def calcPos(self, mjd, config):
"""Calculate the moon's ecliptic lon/lat and geocentric RA/Dec, for the given MJD(s)."""
self.mjd = numpy.copy(mjd)
self.ra = numpy.zeros(len(mjd), 'float')
self.dec = numpy.zeros(len(mjd), 'float')
for i in range(len(mjd)):
# Calculate moon's position.
ra_RAD, dec_RAD, diam = slalib.sla_rdplan(mjd[i], 3,
config['longitude']*_deg2rad, config['latitude']*_deg2rad)
self.ra[i] = ra_RAD * _rad2deg
self.dec[i] = dec_RAD * _rad2deg
# Calculate the lunar phase.
eclon = numpy.zeros(len(mjd), 'float')
eclat = numpy.zeros(len(mjd), 'float')
for i in range(len(mjd)):
eclon[i], eclat[i] = slalib.sla_eqecl(self.ra[i]*_deg2rad, self.dec[i]*_deg2rad, self.mjd[i])
# Calculate the solar longitude.
sun = Sun()
lon_sun = sun.getLon(self.mjd)*_deg2rad
# Calculate the solar elongation of the Moon.
solarelong = numpy.arccos(numpy.cos((lon_sun - eclon)) * numpy.cos(eclat))
# Calculate the phase of the moon. This is the 0-180 degrees phase.
self.phase = 180.0 - solarelong*_rad2deg
# Calculate the illumination of the Moon. This is between 0 - 100, and is what Opsim calls 'moonPhase'.
self.illum = ( 1 + numpy.cos(self.phase*_deg2rad) )/2.0 * 100.0
return
def calcPos(self, mjd, config):
"""Calculate the moon's ecliptic lon/lat and geocentric RA/Dec, for the given MJD(s)."""
self.mjd = numpy.copy(mjd)
self.ra = numpy.zeros(len(mjd), 'float')
self.dec = numpy.zeros(len(mjd), 'float')
for i in range(len(mjd)):
# Calculate moon's position.
ra_RAD, dec_RAD, diam = slalib.sla_rdplan(
mjd[i], 3, config['longitude'] * _deg2rad,
config['latitude'] * _deg2rad)
self.ra[i] = ra_RAD * _rad2deg
self.dec[i] = dec_RAD * _rad2deg
# Calculate the lunar phase.
eclon = numpy.zeros(len(mjd), 'float')
eclat = numpy.zeros(len(mjd), 'float')
for i in range(len(mjd)):
eclon[i], eclat[i] = slalib.sla_eqecl(self.ra[i] * _deg2rad,
self.dec[i] * _deg2rad,
self.mjd[i])
# Calculate the solar longitude.
sun = Sun()
lon_sun = sun.getLon(self.mjd) * _deg2rad
# Calculate the solar elongation of the Moon.
solarelong = numpy.arccos(
numpy.cos((lon_sun - eclon)) * numpy.cos(eclat))
