# Fixture to run all tests for both an unmasked (ndarray) and masked
# (MaskedArray) column.
@pytest.fixture(params=[False, True])
def table_type(request):
return MaskedTable if request.param else table.Table
# Stuff for testing mixin columns
MIXIN_COLS = {
'quantity': [0, 1, 2, 3] * u.m,
'longitude':
coordinates.Longitude([0., 1., 5., 6.] * u.deg, wrap_angle=180. * u.deg),
'latitude':
coordinates.Latitude([5., 6., 10., 11.] * u.deg),
'time':
time.Time([2000, 2001, 2002, 2003], format='jyear'),
'timedelta':
time.TimeDelta([1, 2, 3, 4], format='jd'),
'skycoord':
coordinates.SkyCoord(ra=[0, 1, 2, 3] * u.deg, dec=[0, 1, 2, 3] * u.deg),
'sphericalrep':
coordinates.SphericalRepresentation([0, 1, 2, 3] * u.deg,
[0, 1, 2, 3] * u.deg, 1 * u.kpc),
'cartesianrep':
coordinates.CartesianRepresentation([0, 1, 2, 3] * u.pc,
[4, 5, 6, 7] * u.pc,
[9, 8, 8, 6] * u.pc),
'sphericaldiff':
coordinates.SphericalCosLatDifferential([0, 1, 2, 3] * u.mas / u.yr,
import os import pkg_resources import numpy as np import pickle as pkl import astropy.time as at import astropy.coordinates as asc import astropy.units as au import scipy.interpolate as sin """ EarthLocations taken from [email protected]/pulsar_search """ LF1_LAT = asc.Latitude ( "26:33:19.676", unit=au.degree) LF1_LONG = asc.Longitude( "-97:26:31.174",unit=au.degree) LF1_ELVF = ( 10.36 * au.imperial.foot ).to (au.meter) LF2_LAT = asc.Latitude ( "34:4:43.497" , unit=au.degree) LF2_LONG = asc.Longitude( "-107:37:5.819",unit=au.degree) LF2_ELVF = ( 6967.08 * au.imperial.foot ).to (au.meter) LF3_LAT = asc.Latitude ( "38:25:59.0" , unit=au.degree) LF3_LONG = asc.Longitude( "-79:50:23.0", unit=au.degree) LF3_ELVF = ( 2464.89 * au.imperial.foot ).to (au.meter) LF4_LAT = asc.Latitude ( "34:12:3.0" , unit=au.degree) LF4_LONG = asc.Longitude( "-118:10:18.0", unit=au.degree) LF4_ELVF = ( 1167.89 * au.imperial.foot ).to (au.meter) # Earth locations LF1 = asc.EarthLocation (LF1_LONG, LF1_LAT, LF1_ELVF) LF2 = asc.EarthLocation (LF2_LONG, LF2_LAT, LF2_ELVF) LF3 = asc.EarthLocation (LF3_LONG, LF3_LAT, LF3_ELVF) LF4 = asc.EarthLocation (LF4_LONG, LF4_LAT, LF4_ELVF) class LoFASM_Station (object): """Models LoFASM station coordinate systems and stuff"""
mixin_cols = {
'tm': tm,
'tm2': tm2,
'tm3': tm3,
'dt': time.TimeDelta([1, 2] * u.day),
'sc': sc,
'scd': scd,
'scdc': scdc,
'scpm': scpm,
'scpmrv': scpmrv,
'scrv': scrv,
'x': [1, 2] * u.m,
'qdb': [10, 20] * u.dB(u.mW),
'qdex': [4.5, 5.5] * u.dex(u.cm / u.s**2),
'qmag': [21, 22] * u.ABmag,
'lat': coordinates.Latitude([1, 2] * u.deg),
'lon': coordinates.Longitude([1, 2] * u.deg, wrap_angle=180. * u.deg),
'ang': coordinates.Angle([1, 2] * u.deg),
'el': el,
'sr': sr,
'cr': cr,
'sd': sd,
'srd': srd,
'nd': table.NdarrayMixin([1, 2]),
'obj': obj,
'su': su,
'su2': su2,
}
time_attrs = [
'value', 'shape', 'format', 'scale', 'precision', 'in_subfmt',
'out_subfmt', 'location'
import numpy as np
from astropy.time import Time
import astropy.coordinates as coords
import astropy.units as u
import astroplan
P48_loc = coords.EarthLocation(lat=coords.Latitude('33d21m26.35s'),
lon=coords.Longitude('-116d51m32.04s'),
height=1707.)
