# -*- mode: python; coding: utf-8 -*-
# Copyright (c) 2018 Radio Astronomy Software Group
# Licensed under the 2-clause BSD License
"""Commonly used utility functions."""
from __future__ import absolute_import, division, print_function
import numpy as np
import warnings
import copy
from scipy.spatial.distance import pdist, squareform
from astropy.time import Time
from astropy.coordinates import Angle
from astropy.utils import iers
from collections.abc import Iterable
# parameters for transforming between xyz & lat/lon/alt
gps_b = 6356752.31424518
gps_a = 6378137
e_squared = 6.69437999014e-3
e_prime_squared = 6.73949674228e-3
def _str_to_bytes(s):
warnings.warn(
"_str_to_bytes is deprecated and will be removed in pyuvdata version 2.2. "
"For an input string s, this function is a thin wrapper on s.encode('utf8'). "
"The use of encode is preferred over calling this function.",
DeprecationWarning,
)
return s.encode("utf8")
def _bytes_to_str(b):
warnings.warn(
"_bytes_to_str is deprecated and will be removed in pyuvdata version 2.2. "
"For an input string s, this function is a thin wrapper on s.decode('utf8'). "
"The use of decode is preferred over calling this function.",
DeprecationWarning,
)
return b.decode("utf8")
__all__ = [
"POL_STR2NUM_DICT",
"POL_NUM2STR_DICT",
"CONJ_POL_DICT",
"JONES_STR2NUM_DICT",
"JONES_NUM2STR_DICT",
"LatLonAlt_from_XYZ",
"XYZ_from_LatLonAlt",
"rotECEF_from_ECEF",
"ECEF_from_rotECEF",
"ENU_from_ECEF",
"ECEF_from_ENU",
"phase_uvw",
"unphase_uvw",
"uvcalibrate",
"apply_uvflag",
"get_lst_for_time",
"polstr2num",
"polnum2str",
"jstr2num",
"jnum2str",
"parse_polstr",
"parse_jpolstr",
"conj_pol",
"reorder_conj_pols",
"baseline_to_antnums",
"antnums_to_baseline",
"baseline_index_flip",
"get_baseline_redundancies",
"get_antenna_redundancies",
"collapse",
"mean_collapse",
"absmean_collapse",
"quadmean_collapse",
"or_collapse",
"and_collapse",
]
# fmt: off
# polarization constants
# maps polarization strings to polarization integers
POL_STR2NUM_DICT = {'pI': 1, 'pQ': 2, 'pU': 3, 'pV': 4,
'I': 1, 'Q': 2, 'U': 3, 'V': 4, # support straight stokes names
'rr': -1, 'll': -2, 'rl': -3, 'lr': -4,
'xx': -5, 'yy': -6, 'xy': -7, 'yx': -8}
# maps polarization integers to polarization strings
POL_NUM2STR_DICT = {1: 'pI', 2: 'pQ', 3: 'pU', 4: 'pV',
-1: 'rr', -2: 'll', -3: 'rl', -4: 'lr',
-5: 'xx', -6: 'yy', -7: 'xy', -8: 'yx'}
# maps how polarizations change when antennas are swapped
CONJ_POL_DICT = {'xx': 'xx', 'yy': 'yy', 'xy': 'yx', 'yx': 'xy',
'ee': 'ee', 'nn': 'nn', 'en': 'ne', 'ne': 'en',
'rr': 'rr', 'll': 'll', 'rl': 'lr', 'lr': 'rl',
'I': 'I', 'Q': 'Q', 'U': 'U', 'V': 'V',
'pI': 'pI', 'pQ': 'pQ', 'pU': 'pU', 'pV': 'pV'}
# maps jones matrix element strings to jones integers
# Add entries that don't start with 'J' to allow shorthand versions
JONES_STR2NUM_DICT = {'Jxx': -5, 'Jyy': -6, 'Jxy': -7, 'Jyx': -8,
'xx': -5, 'x': -5, 'yy': -6, 'y': -6, 'xy': -7, 'yx': -8,
'Jrr': -1, 'Jll': -2, 'Jrl': -3, 'Jlr': -4,
'rr': -1, 'r': -1, 'll': -2, 'l': -2, 'rl': -3, 'lr': -4}
# maps jones integers to jones matrix element strings
JONES_NUM2STR_DICT = {-1: 'Jrr', -2: 'Jll', -3: 'Jrl', -4: 'Jlr',
-5: 'Jxx', -6: 'Jyy', -7: 'Jxy', -8: 'Jyx'}
# fmt: on
def _get_iterable(x):
"""Return iterable version of input."""
if isinstance(x, Iterable):
return x
else:
return (x,)
def _fits_gethduaxis(hdu, axis):
"""
Make axis arrays for fits files.
Parameters
----------
hdu : astropy.io.fits HDU object
The HDU to make an axis array for.
axis : int
The axis number of interest (1-based).
Returns
-------
ndarray of float
Array of values for the specified axis.
"""
ax = str(axis)
axis_num = hdu.header["NAXIS" + ax]
val = hdu.header["CRVAL" + ax]
delta = hdu.header["CDELT" + ax]
index = hdu.header["CRPIX" + ax] - 1
return delta * (np.arange(axis_num) - index) + val
def _fits_indexhdus(hdulist):
"""
Get a dict of table names and HDU numbers from a FITS HDU list.
Parameters
----------
hdulist : list of astropy.io.fits HDU objects
List of HDUs to get names for
Returns
-------
dict
dictionary with table names as keys and HDU number as values.
"""
tablenames = {}
for i in range(len(hdulist)):
try:
tablenames[hdulist[i].header["EXTNAME"]] = i
except (KeyError):
continue
return tablenames
def _check_history_version(history, version_string):
"""Check if version_string is present in history string."""
if version_string.replace(" ", "") in history.replace("\n", "").replace(" ", ""):
return True
else:
return False
def _check_histories(history1, history2):
"""Check if two histories are the same."""
if history1.replace("\n", "").replace(" ", "") == history2.replace(
"\n", ""
).replace(" ", ""):
return True
else:
return False
def _combine_histories(history1, history2):
"""Combine histories with minimal repeats."""
hist2_words = history2.split(" ")
add_hist = ""
test_hist1 = " " + history1 + " "
for i, word in enumerate(hist2_words):
if " " + word + " " not in test_hist1:
add_hist += " " + word
keep_going = i + 1 < len(hist2_words)
while keep_going:
if (hist2_words[i + 1] == " ") or (
" " + hist2_words[i + 1] + " " not in test_hist1
):
add_hist += " " + hist2_words[i + 1]
del hist2_words[i + 1]
keep_going = i + 1 < len(hist2_words)
else:
keep_going = False
return history1 + add_hist
[docs]def baseline_to_antnums(baseline, Nants_telescope):
"""
Get the antenna numbers corresponding to a given baseline number.