# Calculate the phase of the moon. This is the 0-180 degrees phase.
self.phase = 180.0 - solarelong * _rad2deg
# Calculate the illumination of the Moon. This is between 0 - 100, and is what Opsim calls 'moonPhase'.
self.illum = (1 + numpy.cos(self.phase * _deg2rad)) / 2.0 * 100.0
return
def transform_celestial(coords, systems):
lons, lats = np.radians(coords['lon']), np.radians(coords['lat'])
out = Table()
out['lon'] = np.zeros(len(coords), dtype='float64')
out['lat'] = np.zeros(len(coords), dtype='float64')
for ii, (lon, lat) in enumerate(zip(lons, lats)):
# First convert to FK5 J2000 in all cases
if systems['in'] == 'fk4':
lon, lat = slalib.sla_fk45z(lon, lat, 2000.0012775136652)
elif systems['in'] == 'icrs':
lon, lat = slalib.sla_hfk5z(lon, lat, 2000)[:2]
elif systems['in'] == 'galactic':
lon, lat = slalib.sla_galeq(lon, lat)
elif systems['in'] == 'ecliptic':
lon, lat = slalib.sla_ecleq(lon, lat, 51544)
# Now convert from FK5 J2000 to out system
if systems['out'] == 'fk4':
# FK5 -> FK4 at BEPOCH 2000 assuming no proper motion or parallax
lon, lat = slalib.sla_fk54z(lon, lat, 2000.0012775136652)[:2]
elif systems['out'] == 'icrs':
# FK5 -> Hipparcos (i.e. ICRF, which is as close as SLALIB
# gets to ICRS) at epoch 2000 and with no proper motion
lon, lat = slalib.sla_fk5hz(lon, lat, 2000)
elif systems['out'] == 'galactic':
# FK5 -> Galactic
lon, lat = slalib.sla_eqgal(lon, lat)
elif systems['out'] == 'ecliptic':
# FK5 -> Ecliptic at TDB (MJD) 51544 (i.e. J2000)
lon, lat = slalib.sla_eqecl(lon, lat, 51544)
out[ii]['lon'] = np.degrees(lon)
out[ii]['lat'] = np.degrees(lat)
return out
def transform_celestial(coords, systems):
lons, lats = np.radians(coords['lon']), np.radians(coords['lat'])
out = Table()
out['lon'] = np.zeros(len(coords), dtype='float64')
out['lat'] = np.zeros(len(coords), dtype='float64')
for ii, (lon, lat) in enumerate(zip(lons, lats)):
# First convert to FK5 J2000 in all cases
if systems['in'] == 'fk4':
lon, lat = slalib.sla_fk45z(lon, lat, 2000.0012775136652)
elif systems['in'] == 'icrs':
lon, lat = slalib.sla_hfk5z(lon, lat, 2000)[:2]
elif systems['in'] == 'galactic':
lon, lat = slalib.sla_galeq(lon, lat)
elif systems['in'] == 'ecliptic':
lon, lat = slalib.sla_ecleq(lon, lat, 51544)
# Now convert from FK5 J2000 to out system
if systems['out'] == 'fk4':
# FK5 -> FK4 at BEPOCH 2000 assuming no proper motion or parallax
lon, lat = slalib.sla_fk54z(lon, lat, 2000.0012775136652)[:2]
elif systems['out'] == 'icrs':
# FK5 -> Hipparcos (i.e. ICRF, which is as close as SLALIB
# gets to ICRS) at epoch 2000 and with no proper motion
lon, lat = slalib.sla_fk5hz(lon, lat, 2000)
elif systems['out'] == 'galactic':
# FK5 -> Galactic
lon, lat = slalib.sla_eqgal(lon, lat)
elif systems['out'] == 'ecliptic':
# FK5 -> Ecliptic at TDB (MJD) 51544 (i.e. J2000)
lon, lat = slalib.sla_eqecl(lon, lat, 51544)
out[ii]['lon'] = np.degrees(lon)
out[ii]['lat'] = np.degrees(lat)
return out
def convert(coords, systems):
if not set(systems.values()).issubset(SUPPORTED_SYSTEMS):
return None
lons, lats = np.radians(coords['lon']), np.radians(coords['lat'])
for ii, (lon, lat) in enumerate(zip(lons, lats)):
# First convert to FK5 J2000 in all cases
if systems['in'] == 'fk4':
lon, lat = slalib.sla_fk45z(lon, lat, 2000.0012775136652)
elif systems['in'] == 'icrs':
