):
if section_counts.startswith("ddim"):
desired_count = int(section_counts[len("ddim") :])
for i in range(1, num_timesteps):
if len(range(0, num_timesteps, i)) == desired_count:
return set(range(0, num_timesteps, i))
raise ValueError(
f"cannot create exactly {num_timesteps} steps with an integer stride"
)
section_counts = [int(x) for x in section_counts.split(",")]
size_per = num_timesteps // len(section_counts)
extra = num_timesteps % len(section_counts)
start_idx = 0
all_steps = []
for i, section_count in enumerate(section_counts):
size = size_per + (1 if i < extra else 0)
if size < section_count:
raise ValueError(
f"cannot divide section of {size} steps into {section_count}"
)
if section_count <= 1:
frac_stride = 1
else:
frac_stride = (size - 1) / (section_count - 1)
cur_idx = 0.0
taken_steps = []
for _ in range(section_count):
taken_steps.append(start_idx + round(cur_idx))
cur_idx += frac_stride
all_steps += taken_steps
start_idx += size
return set(all_steps) |
Take the sum over all non-batch dimensions. | def sum_flat(tensor):
"""
Take the sum over all non-batch dimensions.
"""
return tensor.sum(dim=list(range(1, len(tensor.shape)))) |
Parse filenames of the form path/to/modelNNNNNN.pt, where NNNNNN is the
checkpoint's number of steps. | def parse_resume_step_from_filename(filename):
"""
Parse filenames of the form path/to/modelNNNNNN.pt, where NNNNNN is the
checkpoint's number of steps.
"""
split = filename.split("model")
if len(split) < 2:
return 0
split1 = split[-1].split(".")[0]
try:
return int(split1)
except ValueError:
return 0 |
Log a value of some diagnostic
Call this once for each diagnostic quantity, each iteration
If called many times, last value will be used. | def logkv(key, val):
"""
Log a value of some diagnostic
Call this once for each diagnostic quantity, each iteration
If called many times, last value will be used.
"""
get_current().logkv(key, val) |
The same as logkv(), but if called many times, values averaged. | def logkv_mean(key, val):
"""
The same as logkv(), but if called many times, values averaged.
"""
get_current().logkv_mean(key, val) |
Log a dictionary of key-value pairs | def logkvs(d):
"""
Log a dictionary of key-value pairs
"""
for k, v in d.items():
logkv(k, v) |
Write all of the diagnostics from the current iteration | def dumpkvs():
"""
Write all of the diagnostics from the current iteration
"""
return get_current().dumpkvs() |
Write the sequence of args, with no separators, to the console and output files (if you've configured an output file). | def log(*args, level=INFO):
"""
Write the sequence of args, with no separators, to the console and output files (if you've configured an output file).
"""
get_current().log(*args, level=level) |
Set logging threshold on current logger. | def set_level(level):
"""
Set logging threshold on current logger.
"""
get_current().set_level(level) |
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