# use UTC only
P48_Observer = astroplan.Observer(location=P48_loc)
P48_slew_pars = {
'ha': {
'coord': 'ra',
'accel': 0.27 * u.deg * u.second**(-2.),
'decel': 0.27 * u.deg * u.second**(-2.),
'vmax': 1.6 * u.deg / u.second
},
'dec': {
'coord': 'dec',
'accel': 0.2 * u.deg * u.second**(-2.),
'decel': 0.15 * u.deg * u.second**(-2.),
'vmax': 1.2 * u.deg / u.second
},
'dome': {
'coord': 'az',
'accel': 0.17 * u.deg * u.second**(-2.),
'decel': 0.6 * u.deg * u.second**(-2.),
'vmax': 3. * u.deg / u.second
def corrections(lon, lat, alt, ra, dec, mjd):
"""
Calculate the heliocentric radial velocity corrections for an astronomical
source.
:param lon:
Earth longitude of the observatory (western direction is positive). Can
be anything that initialises an `~astropy.coordinates.Angle` object
(if float, in degrees).
:type lon:
:class:`~astropy.coordinates.Longitude` or float
:param lat:
Earth latitude of observatory. Can be anything that initialises an
`~astropy.coordinates.Latitude` object (if float, in degrees).
:type lat:
:class:`~astropy.coordinates.Latitude` or float
:param alt:
Altitude of the observatory (if float, in meters).
:type alt:
:class:`~astropy.units.Quantity` or float
:param ra:
Right ascension of the object for epoch J2000 (if float, in degrees).
:type ra:
:class:`~astropy.coordinates.Angle` or float
:param dec:
Declination of the object for epoch J2000 (if float, in degrees).
:type dec:
:class:`~astropy.coordinates.Angle` or float
:param mjd:
The modified Julian date for the middle of exposure.
:type mjd:
float
:returns:
A two-length tuple containing the barycentric velocity correction and
the heliocentric velocity correction. Both velocity corrections are
given as :class:`~astropy.units.Quantity` objects.
"""
if not isinstance(lon, coord.Longitude):
lon = coord.Longitude(lon * u.deg)
if not isinstance(lat, coord.Latitude):
lat = coord.Latitude(lat * u.deg)
if not isinstance(alt, u.Quantity):
alt *= u.m
if not isinstance(ra, u.Quantity):
ra *= u.deg
if not isinstance(dec, u.Quantity):
dec *= u.deg
# Here we specify the location so that we can easily calculate the mean
# local siderial time later on
time = Time(2.4e6 + mjd, format="jd", location=(lon, lat, alt))
epoch = time.datetime.year + time.datetime.month/12. \
+ time.datetime.day/365.
# Precess the coordinates to the current epoch
coordinate = coord.SkyCoord(ra, dec, frame="fk5").transform_to(
coord.FK5(equinox="J{}".format(epoch)))
# Convert geodetic latitude into geocentric latitude to correct for rotation
# of the Earth
dlat = ((-11. * 60. + 32.743) * np.sin(2 * lat) + 1.1633 * np.sin(4 * lat) \
- 0.0026 * np.sin(6 * lat)) * u.degree
geocentric_lat = lat + dlat / 3600.