Parameters
----------
baseline : int or array_like of ints
baseline number
Nants_telescope : int
number of antennas
Returns
-------
int or array_like of int
first antenna number(s)
int or array_like of int
second antenna number(s)
"""
if Nants_telescope > 2048:
raise Exception(
"error Nants={Nants}>2048 not " "supported".format(Nants=Nants_telescope)
)
baseline = np.asarray(baseline, dtype=np.int64)
if np.min(baseline) > 2 ** 16:
ant2 = (baseline - 2 ** 16) % 2048 - 1
ant1 = (baseline - 2 ** 16 - (ant2 + 1)) / 2048 - 1
else:
ant2 = (baseline) % 256 - 1
ant1 = (baseline - (ant2 + 1)) / 256 - 1
return np.int32(ant1), np.int32(ant2)
[docs]def antnums_to_baseline(ant1, ant2, Nants_telescope, attempt256=False):
"""
Get the baseline number corresponding to two given antenna numbers.
Parameters
----------
ant1 : int or array_like of int
first antenna number
ant2 : int or array_like of int
second antenna number
Nants_telescope : int
number of antennas
attempt256 : bool
Option to try to use the older 256 standard used in
many uvfits files (will use 2048 standard if there are more
than 256 antennas). Default is False.
Returns
-------
int or array of int
baseline number corresponding to the two antenna numbers.
"""
ant1, ant2 = np.int64((ant1, ant2))
if Nants_telescope is not None and Nants_telescope > 2048:
raise Exception(
"cannot convert ant1, ant2 to a baseline index "
"with Nants={Nants}>2048.".format(Nants=Nants_telescope)
)
if attempt256:
if np.max(ant1) < 255 and np.max(ant2) < 255:
return 256 * (ant1 + 1) + (ant2 + 1)
else:
print("Max antnums are {} and {}".format(np.max(ant1), np.max(ant2)))
message = (
"antnums_to_baseline: found > 256 antennas, using "
"2048 baseline indexing. Beware compatibility "
"with CASA etc"
)
warnings.warn(message)
baseline = 2048 * (ant1 + 1) + (ant2 + 1) + 2 ** 16
if isinstance(baseline, np.ndarray):
return np.asarray(baseline, dtype=np.int64)
else:
return np.int64(baseline)
[docs]def baseline_index_flip(baseline, Nants_telescope):
"""Change baseline number to reverse antenna order."""
ant1, ant2 = baseline_to_antnums(baseline, Nants_telescope)
return antnums_to_baseline(ant2, ant1, Nants_telescope)
def _x_orientation_rep_dict(x_orientation):
"""Create replacement dict based on x_orientation."""
if x_orientation.lower() == "east" or x_orientation.lower() == "e":
return {"x": "e", "y": "n"}
elif x_orientation.lower() == "north" or x_orientation.lower() == "n":
return {"x": "n", "y": "e"}
else:
raise ValueError("x_orientation not recognized.")
[docs]def polstr2num(pol, x_orientation=None):
"""
Convert polarization str to number according to AIPS Memo 117.
Prefer 'pI', 'pQ', 'pU' and 'pV' to make it clear that these are pseudo-Stokes,
not true Stokes, but also supports 'I', 'Q', 'U', 'V'.
Parameters
----------
pol : str
polarization string
x_orientation : str, optional
Orientation of the physical dipole corresponding to what is
labelled as the x polarization ("east" or "north") to allow for
converting from E/N strings. See corresonding parameter on UVData
for more details.
Returns
-------
int
Number corresponding to string
Raises
------
ValueError
If the pol string cannot be converted to a polarization number.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
dict_use = copy.deepcopy(POL_STR2NUM_DICT)
if x_orientation is not None:
try:
rep_dict = _x_orientation_rep_dict(x_orientation)
for key, value in POL_STR2NUM_DICT.items():
new_key = key.replace("x", rep_dict["x"]).replace("y", rep_dict["y"])
dict_use[new_key] = value
except ValueError:
warnings.warn("x_orientation not recognized.")
poldict = {k.lower(): v for k, v in dict_use.items()}
if isinstance(pol, str):
out = poldict[pol.lower()]
elif isinstance(pol, Iterable):
out = [poldict[key.lower()] for key in pol]
else:
raise ValueError(
"Polarization {p} cannot be converted to a polarization number.".format(
p=pol
)
)
return out
[docs]def polnum2str(num, x_orientation=None):
"""
Convert polarization number to str according to AIPS Memo 117.
Uses 'pI', 'pQ', 'pU' and 'pV' to make it clear that these are pseudo-Stokes,
not true Stokes
Parameters
----------
num : int
polarization number
x_orientation : str, optional
Orientation of the physical dipole corresponding to what is
labelled as the x polarization ("east" or "north") to convert to
E/N strings. See corresonding parameter on UVData for more details.
Returns
-------
str
String corresponding to polarization number
Raises
------
ValueError
If the polarization number cannot be converted to a polarization string.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
dict_use = copy.deepcopy(POL_NUM2STR_DICT)
if x_orientation is not None:
try:
rep_dict = _x_orientation_rep_dict(x_orientation)
for key, value in POL_NUM2STR_DICT.items():
new_val = value.replace("x", rep_dict["x"]).replace("y", rep_dict["y"])
dict_use[key] = new_val
except ValueError:
warnings.warn("x_orientation not recognized.")
if isinstance(num, (int, np.int32, np.int64)):
out = dict_use[num]
elif isinstance(num, Iterable):
out = [dict_use[i] for i in num]
else:
raise ValueError(
"Polarization {p} cannot be converted to string.".format(p=num)
)
return out
[docs]def jstr2num(jstr, x_orientation=None):
"""
Convert jones polarization str to number according to calfits memo.
Parameters
----------
jstr : str
antenna (jones) polarization string
x_orientation : str, optional
Orientation of the physical dipole corresponding to what is
labelled as the x polarization ("east" or "north") to allow for
converting from E/N strings. See corresonding parameter on UVData
for more details.
