def velocity_of_Earth(full_BJD):
"""
Calculate 3D velocity of Earth for given epoch.
If you need velocity projected on the plane of the sky, then use
:py:func:`~MulensModel.coordinates.Coordinates.v_Earth_projected`
Parameters :
full_BJD: *float*
Barycentric Julian Data. Full means it should begin
with 245... or 246...
Returns :
velocity: *np.ndarray* (*float*, size of (3,))
3D velocity in km/s. The frame follows *Astropy* conventions.
"""
# The 4 lines below, that calculate velocity for given epoch,
# are based on astropy 1.3 code:
# https://github.com/astropy/astropy/blob/master/astropy/
# coordinates/solar_system.py
time = Time(full_BJD, format='jd', scale='tdb')
(jd1, jd2) = get_jd12(time, 'tdb')
(earth_pv_helio, earth_pv_bary) = erfa.epv00(jd1, jd2)
factor = 1731.45683 # This scales AU/day to km/s.
# The returned values are of np.ndarray type in astropy v1 and v2,
# but np.void in v3. The np.asarray() works in both cases.
velocity = np.asarray(earth_pv_bary[1]) * factor
return velocity
def prepare_earth_position_vel(time):
"""
Get barycentric position and velocity, and heliocentric position of Earth
Parameters
-----------
time : `~astropy.time.Time`
time at which to calculate position and velocity of Earth
Returns
--------
earth_pv : `np.ndarray`
Barycentric position and velocity of Earth, in au and au/day
earth_helio : `np.ndarray`
Heliocentric position of Earth in au
"""
# this goes here to avoid circular import errors
from astropy.coordinates.solar_system import (
get_body_barycentric,
get_body_barycentric_posvel,
solar_system_ephemeris,
)
# get barycentric position and velocity of earth
ephemeris = solar_system_ephemeris.get()
# if we are using the builtin erfa based ephemeris,
# we can use the fact that epv00 already provides all we need.
# This avoids calling epv00 twice, once
# in get_body_barycentric_posvel('earth') and once in
# get_body_barycentric('sun')
if ephemeris == 'builtin':
jd1, jd2 = get_jd12(time, 'tdb')
earth_pv_heliocentric, earth_pv = erfa.epv00(jd1, jd2)
earth_heliocentric = earth_pv_heliocentric['p']
# all other ephemeris providers probably don't have a shortcut like this
else:
earth_p, earth_v = get_body_barycentric_posvel('earth', time)
# get heliocentric position of earth, preparing it for passing to erfa.
sun = get_body_barycentric('sun', time)
earth_heliocentric = (earth_p - sun).get_xyz(xyz_axis=-1).to_value(
u.au)
# Also prepare earth_pv for passing to erfa, which wants it as
# a structured dtype.
earth_pv = pav2pv(
earth_p.get_xyz(xyz_axis=-1).to_value(u.au),
earth_v.get_xyz(xyz_axis=-1).to_value(u.au / u.d))
return earth_pv, earth_heliocentric
def test_icrs_altaz_moonish(testframe):
"""
Check that something expressed in *ICRS* as being moon-like goes to the
right AltAz distance
"""
# we use epv00 instead of get_sun because get_sun includes aberration
earth_pv_helio, earth_pv_bary = erfa.epv00(*get_jd12(testframe.obstime, 'tdb'))
earth_icrs_xyz = earth_pv_bary[0]*u.au
moonoffset = [0, 0, MOONDIST.value]*MOONDIST.unit
moonish_icrs = ICRS(CartesianRepresentation(earth_icrs_xyz + moonoffset))
moonaa = moonish_icrs.transform_to(testframe)
# now check that the distance change is similar to earth radius
assert 1000*u.km < np.abs(moonaa.distance - MOONDIST).to(u.au) < 7000*u.km
def get_sun(time):
"""
Determines the location of the sun at a given time (or times, if the input
is an array `~astropy.time.Time` object), in geocentric coordinates.
Parameters
----------
time : `~astropy.time.Time`
The time(s) at which to compute the location of the sun.
Returns
-------
newsc : `~astropy.coordinates.SkyCoord`
The location of the sun as a `~astropy.coordinates.SkyCoord` in the
`~astropy.coordinates.GCRS` frame.
Notes
-----
The algorithm for determining the sun/earth relative position is based
on the simplified version of VSOP2000 that is part of ERFA. Compared to
JPL's ephemeris, it should be good to about 4 km (in the Sun-Earth
vector) from 1900-2100 C.E., 8 km for the 1800-2200 span, and perhaps
250 km over the 1000-3000.