# Calculate distance of observer from Earth center
r = alt + 6378160.0 * u.m * (0.998327073 \
+ 0.001676438 * np.cos(2 * geocentric_lat) \
- 0.000003510 * np.cos(4 * geocentric_lat) \
+ 0.000000008 * np.cos(6 * geocentric_lat))
# Calculate rotational velocity perpendicular to the radius vector
# Note: 23.934469591229 is the siderial day in hours for 1986
v = 2 * np.pi * r / (23.934469591229 * 3600 * u.second)
# Calculate vdiurnal velocity
try:
vdiurnal = v * np.cos(lat) * np.cos(coordinate.dec) \
* np.sin(coordinate.ra - time.sidereal_time("mean"))
except:
logging.exception("exception in calculating vdirunal velocity")
# Try again with decreased precision.
time.delta_ut1_utc = 0.0
vdiurnal = v * np.cos(lat) * np.cos(coordinate.dec) \
* np.sin(coordinate.ra - time.sidereal_time("mean"))
logging.warn("Explicitly set delta_ut1_utc = 0")
# Calculate baricentric and heliocentric velocities
vh, vb = celestial_velocities(time)
# Project along the line of sight
projection = np.array([
np.cos(coordinate.dec) * np.cos(coordinate.ra),
np.cos(coordinate.dec) * np.sin(coordinate.ra),
np.sin(coordinate.dec)
])
vbar = (vb * projection).sum()
vhel = (vh * projection).sum()
# Using baricentric velocity for correction
vbar_correction = vdiurnal + vbar
vhel_correction = vdiurnal + vhel
# [TODO] it may be useful to return other components of velocity or extra
# information about the transforms (e.g., gmst, ut, lmst, dlat, lat, vbar,
# vhel, etc)
return (vbar_correction, vhel_correction)
def time_latitude():
coordinates.Latitude(3.2, units.degree)
def helcorr(obs_long,
obs_lat,
obs_alt,
ra2000,
dec2000,
jd,
system="barycentric"):
"""
calculates heliocentric Julian date, barycentric and heliocentric radial
velocity corrections, using astropy functions
Parameters
---------
obs_long : float
Longitude of observatory (degrees, western direction is positive)
obs_lat : float
Latitude of observatory (degrees)
obs_alt : float
Altitude of observatory (meters)
ra2000 : float
Right ascension of object for epoch 2000.0 (hours)
dec2000 : float
Declination of object for epoch 2000.0 (degrees)
jd : float
Julian date for the middle of exposure
system : {"barycentric", "heliocentric"}, optional
reference system of the result, barycentric: around earth-sun gravity center,
heliocentric: around sun, usually barycentric is preferred (default: "barycentric)
Returns
-------
correction : float
radial velocity correction due to barycentre offset
hjd : float
Heliocentric Julian date for middle of exposure
"""
jd = 2400000.0 + jd
jd = time.Time(jd, format="jd")
ra = coord.Longitude(ra2000, unit=u.hour)
dec = coord.Latitude(dec2000, unit=u.degree)
observatory = coord.EarthLocation.from_geodetic(obs_long,
obs_lat,
height=obs_alt)
sky_location = coord.SkyCoord(ra, dec, obstime=jd, location=observatory)
times = time.Time(jd, location=observatory)
if system == "barycentric":
correction = sky_location.radial_velocity_correction().to(u.km /
u.s).value
ltt = times.light_travel_time(sky_location)
elif system == "heliocentric":
correction = (
sky_location.radial_velocity_correction("heliocentric").to(
u.km / u.s).value)
ltt = times.light_travel_time(sky_location, "heliocentric")
else:
raise AttributeError(
"Could not parse system, values are: ('barycentric', 'heliocentric')"
)
times = (times.utc + ltt).value - 2400000
return -correction, times
def stack_plot_phase(spec_list,
period_days,
tasc_mjd=None,
semiamplitude=None,
mean_anomaly=None,
alpha=.7,
yheight=0.1,
xlim=None,
ylim=None,
color=None,
optical_phase=False):
"""Plot several spectra on top of each other with matplotlib.
Consider also iraf.specplot('spec1,spec2,spec3').