Returns
-------
int
antenna (jones) polarization number corresponding to string
Raises
------
ValueError
If the jones string cannot be converted to a polarization number.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
dict_use = copy.deepcopy(JONES_STR2NUM_DICT)
if x_orientation is not None:
try:
rep_dict = _x_orientation_rep_dict(x_orientation)
for key, value in JONES_STR2NUM_DICT.items():
new_key = key.replace("x", rep_dict["x"]).replace("y", rep_dict["y"])
dict_use[new_key] = value
except ValueError:
warnings.warn("x_orientation not recognized.")
jdict = {k.lower(): v for k, v in dict_use.items()}
if isinstance(jstr, str):
out = jdict[jstr.lower()]
elif isinstance(jstr, Iterable):
out = [jdict[key.lower()] for key in jstr]
else:
raise ValueError(
"Jones polarization {j} cannot be converted to index.".format(j=jstr)
)
return out
[docs]def jnum2str(jnum, x_orientation=None):
"""
Convert jones polarization number to str according to calfits memo.
Parameters
----------
num : int
antenna (jones) polarization number
x_orientation : str, optional
Orientation of the physical dipole corresponding to what is
labelled as the x polarization ("east" or "north") to convert to
E/N strings. See corresonding parameter on UVData for more details.
Returns
-------
str
antenna (jones) polarization string corresponding to number
Raises
------
ValueError
If the jones polarization number cannot be converted to a jones
polarization string.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
dict_use = copy.deepcopy(JONES_NUM2STR_DICT)
if x_orientation is not None:
try:
rep_dict = _x_orientation_rep_dict(x_orientation)
for key, value in JONES_NUM2STR_DICT.items():
new_val = value.replace("x", rep_dict["x"]).replace("y", rep_dict["y"])
dict_use[key] = new_val
except ValueError:
warnings.warn("x_orientation not recognized.")
if isinstance(jnum, (int, np.int32, np.int64)):
out = dict_use[jnum]
elif isinstance(jnum, Iterable):
out = [dict_use[i] for i in jnum]
else:
raise ValueError(
"Jones polarization {j} cannot be converted to string.".format(j=jnum)
)
return out
[docs]def parse_polstr(polstr, x_orientation=None):
"""
Parse a polarization string and return pyuvdata standard polarization string.
See utils.POL_STR2NUM_DICT for options.
Parameters
----------
polstr : str
polarization string
x_orientation : str, optional
Orientation of the physical dipole corresponding to what is
labelled as the x polarization ("east" or "north") to allow for
converting from E/N strings. See corresonding parameter on UVData
for more details.
Returns
-------
str
AIPS Memo 117 standard string
Raises
------
ValueError
If the pol string cannot be converted to a polarization number.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
return polnum2str(
polstr2num(polstr, x_orientation=x_orientation), x_orientation=x_orientation
)
[docs]def parse_jpolstr(jpolstr, x_orientation=None):
"""
Parse a Jones polarization string and return pyuvdata standard jones string.
See utils.JONES_STR2NUM_DICT for options.
Parameters
----------
jpolstr : str
Jones polarization string
Returns
-------
str
calfits memo standard string
Raises
------
ValueError
If the jones string cannot be converted to a polarization number.
Warns
-----
UserWarning
If the x_orientation not recognized.
"""
return jnum2str(
jstr2num(jpolstr, x_orientation=x_orientation), x_orientation=x_orientation
)
[docs]def conj_pol(pol):
"""
Return the polarization for the conjugate baseline.
For example, (1, 2, 'xy') = conj(2, 1, 'yx').
The returned polarization is determined by assuming the antenna pair is
reversed in the data, and finding the correct polarization correlation
which will yield the requested baseline when conjugated. Note this means
changing the polarization for linear cross-pols, but keeping auto-pol
(e.g. xx) and Stokes the same.
Parameters
----------
pol : str or int
Polarization string or integer.
Returns
-------
cpol : str or int
Polarization as if antennas are swapped (type matches input)
"""
cpol_dict = {k.lower(): v for k, v in CONJ_POL_DICT.items()}
if isinstance(pol, str):
cpol = cpol_dict[pol.lower()]
elif isinstance(pol, Iterable):
cpol = [conj_pol(p) for p in pol]
elif isinstance(pol, (int, np.int32, np.int64)):
cpol = polstr2num(cpol_dict[polnum2str(pol).lower()])
else:
raise ValueError("Polarization not recognized, cannot be conjugated.")
return cpol
[docs]def reorder_conj_pols(pols):
"""
Reorder multiple pols, swapping pols that are conjugates of one another.
For example ('xx', 'xy', 'yx', 'yy') -> ('xx', 'yx', 'xy', 'yy')
This is useful for the _key2inds function in the case where an antenna
pair is specified but the conjugate pair exists in the data. The conjugated
data should be returned in the order of the polarization axis, so after
conjugating the data, the pols need to be reordered.
For example, if a file contains antpair (0, 1) and pols 'xy' and 'yx', but
the user requests antpair (1, 0), they should get:
[(1x, 0y), (1y, 0x)] = [conj(0y, 1x), conj(0x, 1y)]
Parameters
----------
pols : array_like of str or int
Polarization array (strings or ints).
Returns
-------
conj_order : ndarray of int
Indices to reorder polarization array.
"""
if not isinstance(pols, Iterable):
raise ValueError("reorder_conj_pols must be given an array of polarizations.")
cpols = np.array([conj_pol(p) for p in pols]) # Array needed for np.where
conj_order = [np.where(cpols == p)[0][0] if p in cpols else -1 for p in pols]
if -1 in conj_order:
raise ValueError(
"Not all conjugate pols exist in the polarization array provided."
)
return conj_order
[docs]def LatLonAlt_from_XYZ(xyz, check_acceptability=True):
"""
Calculate lat/lon/alt from ECEF x,y,z.
Parameters
----------
xyz : ndarray of float
numpy array, shape (Npts, 3), with ECEF x,y,z coordinates.
check_acceptability : bool
Flag to check XYZ coordinates are reasonable.
