def topo_posvels(xyz, toa):
"""
topo_posvels(xyz, toa)
This routine returns a PosVel instance , containing the positions
(m) and velocities (m / UT1 s) at the time of the toa and
referenced to the ITRF geocentric coordinates. This routine is
basically SOFA's pvtob() with an extra rotation from c2ixys.
"""
# All the times are passed as TT
tt = toa.mjd.tt.jd1, toa.mjd.tt.jd2
# Get a floating-point MJD to use for interpolating IERS values
mjd = toa.mjd.utc.mjd
# Gets x,y coords of Celestial Intermediate Pole and CIO locator s
X, Y, S = erfa.xys00a(*tt)
# Get dX and dY from IERS A
#dX = numpy.interp(mjd, iers_tab['MJD'], iers_tab['dX_2000A_B']) * u.arcsec
#dY = numpy.interp(mjd, iers_tab['MJD'], iers_tab['dY_2000A_B']) * u.arcsec
# Get dX and dY from IERS B
dX = numpy.interp(mjd, iers_tab['MJD'], iers_tab['dX_2000A']) * u.arcsec
dY = numpy.interp(mjd, iers_tab['MJD'], iers_tab['dY_2000A']) * u.arcsec
# Get GCRS to CIRS matrix
rc2i = erfa.c2ixys(X+dX.to(u.rad).value, Y+dY.to(u.rad).value, S)
# Gets the TIO locator s'
sp = erfa.sp00(*tt)
# Get X and Y from IERS A
#xp = numpy.interp(mjd, iers_tab['MJD'], iers_tab['PM_X_B']) * u.arcsec
#yp = numpy.interp(mjd, iers_tab['MJD'], iers_tab['PM_Y_B']) * u.arcsec
# Get X and Y from IERS B
xp = numpy.interp(mjd, iers_tab['MJD'], iers_tab['PM_x']) * u.arcsec
yp = numpy.interp(mjd, iers_tab['MJD'], iers_tab['PM_y']) * u.arcsec
# Get the polar motion matrix
rpm = erfa.pom00(xp.to(u.rad).value, yp.to(u.rad).value, sp)
# Observatory XYZ coords in meters
xyzm = [a.to(u.m).value for a in xyz]
x, y, z = erfa.trxp(rpm, xyzm)
# Functions of Earth Rotation Angle
ut1 = toa.mjd.ut1.jd1, toa.mjd.ut1.jd2
theta = erfa.era00(*ut1)
s, c = math.sin(theta), math.cos(theta)
# Position
pos = numpy.asarray([c*x - s*y, s*x + c*y, z])
pos = erfa.trxp(rc2i, pos) * u.m
# Earth rotation rate in radians per UT1 second
OM = 1.00273781191135448 * 2 * math.pi / erfa.DAYSEC
# Velocity
vel = numpy.asarray([OM * (-s*x - c*y), OM * (c*x - s*y), 0.0])
vel = erfa.trxp(rc2i, vel) * u.m / u.s
return utils.PosVel(pos, vel, obj=toa.obs, origin="EARTH")
def cirs_to_itrs_mat(time):
# compute the polar motion p-matrix
xp, yp = get_polar_motion(time)
sp = erfa.sp00(*get_jd12(time, 'tt'))
pmmat = erfa.pom00(xp, yp, sp)
# now determine the Earth Rotation Angle for the input obstime
# era00 accepts UT1, so we convert if need be
era = erfa.era00(*get_jd12(time, 'ut1'))
# c2tcio expects a GCRS->CIRS matrix, but we just set that to an I-matrix
# because we're already in CIRS
return erfa.c2tcio(np.eye(3), era, pmmat)
def tete_to_itrs_mat(time):
# compute the polar motion p-matrix
xp, yp = get_polar_motion(time)
sp = erfa.sp00(*get_jd12(time, 'tt'))
pmmat = erfa.pom00(xp, yp, sp)
# now determine the greenwich apparent siderial time for the input obstime
# we use the 2006A model for consistency with RBPN matrix use in GCRS <-> TETE
ujd1, ujd2 = get_jd12(time, 'ut1')
jd1, jd2 = get_jd12(time, 'tt')
gast = erfa.gst06a(ujd1, ujd2, jd1, jd2)
# c2tcio expects a GCRS->CIRS matrix, but we just set that to an I-matrix
# because we're already in CIRS equivalent frame
return erfa.c2tcio(np.eye(3), gast, pmmat)
def teme_to_itrs_mat(time):
# Sidereal time, rotates from ITRS to mean equinox
# Use 1982 model for consistency with Vallado et al (2006)
# http://www.celestrak.com/publications/aiaa/2006-6753/AIAA-2006-6753.pdf
gst = erfa.gmst82(*get_jd12(time, 'ut1'))
# Polar Motion
# Do not include TIO locator s' because it is not used in Vallado 2006
xp, yp = get_polar_motion(time)
pmmat = erfa.pom00(xp, yp, 0)
# rotation matrix
# c2tcio expects a GCRS->CIRS matrix as it's first argument.
# Here, we just set that to an I-matrix, because we're already
# in TEME and the difference between TEME and CIRS is just the
# rotation by the sidereal time rather than the Earth Rotation Angle
return erfa.c2tcio(np.eye(3), gst, pmmat)
def _polar_mot_matrix(obstime):
"""
Form the matrix of polar motion for a given date, IAU 2000.