lon, lat = slalib.sla_hfk5z(lon, lat, 2000)[:2]
elif systems['in'] == 'galactic':
lon, lat = slalib.sla_galeq(lon, lat)
elif systems['in'] == 'ecliptic':
lon, lat = slalib.sla_ecleq(lon, lat, 51544)
# Now convert from FK5 J2000 to out system
if systems['out'] == 'fk4':
# FK5 -> FK4 at BEPOCH 2000 assuming no proper motion or parallax
lon, lat = slalib.sla_fk54z (lon, lat, 2000.0012775136652)[:2]
elif systems['out'] == 'icrs':
# FK5 -> Hipparcos (i.e. ICRF, which is as close as SLALIB
# gets to ICRS) at epoch 2000 and with no proper motion
lon, lat = slalib.sla_fk5hz(lon, lat, 2000)
elif systems['out'] == 'galactic':
# FK5 -> Galactic
lon, lat = slalib.sla_eqgal(lon, lat)
elif systems['out'] == 'ecliptic':
# FK5 -> Ecliptic at TDB (MJD) 51544 (i.e. J2000)
lon, lat = slalib.sla_eqecl(lon, lat, 51544)
lons[ii], lats[ii] = lon, lat
return dict(lon=np.degrees(lons), lat=np.degrees(lats))
# Read in initial coordinates as J2000 coordinates
data_j2000 = np.radians(np.loadtxt('../initial_coords.txt'))
ra_j2000_fk5, dec_j2000_fk5 = data_j2000[:, 0], data_j2000[:, 1]
vals = {}
for system in 'FK4', 'Ecliptic', 'Galactic', 'ICRS':
vals[system] = [np.zeros_like(ra_j2000_fk5), np.zeros_like(dec_j2000_fk5)]
for ii, (raj, decj) in enumerate(zip(ra_j2000_fk5, dec_j2000_fk5)):
# FK5 -> FK4 at BEPOCH 2000.0 assuming no proper motion or parallax
r1950, d1950, dr1950, dd1950 = S.sla_fk54z(raj, decj, 2000.0)
vals['FK4'][0][ii], vals['FK4'][1][ii] = r1950, d1950
# FK5 -> Ecliptic at TDB (MJD) 51544.0 (i.e. J2000)
dl, db = S.sla_eqecl(raj, decj, 51544.0)
vals['Ecliptic'][0][ii], vals['Ecliptic'][1][ii] = dl, db
# FK5 -> Galactic
dl, db = S.sla_eqgal(raj, decj)
vals['Galactic'][0][ii], vals['Galactic'][1][ii] = dl, db
# FK5 -> Hipparcos (i.e. ICRF, which is as close as SLALIB
# gets to ICRS) at epoch 2000.0 and with no proper motion
rh, dh = S.sla_fk5hz(raj, decj, 2000.0)
vals['ICRS'][0][ii], vals['ICRS'][1][ii] = rh, dh
glon = vals['Galactic'][0]
glat = vals['Galactic'][1]
np.savetxt('coords_galactic.txt',
zip(np.degrees(glon), np.degrees(glat)),
# Read in initial coordinates as J2000 coordinates
data_j2000 = np.radians(np.loadtxt('../initial_coords.txt'))
ra_j2000_fk5, dec_j2000_fk5 = data_j2000[:,0], data_j2000[:,1]
vals = {}
for system in 'FK4', 'Ecliptic', 'Galactic', 'ICRS':
vals[system] = [np.zeros_like(ra_j2000_fk5), np.zeros_like(dec_j2000_fk5)]
for ii, (raj, decj) in enumerate(zip(ra_j2000_fk5, dec_j2000_fk5)):
# FK5 -> FK4 at BEPOCH 2000.0 assuming no proper motion or parallax
r1950, d1950, dr1950, dd1950 = S.sla_fk54z (raj, decj, 2000.0)
vals['FK4'][0][ii],vals['FK4'][1][ii] = r1950, d1950
# FK5 -> Ecliptic at TDB (MJD) 51544.0 (i.e. J2000)
dl, db = S.sla_eqecl(raj, decj, 51544.0)
vals['Ecliptic'][0][ii],vals['Ecliptic'][1][ii] = dl, db
# FK5 -> Galactic
dl, db = S.sla_eqgal(raj, decj)
vals['Galactic'][0][ii],vals['Galactic'][1][ii] = dl, db
# FK5 -> Hipparcos (i.e. ICRF, which is as close as SLALIB
# gets to ICRS) at epoch 2000.0 and with no proper motion
rh, dh = S.sla_fk5hz(raj, decj, 2000.0)
vals['ICRS'][0][ii],vals['ICRS'][1][ii] = rh, dh
glon = vals['Galactic'][0]
glat = vals['Galactic'][1]
np.savetxt('coords_galactic.txt', zip(np.degrees(glon),
def read(self, parfilenm):
self.FILE = parfilenm
pf = open(parfilenm)
for line in pf.readlines():
# Convert any 'D-' or 'D+' to 'E-' or 'E+'
line = line.replace("D-", "E-")