Returns
-------
latitude : ndarray or float
latitude, numpy array (if Npts > 1) or value (if Npts = 1) in radians
longitude : ndarray or float
longitude, numpy array (if Npts > 1) or value (if Npts = 1) in radians
altitude : ndarray or float
altitude, numpy array (if Npts > 1) or value (if Npts = 1) in meters
"""
# convert to a numpy array
xyz = np.array(xyz)
if xyz.ndim > 1 and xyz.shape[1] != 3:
raise ValueError("The expected shape of ECEF xyz array is (Npts, 3).")
else:
xyz_use = xyz
if xyz_use.ndim == 1:
xyz_use = xyz_use[np.newaxis, :]
# checking for acceptable values
if check_acceptability:
if np.any(np.linalg.norm(xyz_use, axis=1) < 6.35e6) or np.any(
np.linalg.norm(xyz_use, axis=1) > 6.39e6
):
raise ValueError("xyz values should be ECEF x, y, z coordinates in meters")
# see wikipedia geodetic_datum and Datum transformations of
# GPS positions PDF in docs/references folder
gps_p = np.sqrt(xyz_use[:, 0] ** 2 + xyz_use[:, 1] ** 2)
gps_theta = np.arctan2(xyz_use[:, 2] * gps_a, gps_p * gps_b)
latitude = np.arctan2(
xyz_use[:, 2] + e_prime_squared * gps_b * np.sin(gps_theta) ** 3,
gps_p - e_squared * gps_a * np.cos(gps_theta) ** 3,
)
longitude = np.arctan2(xyz_use[:, 1], xyz_use[:, 0])
gps_n = gps_a / np.sqrt(1 - e_squared * np.sin(latitude) ** 2)
altitude = (gps_p / np.cos(latitude)) - gps_n
if xyz.ndim == 1:
longitude = longitude[0]
latitude = latitude[0]
altitude = altitude[0]
return latitude, longitude, altitude
[docs]def XYZ_from_LatLonAlt(latitude, longitude, altitude):
"""
Calculate ECEF x,y,z from lat/lon/alt values.
Parameters
----------
latitude : ndarray or float
latitude, numpy array (if Npts > 1) or value (if Npts = 1) in radians
longitude : ndarray or float
longitude, numpy array (if Npts > 1) or value (if Npts = 1) in radians
altitude : ndarray or float
altitude, numpy array (if Npts > 1) or value (if Npts = 1) in meters
Returns
-------
xyz : ndarray of float
numpy array, shape (Npts, 3), with ECEF x,y,z coordinates.
"""
latitude = np.array(latitude)
longitude = np.array(longitude)
altitude = np.array(altitude)
n_pts = latitude.size
if longitude.size != n_pts:
raise ValueError(
"latitude, longitude and altitude must all have the same length"
)
if altitude.size != n_pts:
raise ValueError(
"latitude, longitude and altitude must all have the same length"
)
# see wikipedia geodetic_datum and Datum transformations of
# GPS positions PDF in docs/references folder
gps_n = gps_a / np.sqrt(1 - e_squared * np.sin(latitude) ** 2)
xyz = np.zeros((n_pts, 3))
xyz[:, 0] = (gps_n + altitude) * np.cos(latitude) * np.cos(longitude)
xyz[:, 1] = (gps_n + altitude) * np.cos(latitude) * np.sin(longitude)
xyz[:, 2] = (gps_b ** 2 / gps_a ** 2 * gps_n + altitude) * np.sin(latitude)
xyz = np.squeeze(xyz)
return xyz
[docs]def rotECEF_from_ECEF(xyz, longitude):
"""
Get rotated ECEF positions such that the x-axis goes through the longitude.
Miriad and uvfits expect antenna positions in this frame
(with longitude of the array center/telescope location)
Parameters
----------
xyz : ndarray of float
numpy array, shape (Npts, 3), with ECEF x,y,z coordinates.
longitude : float
longitude in radians to rotate coordinates to
(usually the array center/telescope location).
Returns
-------
ndarray of float
Rotated ECEF coordinates, shape (Npts, 3).
"""
angle = -1 * longitude
rot_matrix = np.array(
[
[np.cos(angle), -1 * np.sin(angle), 0],
[np.sin(angle), np.cos(angle), 0],
[0, 0, 1],
]
)
return rot_matrix.dot(xyz.T).T
[docs]def ECEF_from_rotECEF(xyz, longitude):
"""
Calculate ECEF from a rotated ECEF (Inverse of rotECEF_from_ECEF).
Parameters
----------
xyz : ndarray of float
numpy array, shape (Npts, 3), with rotated ECEF x,y,z coordinates.
longitude : float
longitude in radians giving the x direction of the rotated coordinates
(usually the array center/telescope location).
Returns
-------
ndarray of float
ECEF coordinates, shape (Npts, 3).
"""
angle = longitude
rot_matrix = np.array(
[
[np.cos(angle), -1 * np.sin(angle), 0],
[np.sin(angle), np.cos(angle), 0],
[0, 0, 1],
]
)
return rot_matrix.dot(xyz.T).T
[docs]def ENU_from_ECEF(xyz, latitude, longitude, altitude):
"""
Calculate local ENU (east, north, up) coordinates from ECEF coordinates.
Parameters
----------
xyz : ndarray of float
numpy array, shape (Npts, 3), with ECEF x,y,z coordinates.
latitude : float
Latitude of center of ENU coordinates in radians.
longitude : float
Longitude of center of ENU coordinates in radians.
altitude : float
Altitude of center of ENU coordinates in radians.
Returns
-------
ndarray of float
numpy array, shape (Npts, 3), with local ENU coordinates
"""
xyz = np.array(xyz)
if xyz.ndim > 1 and xyz.shape[1] != 3:
raise ValueError("The expected shape of ECEF xyz array is (Npts, 3).")
xyz_in = xyz
if xyz_in.ndim == 1:
xyz_in = xyz_in[np.newaxis, :]
# check that these are sensible ECEF values -- their magnitudes need to be
# on the order of Earth's radius
ecef_magnitudes = np.linalg.norm(xyz_in, axis=1)
sensible_radius_range = (6.35e6, 6.39e6)
if np.any(ecef_magnitudes <= sensible_radius_range[0]) or np.any(
ecef_magnitudes >= sensible_radius_range[1]
):
raise ValueError(
"ECEF vector magnitudes must be on the order of the radius of the earth"
)
xyz_center = XYZ_from_LatLonAlt(latitude, longitude, altitude)
xyz_use = np.zeros_like(xyz_in)
xyz_use[:, 0] = xyz_in[:, 0] - xyz_center[0]
xyz_use[:, 1] = xyz_in[:, 1] - xyz_center[1]
xyz_use[:, 2] = xyz_in[:, 2] - xyz_center[2]
enu = np.zeros_like(xyz_use)
enu[:, 0] = -np.sin(longitude) * xyz_use[:, 0] + np.cos(longitude) * xyz_use[:, 1]
enu[:, 1] = (
-np.sin(latitude) * np.cos(longitude) * xyz_use[:, 0]
- np.sin(latitude) * np.sin(longitude) * xyz_use[:, 1]
+ np.cos(latitude) * xyz_use[:, 2]
)
enu[:, 2] = (
np.cos(latitude) * np.cos(longitude) * xyz_use[:, 0]
+ np.cos(latitude) * np.sin(longitude) * xyz_use[:, 1]
+ np.sin(latitude) * xyz_use[:, 2]
)
if len(xyz.shape) == 1:
enu = np.squeeze(enu)
return enu
[docs]def ECEF_from_ENU(enu, latitude, longitude, altitude):
"""
Calculate ECEF coordinates from local ENU (east, north, up) coordinates.