The matrix operates in the sense V(TRS) = rpom * V(CIP), meaning that
it is the final rotation when computing the
pointing direction to a celestial source.
Parameters
----------
obstime : Time
time at which the polar motion should be calculated.
Returns
-------
3x3 rotation matrix due to polar motion
"""
# compute the polar motion p-matrix
xp, yp = get_polar_motion(obstime)
# noinspection PyArgumentList
sp = erfa.sp00(*get_jd12(obstime, "tt"))
polar_mot_mat = erfa.pom00(xp, yp, sp)
return polar_mot_mat
def tete_to_itrs_mat(time, rbpn=None):
"""Compute the polar motion p-matrix at the given time.
If the nutation-precession matrix is already known, it should be passed in,
as this is by far the most expensive calculation.
"""
xp, yp = get_polar_motion(time)
sp = erfa.sp00(*get_jd12(time, 'tt'))
pmmat = erfa.pom00(xp, yp, sp)
# now determine the greenwich apparent siderial time for the input obstime
# we use the 2006A model for consistency with RBPN matrix use in GCRS <-> TETE
ujd1, ujd2 = get_jd12(time, 'ut1')
jd1, jd2 = get_jd12(time, 'tt')
if rbpn is None:
# erfa.gst06a calls pnm06a to calculate rbpn and then gst06. Use it in
# favour of getting rbpn with erfa.pnm06a to avoid a possibly large array.
gast = erfa.gst06a(ujd1, ujd2, jd1, jd2)
else:
gast = erfa.gst06(ujd1, ujd2, jd1, jd2, rbpn)
# c2tcio expects a GCRS->CIRS matrix, but we just set that to an I-matrix
# because we're already in CIRS equivalent frame
return erfa.c2tcio(np.eye(3), gast, pmmat)
ERA = erfa.era00(DJMJD0 + DATE, TUT)
print("Earth rotation angle")
print('ERA = %.17f radians' % ERA)
print(" = %.17f degrees" % math.degrees(ERA))
print(" = %s%dd%dm%d.%ds" % erfa.a2af(6, ERA))
print(" = %s%dh%dm%d.%ds" % erfa.a2tf(6, ERA))
# Form celestial-terrestrial matrix (no polar motion yet).
##RC2TI = erfa.cr(RC2I)
##RC2TI = erfa.rz(ERA, RC2TI)
RC2TI = erfa.rz(ERA, RC2I)
print("celestial to terrestrial matrix (no polar motion)")
pprint(RC2TI)
# Polar motion matrix (TIRS->ITRS, IERS 2003).
RPOM = erfa.pom00(XP, YP, erfa.sp00(DJMJD0, TT))
# Form celestial-terrestrial matrix (including polar motion).
RC2IT = erfa.rxr(RPOM, RC2TI)
print("celestial to terrestrial matrix (including polar motion)")
pprint(RC2IT)
##B = scipy.matrix(RC2IT)
print('''
================================================
IAU 2000A, equinox based, using classical angles
================================================
''')
# Nutation, IAU 2000A.
ERA = erfa.era00(DJMJD0+DATE, TUT)
print("Earth rotation angle")
print('ERA = %.17f radians'%ERA)
print(" = %.17f degrees"%math.degrees(ERA))
print(" = %s%dd%dm%d.%ds"%erfa.a2af(6, ERA))
print(" = %s%dh%dm%d.%ds"%erfa.a2tf(6, ERA))
# Form celestial-terrestrial matrix (no polar motion yet).
##RC2TI = erfa.cr(RC2I)
##RC2TI = erfa.rz(ERA, RC2TI)
RC2TI = erfa.rz(ERA, RC2I)
print("celestial to terrestrial matrix (no polar motion)")
pprint(RC2TI)
# Polar motion matrix (TIRS->ITRS, IERS 2003).
RPOM = erfa.pom00(XP, YP, erfa.sp00(DJMJD0,TT))
# Form celestial-terrestrial matrix (including polar motion).
RC2IT = erfa.rxr(RPOM, RC2TI)
print("celestial to terrestrial matrix (including polar motion)")
pprint(RC2IT)
##B = scipy.matrix(RC2IT)
print('''
================================================
IAU 2000A, equinox based, using classical angles
================================================
''')
# Nutation, IAU 2000A.
def old_gcrs_posvel_from_itrf(loc, toas, obsname="obs"):
"""Return a list of PosVel instances for the observatory at the TOA times.
Observatory location should be given in the loc argument as an astropy
EarthLocation object. This location will be in the ITRF frame (i.e.
co-rotating with the Earth).
The optional obsname argument will be used as label in the returned
PosVel instance.
This routine returns a list of PosVel instances, containing the
positions (m) and velocities (m / s) at the times of the toas and
referenced to the Earth-centered Inertial (ECI, aka GCRS) coordinates.