Parameters
----------
spec_list : list of strings
List of text or fits spectra extracted by extract1D
(e.g., ['red0001_flux.spec.txt',red0002_flux.spec.fits'])
alpha : float, default 1.0
Opacity of the plot lines
yheight : float, default 0.1
Proportion of phase 0-1 to scale the range of each spectrum to.
optical_phase : boolean, default False
if False, use TASC as phase zero point; else use TASC-0.25
"""
category20 = N.array([
'#1f77b4', '#aec7e8', '#ff7f0e', '#ffbb78', '#2ca02c', '#98df8a',
'#d62728', '#ff9896', '#9467bd', '#c5b0d5', '#8c564b', '#c49c94',
'#e377c2', '#f7b6d2', '#7f7f7f', '#c7c7c7', '#bcbd22', '#dbdb8d',
'#17becf', '#9edae5'
])
sb.set_style('white')
# sb.set_palette(sb.dark_palette(color, n_colors = len(spec_list)),
# n_colors=len(spec_list))
mpl.rcParams['xtick.labelsize'] = 14
mpl.rcParams['ytick.labelsize'] = 14
mpl.rcParams['axes.labelsize'] = 16
mpl.rcParams['font.size'] = 16
mpl.rcParams['legend.fontsize'] = 14
atm_bands = [
[6701, 6715], # dome overhead lamp flourescence feature
[6860, 7000],
[7570, 7700],
[7150, 7350],
[8100, 8401]
] # trim a funky bin with +1
def exclude_bands(wave, bands):
winband = N.zeros(len(wave)).astype(N.bool)
for band in bands:
winband |= ((wave >= band[0]) & (wave <= band[1]))
#woutband = ~winband
return winband
phases = []
xs = []
ys = []
labels = []
mjds = []
for spec in spec_list:
if spec.endswith('txt'):
dat = N.genfromtxt(spec, names='wave, flux', dtype='f4, f4')
raise ValueError('Need fits spectra')
elif spec.endswith('fits'):
hdulist = pyfits.open(spec)
hdr = hdulist[0].header
flux = hdulist[0].data
crpix1 = hdr['CRPIX1']
crval1 = hdr['CRVAL1']
cd1_1 = hdr['CDELT1']
mjd = hdr['MJD']
spec_length = len(flux)
wave = cd1_1 * (N.arange(spec_length) - (crpix1 - 1)) + crval1
dat = {'wave': wave, 'flux': flux}
P200_loc = coord.EarthLocation(lat=coord.Latitude('33d21m21.6s'),
lon=coord.Longitude('-116d51m46.80s'),
height=1706.)
t = BaryTime(mjd, format='mjd', scale='utc', location=P200_loc)
PSR_coords = coord.SkyCoord(322.43776,
-4.48521,
frame='icrs',
unit=u.deg)
bjd_tdb = t.bcor(PSR_coords).mjd
phase = mjd_to_phase(bjd_tdb, period_days, tasc_mjd=tasc_mjd)[0]
# for j2129: convert to optical phase convention
tasc_phase = phase
if optical_phase:
phase = (phase - 0.25) % 1
if xlim is None:
wmin = 0
else:
wmin = N.nonzero(wave > xlim[0])[0][0]
offset_val = N.median(dat['flux'][wmin:wmin + 100])
pct = N.percentile(dat['flux'], [5, 95])
scale_val = yheight / (pct[1] - pct[0])
w = exclude_bands(wave, atm_bands)
dat['flux'][w] = N.NaN
# correct for the binary shift
if (semiamplitude is not None) and (mean_anomaly is not None):
predicted_shift = mean_anomaly - semiamplitude * \
N.cos(2.*N.pi * tasc_phase)
# delta_lambda/lambda_emitted = v/c in nonrel. case
# so lambda_emitted = lambda_obs/ (1+v/c)
dat['wave'] = dat['wave'] / (1 + predicted_shift / 299792.458)
mjds.append(mjd)
phases.append(phase)
xs.append(dat['wave'])
ys.append((dat['flux'] - offset_val) * scale_val + phase)
labels.append(spec)
mjds_set = N.sort(N.unique(N.floor(mjds)))
assert (len(mjds_set) < len(category20))