Parameters
----------
enu : ndarray of float
numpy array, shape (Npts, 3), with local ENU coordinates.
latitude : float
Latitude of center of ENU coordinates in radians.
longitude : float
Longitude of center of ENU coordinates in radians.
altitude : float
Altitude of center of ENU coordinates in radians.
Returns
-------
xyz : ndarray of float
numpy array, shape (Npts, 3), with ECEF x,y,z coordinates.
"""
enu = np.array(enu)
if enu.ndim > 1 and enu.shape[1] != 3:
raise ValueError("The expected shape of the ENU array is (Npts, 3).")
enu_use = enu
if enu_use.ndim == 1:
enu_use = enu_use[np.newaxis, :]
xyz = np.zeros_like(enu_use)
xyz[:, 0] = (
-np.sin(latitude) * np.cos(longitude) * enu_use[:, 1]
- np.sin(longitude) * enu_use[:, 0]
+ np.cos(latitude) * np.cos(longitude) * enu_use[:, 2]
)
xyz[:, 1] = (
-np.sin(latitude) * np.sin(longitude) * enu_use[:, 1]
+ np.cos(longitude) * enu_use[:, 0]
+ np.cos(latitude) * np.sin(longitude) * enu_use[:, 2]
)
xyz[:, 2] = np.cos(latitude) * enu_use[:, 1] + np.sin(latitude) * enu_use[:, 2]
xyz_center = XYZ_from_LatLonAlt(latitude, longitude, altitude)
xyz[:, 0] = xyz[:, 0] + xyz_center[0]
xyz[:, 1] = xyz[:, 1] + xyz_center[1]
xyz[:, 2] = xyz[:, 2] + xyz_center[2]
if len(enu.shape) == 1:
xyz = np.squeeze(xyz)
return xyz
[docs]def phase_uvw(ra, dec, initial_uvw):
"""
Calculate phased uvws/positions from unphased ones in an icrs or gcrs frame.
This code expects input uvws or positions relative to the telescope
location in the same frame that ra/dec are in (e.g. icrs or gcrs) and
returns phased ones in the same frame.
Note that this code is nearly identical to ENU_from_ECEF, except that it
uses an arbitrary phasing center rather than a coordinate center.
Parameters
----------
ra : float
Right ascension of phase center.
dec : float
Declination of phase center.
initial_uvw : ndarray of float
Unphased uvws or positions relative to the array center,
shape (Nlocs, 3).
Returns
-------
uvw : ndarray of float
uvw array in the same frame as initial_uvws, ra and dec.
"""
if initial_uvw.ndim == 1:
initial_uvw = initial_uvw[np.newaxis, :]
uvw = np.zeros_like(initial_uvw)
uvw[:, 0] = -np.sin(ra) * initial_uvw[:, 0] + np.cos(ra) * initial_uvw[:, 1]
uvw[:, 1] = (
-np.sin(dec) * np.cos(ra) * initial_uvw[:, 0]
- np.sin(dec) * np.sin(ra) * initial_uvw[:, 1]
+ np.cos(dec) * initial_uvw[:, 2]
)
uvw[:, 2] = (
np.cos(dec) * np.cos(ra) * initial_uvw[:, 0]
+ np.cos(dec) * np.sin(ra) * initial_uvw[:, 1]
+ np.sin(dec) * initial_uvw[:, 2]
)
return uvw
[docs]def unphase_uvw(ra, dec, uvw):
"""
Calculate unphased uvws/positions from phased ones in an icrs or gcrs frame.
This code expects phased uvws or positions in the same frame that ra/dec
are in (e.g. icrs or gcrs) and returns unphased ones in the same frame.
Parameters
----------
ra : float
Right ascension of phase center.
dec : float
Declination of phase center.
uvw : ndarray of float
Phased uvws or positions relative to the array center,
shape (Nlocs, 3).
Returns
-------
unphased_uvws : ndarray of float
Unphased uvws or positions relative to the array center,
shape (Nlocs, 3).
"""
if uvw.ndim == 1:
uvw = uvw[np.newaxis, :]
unphased_uvws = np.zeros_like(uvw)
unphased_uvws[:, 0] = (
-np.sin(ra) * uvw[:, 0]
- np.sin(dec) * np.cos(ra) * uvw[:, 1]
+ np.cos(dec) * np.cos(ra) * uvw[:, 2]
)
unphased_uvws[:, 1] = (
np.cos(ra) * uvw[:, 0]
- np.sin(dec) * np.sin(ra) * uvw[:, 1]
+ np.cos(dec) * np.sin(ra) * uvw[:, 2]
)
unphased_uvws[:, 2] = np.cos(dec) * uvw[:, 1] + np.sin(dec) * uvw[:, 2]
return unphased_uvws
[docs]def get_lst_for_time(jd_array, latitude, longitude, altitude):
"""
Get the lsts for a set of jd times at an earth location.
Parameters
----------
jd_array : ndarray of float
JD times to get lsts for.
latitude : float
Latitude of location to get lst for in degrees.
longitude : float
Longitude of location to get lst for in degrees.
altitude : float
Altitude of location to get lst for in meters.
Returns
-------
ndarray of float
LSTs in radians corresponding to the jd_array.