This routine is basically SOFA's pvtob() [Position and velocity of
a terrestrial observing station] with an extra rotation from c2ixys()
[Form the celestial to intermediate-frame-of-date matrix given the CIP
X,Y and the CIO locator s].
"""
unpack = False
# If the input is a single TOA (i.e. a row from the table),
# then put it into a list
if type(toas) == table.row.Row:
ttoas = Time([toas["mjd"]])
unpack = True
elif type(toas) == table.table.Table:
ttoas = toas["mjd"]
elif isinstance(toas, Time):
if toas.isscalar:
ttoas = Time([toas])
unpack = True
else:
ttoas = toas
else:
if np.isscalar(toas):
ttoas = Time([toas], format="mjd")
unpack = True
else:
ttoas = toas
N = len(ttoas)
if len(ttoas.shape) != 1:
raise ValueError("At most one-dimensional array of times possible, "
"shape was {}".format(ttoas.shape))
# Get various times from the TOAs as arrays
tts = np.asarray([(t.jd1, t.jd2) for t in ttoas.tt]).T
ut1s = np.asarray([(t.jd1, t.jd2) for t in ttoas.ut1]).T
mjds = np.asarray(ttoas.mjd)
iers_b = get_iers_b_up_to_date(mjds.max())
# Get x, y coords of Celestial Intermediate Pole and CIO locator s
X, Y, S = erfa.xys00a(*tts)
# Get dX and dY from IERS A in arcsec and convert to radians
# dX = np.interp(mjds, iers_tab['MJD'], iers_tab['dX_2000A_B']) * asec2rad
# dY = np.interp(mjds, iers_tab['MJD'], iers_tab['dY_2000A_B']) * asec2rad
# Get dX and dY from IERS B in arcsec and convert to radians
dX = np.interp(mjds, iers_b["MJD"].to_value(u.d),
iers_b["dX_2000A"].to_value(u.rad))
dY = np.interp(mjds, iers_b["MJD"].to_value(u.d),
iers_b["dY_2000A"].to_value(u.rad))
# Get GCRS to CIRS matrices
rc2i = erfa.c2ixys(X + dX, Y + dY, S)
# Gets the TIO locator s'
sp = erfa.sp00(*tts)
# Get X and Y from IERS A in arcsec and convert to radians
# xp = np.interp(mjds, iers_tab['MJD'], iers_tab['PM_X_B']) * asec2rad
# yp = np.interp(mjds, iers_tab['MJD'], iers_tab['PM_Y_B']) * asec2rad
# Get X and Y from IERS B in arcsec and convert to radians
xp = np.interp(mjds, iers_b["MJD"].to_value(u.d),
iers_b["PM_x"].to_value(u.rad))
yp = np.interp(mjds, iers_b["MJD"].to_value(u.d),
iers_b["PM_y"].to_value(u.rad))
# Get the polar motion matrices
rpm = erfa.pom00(xp, yp, sp)
# Observatory geocentric coords in m
xyzm = np.array([a.to_value(u.m) for a in loc.geocentric])
x, y, z = np.dot(xyzm, rpm).T
# Functions of Earth Rotation Angle
theta = erfa.era00(*ut1s)
s, c = np.sin(theta), np.cos(theta)
sx, cx = s * x, c * x
sy, cy = s * y, c * y
# Initial positions and velocities
iposs = np.asarray([cx - sy, sx + cy, z]).T
ivels = np.asarray([OM * (-sx - cy), OM * (cx - sy), np.zeros_like(x)]).T
# There is probably a way to do this with np.einsum or something...
# and here it is .
poss = np.empty((N, 3), dtype=np.float64)
vels = np.empty((N, 3), dtype=np.float64)
poss = np.einsum("ij,ijk->ik", iposs, rc2i)
vels = np.einsum("ij,ijk->ik", ivels, rc2i)
r = PosVel(poss.T * u.m, vels.T * u.m / u.s, obj=obsname, origin="earth")
if unpack:
return r[0]
else:
return r
for c,a in erfa.a2af(6, ERA):
print(" = %s"%c, end='')
print("%dd%dm%d.%ds"%tuple(a))
for c,a in erfa.a2af(6, ERA):
print(" = %s"%c, end='')
print("%dd%dm%d.%ds"%tuple(a))
# Form celestial-terrestrial matrix (no polar motion yet).
##RC2TI = erfa.cr(RC2I)
##RC2TI = erfa.rz(ERA, RC2TI)
RC2TI = erfa.rz(ERA, RC2I)
print("celestial to terrestrial matrix (no polar motion)")
pprint(RC2TI)
# Polar motion matrix (TIRS->ITRS, IERS 2003).
RPOM = erfa.pom00(np.array([XP]), np.array([YP]), erfa.sp00(DJMJD0,TT))
# Form celestial-terrestrial matrix (including polar motion).
RC2IT = erfa.rxr(RPOM, RC2TI)
print("celestial to terrestrial matrix (including polar motion)")
pprint(RC2IT)
##B = scipy.matrix(RC2IT)
print('''
================================================
IAU 2000A, equinox based, using classical angles
================================================
''')
# Nutation, IAU 2000A.