"""
earth_pv_helio, earth_pv_bary = erfa.epv00(*get_jd12(time, 'tdb'))
# We have to manually do aberration because we're outputting directly into
# GCRS
earth_p = earth_pv_helio['p']
earth_v = earth_pv_bary['v']
# convert barycentric velocity to units of c, but keep as array for passing in to erfa
earth_v /= c.to_value(u.au/u.d)
dsun = np.sqrt(np.sum(earth_p**2, axis=-1))
invlorentz = (1-np.sum(earth_v**2, axis=-1))**0.5
properdir = erfa.ab(earth_p/dsun.reshape(dsun.shape + (1,)),
-earth_v, dsun, invlorentz)
cartrep = CartesianRepresentation(x=-dsun*properdir[..., 0] * u.AU,
y=-dsun*properdir[..., 1] * u.AU,
z=-dsun*properdir[..., 2] * u.AU)
return SkyCoord(cartrep, frame=GCRS(obstime=time))
def __init__(self, utc, longitude, latitude, altitude):
try:
super().__init__(utc, longitude, latitude, altitude)
except TypeError:
super(Ephem, self).__init__(utc, longitude, latitude, altitude)
# julian centuries at the given UTC
self.jc = (self.tdb1+self.tdb2-erfa.DJ00)/erfa.DJC
# heliocentric position of major bodies
self.p94 = [erfa.plan94(self.tdb1, self.tdb2, i) for i in range(1,9)]
# Earth heliocentric position and velocity
self.eph, self.epb = erfa.epv00(self.tdb1, self.tdb2)
self.distances_from_earth = {}
self.RA_DEC = {}
## # precession angles
## eps0,psia,oma,bpa,bqa,pia,bpia,epsa,chia,za,zetaa,thetaa,pa,gam,phi,psi = erfa.p06e(self.tt1, self.tt2)
##
## # Fundamental argument of major bodies
## mer = erfa.fame03(self.jc))
self.sun()
self.planets()
def _get_body_barycentric_posvel(body,
time,
ephemeris=None,
get_velocity=True):
"""Calculate the barycentric position (and velocity) of a solar system body.
Parameters
----------
body : str or other
The solar system body for which to calculate positions. Can also be a
kernel specifier (list of 2-tuples) if the ``ephemeris`` is a JPL
kernel.
time : `~astropy.time.Time`
Time of observation.
ephemeris : str, optional
Ephemeris to use. By default, use the one set with
``astropy.coordinates.solar_system_ephemeris.set``
get_velocity : bool, optional
Whether or not to calculate the velocity as well as the position.
Returns
-------
position : `~astropy.coordinates.CartesianRepresentation` or tuple
Barycentric (ICRS) position or tuple of position and velocity.
Notes
-----
No velocity can be calculated with the built-in ephemeris for the Moon.
Whether or not velocities are calculated makes little difference for the
built-in ephemerides, but for most JPL ephemeris files, the execution time
roughly doubles.
"""
if ephemeris is None:
ephemeris = solar_system_ephemeris.get()
if ephemeris is None:
raise ValueError(_EPHEMERIS_NOTE)
kernel = solar_system_ephemeris.kernel
else:
kernel = _get_kernel(ephemeris)
jd1, jd2 = get_jd12(time, 'tdb')
if kernel is None:
body = body.lower()
earth_pv_helio, earth_pv_bary = erfa.epv00(jd1, jd2)
if body == 'earth':
body_pv_bary = earth_pv_bary
elif body == 'moon':
if get_velocity:
raise KeyError("the Moon's velocity cannot be calculated with "
"the '{}' ephemeris.".format(ephemeris))
return calc_moon(time).cartesian
else:
sun_pv_bary = erfa.pvmpv(earth_pv_bary, earth_pv_helio)
if body == 'sun':
body_pv_bary = sun_pv_bary
else:
try:
body_index = PLAN94_BODY_NAME_TO_PLANET_INDEX[body]
except KeyError:
raise KeyError(
"{}'s position and velocity cannot be "
"calculated with the '{}' ephemeris.".format(
body, ephemeris))
body_pv_helio = erfa.plan94(jd1, jd2, body_index)
body_pv_bary = erfa.pvppv(body_pv_helio, sun_pv_bary)
body_pos_bary = CartesianRepresentation(body_pv_bary['p'],
unit=u.au,
xyz_axis=-1,
copy=False)
if get_velocity:
body_vel_bary = CartesianRepresentation(body_pv_bary['v'],
unit=u.au / u.day,
xyz_axis=-1,
copy=False)
else:
if isinstance(body, str):
# Look up kernel chain for JPL ephemeris, based on name
try:
kernel_spec = BODY_NAME_TO_KERNEL_SPEC[body.lower()]
except KeyError:
raise KeyError("{}'s position cannot be calculated with "
"the {} ephemeris.".format(body, ephemeris))
else:
# otherwise, assume the user knows what their doing and intentionally
# passed in a kernel chain
kernel_spec = body
# jplephem cannot handle multi-D arrays, so convert to 1D here.
jd1_shape = getattr(jd1, 'shape', ())
if len(jd1_shape) > 1:
jd1, jd2 = jd1.ravel(), jd2.ravel()
# Note that we use the new jd1.shape here to create a 1D result array.
# It is reshaped below.
body_posvel_bary = np.zeros((2 if get_velocity else 1, 3) +
getattr(jd1, 'shape', ()))
for pair in kernel_spec:
spk = kernel[pair]
if spk.data_type == 3:
# Type 3 kernels contain both position and velocity.
posvel = spk.compute(jd1, jd2)
if get_velocity:
body_posvel_bary += posvel.reshape(body_posvel_bary.shape)
else:
body_posvel_bary[0] += posvel[:4]
else:
# spk.generate first yields the position and then the
# derivative. If no velocities are desired, body_posvel_bary
# has only one element and thus the loop ends after a single
# iteration, avoiding the velocity calculation.
for body_p_or_v, p_or_v in zip(body_posvel_bary,
spk.generate(jd1, jd2)):
body_p_or_v += p_or_v
body_posvel_bary.shape = body_posvel_bary.shape[:2] + jd1_shape
body_pos_bary = CartesianRepresentation(body_posvel_bary[0],
unit=u.km,
copy=False)
if get_velocity:
body_vel_bary = CartesianRepresentation(body_posvel_bary[1],
unit=u.km / u.day,
copy=False)
return (body_pos_bary, body_vel_bary) if get_velocity else body_pos_bary
)
reprd("CIRS -> topocentric:", rot, dot)
# CIRS to topocentric.
aob, zob, hob, dob, rob = erfa.atio13(ri, di, utc1, utc2, dut1, elong, phi, hm, xp, yp, phpa, tc, rh, wl)
reprd("CIRS -> observed:", rob, dob)
# ICRS to observed.
aob, zob, hob, dob, rob, eo = erfa.atco13(
rc, dc, pr, pd, px, rv, utc1, utc2, dut1, elong, phi, hm, xp, yp, phpa, tc, rh, wl
)
reprd("ICRS -> observed:", rob, dob)
# ICRS to CIRS using some user-supplied parameters.
# SOFA heliocentric Earth ephemeris.
pvh, pvb = erfa.epv00(tt1, tt2)
# JPL DE405 barycentric Earth ephemeris.
pvb = np.array(
[
(
(-0.9741704366519668, -0.2115201000882231, -0.0917583114068277),
(0.0036436589347388, -0.0154287318503146, -0.0066892203821059),
)
]
)
# era 2000A CIP.
r = erfa.pnm00a(tt1, tt2)
x, y = erfa.bpn2xy(r)
reprd("CIRS -> topocentric:", rot, dot)
# CIRS to topocentric.
aob, zob, hob, dob, rob = erfa.atio13(ri, di, utc1, utc2, dut1, elong, phi, hm,
xp, yp, phpa, tc, rh, wl)
reprd("CIRS -> observed:", rob, dob)
# ICRS to observed.
aob, zob, hob, dob, rob, eo = erfa.atco13(rc, dc, pr, pd, px, rv, utc1, utc2,
dut1, elong, phi, hm, xp, yp, phpa,
tc, rh, wl)
reprd("ICRS -> observed:", rob, dob)
# ICRS to CIRS using some user-supplied parameters.
# SOFA heliocentric Earth ephemeris.
pvh, pvb = erfa.epv00(tt1, tt2)
# JPL DE405 barycentric Earth ephemeris.
pvb = ((-0.9741704366519668, -0.2115201000882231, -0.0917583114068277),
(0.0036436589347388, -0.0154287318503146, -0.0066892203821059))
# era 2000A CIP.
r = erfa.pnm00a(tt1, tt2)
x, y = erfa.bpn2xy(r)
# Apply IERS corrections.
x += dx
y += dy
# SOFA CIO locator. */
s = erfa.s06(tt1, tt2, x, y)