"""
lst_array = np.zeros_like(jd_array)
for ind, jd in enumerate(np.unique(jd_array)):
t = Time(
jd,
format="jd",
location=(Angle(longitude, unit="deg"), Angle(latitude, unit="deg")),
)
# avoid errors if iers.conf.auto_max_age is set to None, as we do in
# testing if the iers url is down
if iers.conf.auto_max_age is None: # pragma: no cover
delta, status = t.get_delta_ut1_utc(return_status=True)
if status in (iers.TIME_BEFORE_IERS_RANGE, iers.TIME_BEYOND_IERS_RANGE):
warnings.warn(
"time is out of IERS range, setting delta ut1 utc to "
"extrapolated value"
)
t.delta_ut1_utc = delta
lst_array[
np.where(np.isclose(jd, jd_array, atol=1e-6, rtol=1e-12))
] = t.sidereal_time("apparent").radian
return lst_array
[docs]def get_baseline_redundancies(baselines, baseline_vecs, tol=1.0, with_conjugates=False):
"""
Find redundant baseline groups.
Parameters
----------
baselines : array_like of int
Baseline numbers, shape (Nbls,)
baseline_vecs : array_like of float
Baseline vectors in meters, shape shape (Nbls, 3)
tol : float
Absolute tolerance of redundancy, in meters.
with_conjugates : bool
Option to include baselines that are redundant when flipped.
Returns
-------
baseline_groups : list of lists of int
list of lists of redundant baseline numbers
vec_bin_centers : list of array_like of float
List of vectors describing redundant group centers
lengths : list of float
List of redundant group baseline lengths in meters
baseline_ind_conj : list of int
List of baselines that are redundant when reversed. Only returned if
with_conjugates is True
"""
Nbls = baselines.shape[0]
if not baseline_vecs.shape == (Nbls, 3):
raise ValueError("Baseline vectors must be shape (Nbls, 3)")
baseline_vecs = copy.copy(baseline_vecs) # Protect the vectors passed in.
if with_conjugates:
conjugates = []
for bv in baseline_vecs:
uneg = bv[0] < -tol
uzer = np.isclose(bv[0], 0.0, atol=tol)
vneg = bv[1] < -tol
vzer = np.isclose(bv[1], 0.0, atol=tol)
wneg = bv[2] < -tol
conjugates.append(uneg or (uzer and vneg) or (uzer and vzer and wneg))
conjugates = np.array(conjugates, dtype=bool)
baseline_vecs[conjugates] *= -1
baseline_ind_conj = baselines[conjugates]
bl_gps, vec_bin_centers, lens = get_baseline_redundancies(
baselines, baseline_vecs, tol=tol, with_conjugates=False
)
return bl_gps, vec_bin_centers, lens, baseline_ind_conj
# For each baseline, list all others that are within the tolerance distance.
adj_triu_mat = pdist(baseline_vecs) < tol
adj = {} # Adjacency dictionary
for bi, col in enumerate(squareform(adj_triu_mat)):
col[bi] = True
adj[baselines[bi]] = baselines[col]
# The adjacency list defines a set of graph edges.
# For each baseline b0, loop over its adjacency list ai \in adj[b0]
# If adj[b0] is a subset of adj[ai], then ai is in a redundant group with b0
bl_gps = []
for k in adj.keys():
a0 = adj[k]
group = [k]
for a in a0:
if set(a0).issubset(adj[a]) and a not in group:
group.append(a)
group.sort()
bl_gps.append(group)
# Groups can be different lengths, but we need to take a unique over an axis
# to properly identify unique groups
# Pad out all the sub-lists to be the same length
pad = len(max(bl_gps, key=len))
bl_gps = np.array([i + [-1] * (pad - len(i)) for i in bl_gps])
# We end up with multiple copies of each redundant group, so remove duplicates
bl_gps = np.unique(bl_gps, axis=0).tolist()
# remove the dummy pad baselines from each list
bl_gps = [[bl for bl in gp if bl != -1] for gp in bl_gps]
n_unique = len(bl_gps)
vec_bin_centers = np.zeros((n_unique, 3))
for gi, gp in enumerate(bl_gps):
inds = [np.where(i == baselines)[0] for i in gp]
vec_bin_centers[gi] = np.mean(baseline_vecs[inds, :], axis=0)
lens = np.sqrt(np.sum(vec_bin_centers ** 2, axis=1))
if np.sum([len(bg) for bg in bl_gps]) > Nbls:
raise ValueError(
"Some baselines are falling into multiple"
" redundant groups. Lower the tolerance to resolve ambiguity."
)
return bl_gps, vec_bin_centers, lens
[docs]def get_antenna_redundancies(
antenna_numbers, antenna_positions, tol=1.0, include_autos=False
):
"""
Find redundant baseline groups based on antenna positions.
Parameters
----------
antenna_numbers : array_like of int
Antenna numbers, shape (Nants,).
antenna_positions : array_like of float
Antenna position vectors in the ENU (topocentric) frame in meters,
shape (Nants, 3).
tol : float
Redundancy tolerance in meters.
include_autos : bool
Option to include autocorrelations.
Returns
-------
baseline_groups : list of lists of int
list of lists of redundant baseline numbers
vec_bin_centers : list of array_like of float
List of vectors describing redundant group centers
lengths : list of float
List of redundant group baseline lengths in meters
Notes
-----
The baseline numbers refer to antenna pairs (a1, a2) such that
the baseline vector formed from ENU antenna positions,
blvec = enu[a1] - enu[a2]
is close to the other baselines in the group.
This is achieved by putting baselines in a form of the u>0
convention, but with a tolerance in defining the signs of
vector components.
To guarantee that the same baseline numbers are present in a UVData
object, ``UVData.conjugate_bls('u>0', uvw_tol=tol)``, where `tol` is
the tolerance used here.
"""
Nants = antenna_numbers.size
bls = []
bl_vecs = []
for aj in range(Nants):
mini = aj + 1
if include_autos:
mini = aj
for ai in range(mini, Nants):
anti, antj = antenna_numbers[ai], antenna_numbers[aj]
bidx = antnums_to_baseline(antj, anti, Nants)
bv = antenna_positions[ai] - antenna_positions[aj]
bl_vecs.append(bv)
bls.append(bidx)
bls = np.array(bls)
bl_vecs = np.array(bl_vecs)
gps, vecs, lens, conjs = get_baseline_redundancies(
bls, bl_vecs, tol=tol, with_conjugates=True
)
# Flip the baselines in the groups.
for gi, gp in enumerate(gps):
for bi, bl in enumerate(gp):
if bl in conjs:
gps[gi][bi] = baseline_index_flip(bl, Nants)
return gps, vecs, lens
[docs]def mean_collapse(
arr, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Collapse by averaging data.
This is similar to np.average, except it handles infs (by giving them
zero weight) and zero weight axes (by forcing result to be inf with zero
output weight).