if color is None:
colors = category20[[
N.where(mjds_set == N.floor(mi))[0][0] for mi in mjds
]]
else:
colors = [color for mi in mjds]
fig = plt.figure(figsize=(20, 8))
ax = plt.subplot(111)
args = N.argsort(phases)
for i in args:
print(labels[i], phases[i])
plt.plot(xs[i],
ys[i],
label=labels[i],
alpha=alpha,
linewidth=1.,
color=colors[i])
plt.xlabel("Wavelength (Angstrom)")
plt.ylabel("Orbital Phase (cycles)")
if xlim is not None:
plt.xlim(xlim)
if ylim is not None:
plt.ylim(ylim)
#plt.legend()
sb.despine()
plt.show()
return ax
def correct_rvs_homebrew(savfile='bestfitvels.sav',
outfile='test_rv_vlsr.txt',
observatory='Palomar'):
"""take output of getvel.pro and correct to solar system barycenter
requires all observations to come from the same observatory"""
sav = readsav(savfile, python_dict=True)
minchi2 = sav['minchi2fit']
fitvels = sav['fitvels']
velerrs = sav['velerrs']
exptimes = sav['exptime']
if len(minchi2.shape) == 2:
(ntemplates, nobs) = minchi2.shape
wbest = minchi2.argmin(axis=0)
best_vel = fitvels[wbest, N.arange(nobs)]
best_err = velerrs[wbest, N.arange(nobs)]
else:
nobs = minchi2.shape[0]
ntemplates = 1
best_vel = fitvels
best_err = velerrs
#intermediate_file = 'rv.obs'
#f = open(intermediate_file,'w')
f = open(outfile, 'w')
f.write("# BJD_TDB EXPTIME VLSR VERR VSYS\n")
sys_errs = []
for i, obsfile in enumerate(sav['observations'].tolist()):
velocity = best_vel[i]
if observatory == 'Palomar':
# DBSP spectra reduced by my pipeline
hdulist = pyfits.open(obsfile + '.spec.fits')
hdr = hdulist[0].header
ra = hdr['RA']
dec = hdr['DEC']
sys_velerr = hdr[
'VERR'] # velocity error do to wavelength uncertainty
sys_errs.append(sys_velerr)
obs_mid = find_midpoint_time(hdr)
tel_loc = coord.EarthLocation(
lat=coord.Latitude('33d21m21.6s'),
lon=coord.Longitude('-116d51m46.80s'),
height=1706.)
t = BaryTime(obs_mid,
format='datetime',
scale='utc',
location=tel_loc)
elif observatory == 'Keck':
# LRIS spectra reducd by Dan Perley's pipeline
sys_errs.append(0.)
rahms = get_dperley_header(obsfile + '.spec',
'RA').strip().strip("'")
decdms = get_dperley_header(obsfile + '.spec',
'DEC').strip().strip("'")
c = coord.SkyCoord(ra=rahms, dec=decdms, unit=(u.hourangle, u.deg))
ra = c.ra.value
dec = c.dec.value
exptime = get_dperley_header(
obsfile + '.spec', 'EXPTIME', converter=N.float) * u.second
mjd = get_dperley_header(
obsfile + '.spec', 'MJD-OBS', converter=N.float) * u.day
tel_loc = coord.EarthLocation(
lat=coord.Latitude('19d49m34.9s'),
lon=coord.Longitude('-155d28m30.04s'),
height=4145.)
t = BaryTime(mjd + exptime / 2.,
format='mjd',
scale='utc',
location=tel_loc)
else:
raise NotImplementedError(
'Observatory {} not implemented'.format(observatory))
PSR_coords = coord.SkyCoord(ra, dec, frame='icrs', unit=u.deg)
(h_pos, h_vel, b_pos, b_vel) = t._obs_pos()
m, vect = t._vect(PSR_coords)
v_corr = (b_vel.dot(vect) * const.au / (1 * u.day)).to(u.km / u.s)
bjd_tdb = t.bcor(PSR_coords).jd
f.write('{} {} {} {:.2f} {}\n'.format(bjd_tdb[0], exptimes[i],
best_vel[i] + v_corr.value[0],
best_err[i], sys_errs[i]))
f.close()