line = line.replace("D+", "E+")
try:
splitline = line.split()
key = splitline[0]
if key in str_keys:
setattr(self, key, splitline[1])
elif key in float_keys:
try:
setattr(self, key, float(splitline[1]))
except ValueError:
pass
if len(
splitline
) == 3: # Some parfiles don't have flags, but do have errors
if splitline[2] not in ['0', '1']:
setattr(self, key + '_ERR', float(splitline[2]))
if len(splitline) == 4:
setattr(self, key + '_ERR', float(splitline[3]))
except:
print ''
# Read PSR name
if hasattr(self, 'PSR'):
setattr(self, 'PSR', self.PSR)
if hasattr(self, 'PSRJ'):
setattr(self, 'PSRJ', self.PSRJ)
# Deal with Ecliptic coords
if (hasattr(self, 'BETA') and hasattr(self, 'LAMBDA')):
self.use_eclip = True
setattr(self, 'ELAT', self.BETA)
setattr(self, 'ELONG', self.LAMBDA)
if (slalib and hasattr(self, 'ELAT') and hasattr(self, 'ELONG')):
self.use_eclip = True
if hasattr(self, 'POSEPOCH'):
epoch = self.POSEPOCH
else:
epoch = self.PEPOCH
ra_rad, dec_rad = sla_ecleq(self.ELONG * pu.DEGTORAD,
self.ELAT * pu.DEGTORAD, epoch)
rstr = pu.coord_to_string(*pu.rad_to_hms(ra_rad))
dstr = pu.coord_to_string(*pu.rad_to_dms(dec_rad))
setattr(self, 'RAJ', rstr)
setattr(self, 'DECJ', dstr)
if hasattr(self, 'RAJ'):
setattr(self, 'RA_RAD', pu.ra_to_rad(self.RAJ))
if hasattr(self, 'DECJ'):
setattr(self, 'DEC_RAD', pu.dec_to_rad(self.DECJ))
# Compute the Galactic coords
if (slalib and hasattr(self, 'RA_RAD') and hasattr(self, 'DEC_RAD')):
l, b = sla_eqgal(self.RA_RAD, self.DEC_RAD)
setattr(self, 'GLONG', l * pu.RADTODEG)
setattr(self, 'GLAT', b * pu.RADTODEG)
# Compute the Ecliptic coords
if (slalib and hasattr(self, 'RA_RAD') and hasattr(self, 'DEC_RAD')):
if hasattr(self, 'POSEPOCH'):
epoch = self.POSEPOCH
else:
epoch = self.PEPOCH
elon, elat = sla_eqecl(self.RA_RAD, self.DEC_RAD, epoch)
setattr(self, 'ELONG', elon * pu.RADTODEG)
setattr(self, 'ELAT', elat * pu.RADTODEG)
if hasattr(self, 'P'):
setattr(self, 'P0', self.P)
if hasattr(self, 'P0'):
setattr(self, 'F0', 1.0 / self.P0)
if hasattr(self, 'F0'):
setattr(self, 'P0', 1.0 / self.F0)
if hasattr(self, 'F1'):
setattr(self, 'P1', -self.F1 / (self.F0 * self.F0))
if hasattr(self, 'FB0'):
setattr(self, 'PB', (1.0 / self.FB0) / 86400.0)
if hasattr(self, 'P0_ERR'):
if hasattr(self, 'P1_ERR'):
f, ferr, fd, fderr = pu.pferrs(self.P0, self.P0_ERR, self.P1,
self.P1_ERR)
setattr(self, 'F0_ERR', ferr)
setattr(self, 'F1', fd)
setattr(self, 'F1_ERR', fderr)
else:
f, fd, = pu.p_to_f(self.P0, self.P1)
setattr(self, 'F0_ERR', self.P0_ERR / (self.P0 * self.P0))
setattr(self, 'F1', fd)
if hasattr(self, 'F0_ERR'):
if hasattr(self, 'F1_ERR'):
p, perr, pd, pderr = pu.pferrs(self.F0, self.F0_ERR, self.F1,
self.F1_ERR)
setattr(self, 'P0_ERR', perr)
setattr(self, 'P1', pd)
setattr(self, 'P1_ERR', pderr)
else:
p, pd, = pu.p_to_f(self.F0, self.F1)
setattr(self, 'P0_ERR', self.F0_ERR / (self.F0 * self.F0))
setattr(self, 'P1', pd)
if hasattr(self, 'DM'):
setattr(self, 'DM', self.DM)
if hasattr(self, 'EPS1') and hasattr(self, 'EPS2'):
self.use_ell = True
ecc = math.sqrt(self.EPS1 * self.EPS1 + self.EPS2 * self.EPS2)
omega = math.atan2(self.EPS1, self.EPS2)
setattr(self, 'ECC', ecc)
setattr(self, 'OM', omega)
if hasattr(self, 'PB') and hasattr(self,
'A1') and not hasattr(self, 'ECC'):
setattr(self, 'ECC', 0.0)
pf.close()