Parameters
----------
arr : array
Input array to process.
weights: ndarray, optional
weights for average. If none, will default to equal weight for all
non-infinite data.
axis : int or tuple, optional
Axis or axes to collapse (passed to np.sum). Default is all.
return_weights : bool
Whether to return sum of weights.
return_weights_square: bool
Whether to return the sum of the square of the weights. Default is False.
"""
arr = copy.deepcopy(arr) # avoid changing outside
if weights is None:
weights = np.ones_like(arr)
else:
weights = copy.deepcopy(weights)
weights = weights * np.logical_not(np.isinf(arr))
arr[np.isinf(arr)] = 0
weight_out = np.sum(weights, axis=axis)
if return_weights_square:
weights_square = weights ** 2
weights_square_out = np.sum(weights_square, axis=axis)
out = np.sum(weights * arr, axis=axis)
where = weight_out > 1e-10
out = np.true_divide(out, weight_out, where=where)
out = np.where(where, out, np.inf)
if return_weights and return_weights_square:
return out, weight_out, weights_square_out
elif return_weights:
return out, weight_out
elif return_weights_square:
return out, weights_square_out
else:
return out
[docs]def absmean_collapse(
arr, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Collapse by averaging absolute value of data.
Parameters
----------
arr : array
Input array to process.
weights: ndarray, optional
weights for average. If none, will default to equal weight for all
non-infinite data.
axis : int or tuple, optional
Axis or axes to collapse (passed to np.sum). Default is all.
return_weights : bool
Whether to return sum of weights.
return_weights_square: bool
whether to return the sum of the squares of the weights. Default is False.
"""
return mean_collapse(
np.abs(arr),
weights=weights,
axis=axis,
return_weights=return_weights,
return_weights_square=return_weights_square,
)
[docs]def quadmean_collapse(
arr, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Collapse by averaging in quadrature.
Parameters
----------
arr : array
Input array to process.
weights: ndarray, optional
weights for average. If none, will default to equal weight for all
non-infinite data.
axis : int or tuple, optional
Axis or axes to collapse (passed to np.sum). Default is all.
return_weights : bool
Whether to return sum of weights.
return_weights_square: bool
whether to return the sum of the squares of the weights. Default is False.
"""
out = mean_collapse(
np.abs(arr) ** 2,
weights=weights,
axis=axis,
return_weights=return_weights,
return_weights_square=return_weights_square,
)
if return_weights and return_weights_square:
return np.sqrt(out[0]), out[1], out[2]
elif return_weights or return_weights_square:
return np.sqrt(out[0]), out[1]
else:
return np.sqrt(out)
[docs]def or_collapse(
arr, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Collapse using OR operation.
Parameters
----------
arr : array
Input array to process.
weights: ndarray, optional
NOT USED, but kept for symmetry with other collapsing functions.
axis : int or tuple, optional
Axis or axes to collapse (take OR over). Default is all.
return_weights : bool
Whether to return dummy weights array.
NOTE: the dummy weights will simply be an array of ones
return_weights_square: bool
NOT USED, but kept for symmetry with other collapsing functions.
"""
if arr.dtype != np.bool:
raise ValueError("Input to or_collapse function must be boolean array")
out = np.any(arr, axis=axis)
if (weights is not None) and not np.all(weights == weights.reshape(-1)[0]):
warnings.warn("Currently weights are not handled when OR-ing boolean arrays.")
if return_weights:
return out, np.ones_like(out, dtype=np.float)
else:
return out
[docs]def and_collapse(
arr, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Collapse using AND operation.
Parameters
----------
arr : array
Input array to process.
weights: ndarray, optional
NOT USED, but kept for symmetry with other collapsing functions.
axis : int or tuple, optional
Axis or axes to collapse (take AND over). Default is all.
return_weights : bool
Whether to return dummy weights array.
NOTE: the dummy weights will simply be an array of ones
return_weights_square: bool
NOT USED, but kept for symmetry with other collapsing functions.
"""
if arr.dtype != np.bool:
raise ValueError("Input to and_collapse function must be boolean array")
out = np.all(arr, axis=axis)
if (weights is not None) and not np.all(weights == weights.reshape(-1)[0]):
warnings.warn("Currently weights are not handled when AND-ing boolean arrays.")
if return_weights:
return out, np.ones_like(out, dtype=np.float)
else:
return out
[docs]def collapse(
arr, alg, weights=None, axis=None, return_weights=False, return_weights_square=False
):
"""
Parent function to collapse an array with a given algorithm.
Parameters
----------
arr : array
Input array to process.
alg : str
Algorithm to use. Must be defined in this function with
corresponding subfunction above.
weights: ndarray, optional
weights for collapse operation (e.g. weighted mean).
NOTE: Some subfunctions do not use the weights. See corresponding
doc strings.
axis : int or tuple, optional
Axis or axes to collapse. Default is all.
return_weights : bool
Whether to return sum of weights.
return_weights_square: bool
Whether to return the sum of the squares of the weights. Default is False.
"""
collapse_dict = {
"mean": mean_collapse,
"absmean": absmean_collapse,
"quadmean": quadmean_collapse,
"or": or_collapse,
"and": and_collapse,
}
try:
out = collapse_dict[alg](
arr,
weights=weights,
axis=axis,
return_weights=return_weights,
return_weights_square=return_weights_square,
)
except KeyError:
raise ValueError(
"Collapse algorithm must be one of: "
+ ", ".join(collapse_dict.keys())
+ "."
)
return out
[docs]def uvcalibrate(
uvdata,
uvcal,
inplace=True,
prop_flags=True,
flag_missing=True,
Dterm_cal=False,
delay_convention="minus",
undo=False,
):
"""
Calibrate a UVData object with a UVCal object.
Parameters
----------
uvdata : UVData object
UVData object to calibrate.
uvcal : UVCal object
UVCal object containing the calibration.
inplace : bool, optional
if True edit uvdata in place, else deepcopy
prop_flags : bool, optional
if True, propagate calibration flags to data flags
and doesn't use flagged gains. Otherwise, uses flagged gains and
does not propagate calibration flags to data flags.
flag_missing : bool, optional
if True, flag baselines in uvdata
if a participating antenna or polarization is missing in uvcal.
Dterm_cal : bool, optional
Calibrate the off-diagonal terms in the Jones matrix if present
in uvcal. Default is False. Currently not implemented.
delay_convention : str, optional
Exponent sign to use in conversion of 'delay' to 'gain' cal_type
if the input uvcal is not inherently 'gain' cal_type. Default to 'minus'.
undo : bool, optional
If True, undo the provided calibration. i.e. apply the calibration with
flipped gain_convention. Flag propagation rules apply the same.
Returns
-------
UVData, optional
Returns if not inplace
"""
# deepcopy for not inplace
if not inplace:
uvdata = copy.deepcopy(uvdata)
# input checks
if uvcal.cal_type == "delay":
# make a copy that is converted to gain
uvcal = copy.deepcopy(uvcal)
uvcal.convert_to_gain(delay_convention=delay_convention)
# D-term calibration
if Dterm_cal:
# check for D-terms
if -7 not in uvcal.jones_array and -8 not in uvcal.jones_array:
raise ValueError(
"Cannot apply D-term calibration without -7 or -8"
"Jones polarization in uvcal object."
)
raise NotImplementedError("D-term calibration is not yet implemented.")
# No D-term calibration
else:
# iterate over keys
for key in uvdata.get_antpairpols():
# get indices for this key
blt_inds = uvdata.antpair2ind(key)
pol_ind = np.argmin(
np.abs(
uvdata.polarization_array - polstr2num(key[2], uvdata.x_orientation)
)
)
# try to get gains for each antenna
ant1 = (key[0], key[2][0])
ant2 = (key[1], key[2][1])
if not uvcal._has_key(*ant1) or not uvcal._has_key(*ant2):
if flag_missing:
uvdata.flag_array[blt_inds, 0, :, pol_ind] = True
continue
gain = (
uvcal.get_gains(ant1) * np.conj(uvcal.get_gains(ant2))
).T # tranpose to match uvdata shape
flag = (uvcal.get_flags(ant1) | uvcal.get_flags(ant2)).T
# propagate flags
if prop_flags:
mask = np.isclose(gain, 0.0) | flag
gain[mask] = 1.0
uvdata.flag_array[blt_inds, 0, :, pol_ind] += mask
# apply to data
mult_gains = uvcal.gain_convention == "multiply"
if undo:
mult_gains = not mult_gains
if mult_gains:
uvdata.data_array[blt_inds, 0, :, pol_ind] *= gain
else:
uvdata.data_array[blt_inds, 0, :, pol_ind] /= gain
# update attributes
uvdata.history += "\nCalibrated with pyuvdata.utils.uvcalibrate."
if undo:
uvdata.vis_units = "UNCALIB"
else:
if uvcal.gain_scale is not None:
uvdata.vis_units = uvcal.gain_scale
if not inplace:
return uvdata
[docs]def apply_uvflag(
uvd, uvf, inplace=True, unflag_first=False, flag_missing=True, force_pol=True
):
"""
Apply flags from a UVFlag to a UVData instantiation.
Note that if uvf.Nfreqs or uvf.Ntimes is 1, it will broadcast flags across
that axis.
Parameters
----------
uvd : UVData object
UVData object to add flags to.
uvf : UVFlag object
A UVFlag object in flag mode.
inplace : bool
If True overwrite flags in uvd, otherwise return new object
unflag_first : bool
If True, completely unflag the UVData before applying flags.
Else, OR the inherent uvd flags with uvf flags.
flag_missing : bool
If input uvf is a baseline type and antpairs in uvd do not exist in uvf,
flag them in uvd. Otherwise leave them untouched.
force_pol : bool
If True, broadcast flags to all polarizations if they do not match.
Only works if uvf.Npols == 1.
Returns
-------
UVData
If not inplace, returns new UVData object with flags applied
"""
# assertions
if uvf.mode != "flag":
raise ValueError("UVFlag must be flag mode")
if not inplace:
uvd = copy.deepcopy(uvd)
# make a deepcopy by default b/c it is generally edited inplace downstream
uvf = copy.deepcopy(uvf)
# convert to baseline type
if uvf.type != "baseline":
# edits inplace
uvf.to_baseline(uvd, force_pol=force_pol)
else:
# make sure polarizations match or force_pol
uvd_pols, uvf_pols = (
uvd.polarization_array.tolist(),
uvf.polarization_array.tolist(),
)
if set(uvd_pols) != set(uvf_pols):
if uvf.Npols == 1 and force_pol:
# if uvf is 1pol we can make them match: also edits inplace
uvf.polarization_array = uvd.polarization_array
uvf.Npols = len(uvf.polarization_array)
uvf_pols = uvf.polarization_array.tolist()
else:
raise ValueError("Input uvf and uvd polarizations do not match")
# make sure polarization ordering is correct: also edits inplace
uvf.polarization_array = uvf.polarization_array[
[uvd_pols.index(pol) for pol in uvf_pols]
]
# check time and freq shapes match: if Ntimes or Nfreqs is 1, allow
# implicit broadcasting
if uvf.Ntimes == 1:
mismatch_times = False
elif uvf.Ntimes == uvd.Ntimes:
tdiff = np.unique(uvf.time_array) - np.unique(uvd.time_array)
mismatch_times = np.any(tdiff > np.max(np.abs(uvf._time_array.tols)))
else:
mismatch_times = True
if mismatch_times:
raise ValueError("UVFlag and UVData have mismatched time arrays.")
if uvf.Nfreqs == 1:
mismatch_freqs = False
elif uvf.Nfreqs == uvd.Nfreqs:
fdiff = np.unique(uvf.freq_array) - np.unique(uvd.freq_array)
mismatch_freqs = np.any(fdiff > np.max(np.abs(uvf._freq_array.tols)))
else:
mismatch_freqs = True
if mismatch_freqs:
raise ValueError("UVFlag and UVData have mismatched frequency arrays.")
# unflag if desired
if unflag_first:
uvd.flag_array[:] = False
# iterate over antpairs and apply flags: TODO need to be able to handle
# conjugated antpairs
uvf_antpairs = uvf.get_antpairs()
for ap in uvd.get_antpairs():
uvd_ap_inds = uvd.antpair2ind(ap)
if ap not in uvf_antpairs:
if flag_missing:
uvd.flag_array[uvd_ap_inds] = True
continue
uvf_ap_inds = uvf.antpair2ind(*ap)
# addition of boolean is OR
uvd.flag_array[uvd_ap_inds] += uvf.flag_array[uvf_ap_inds]
uvd.history += "\nFlagged with pyuvdata.utils.apply_uvflags."
if not inplace:
return uvd