def run(mk, time_start='', time_finish='', step=60, target='MERCURY',
frame='', sensor='MPO_MERTIS_TIR_PLANET', pixel_line='',
pixel_sample='', observer='MPO'):
spiceypy.furnsh(mk)
target = target.upper()
if not time_start: time_start = datetime.datetime.now().strftime('%Y-%m-%dT%H:%M:%S')
if not frame: frame = f'IAU_{target}'
if not time_finish: time_finish = time_start
if not pixel_sample: pixel_sample = np.floor(ccd_center(sensor)[0])
if not pixel_line: pixel_line = np.floor(ccd_center(sensor)[1])
if pixel_sample == 'all':
pixel_sample = np.arange(1, pixel_samples(sensor), 1)
else:
pixel_sample = [pixel_sample]
if pixel_line == 'all':
pixel_line = np.arange(1, pixel_lines(sensor), 1)
else:
pixel_line = [pixel_line]
et_start = spiceypy.utc2et(time_start)
et_finish = spiceypy.utc2et(time_finish)
if et_start != et_finish:
interval = np.arange(et_start, et_finish, step)
else:
interval = [et_start]
# Time tag [UTC]
# pixel id [(x,y)]
# corner id [(x,y)]
# Requested geometry
# lat lon intersection (planetocentric)
# lat lon subspacecraft
# lat lon subsolar
# target distance intersection
# target angular diameter
# local solar time intersection
# phase angle intersection
# emission angle intersection
# incidence angle intersection
with open('spice4mertis.csv', 'w') as o:
o.write('utc,et,pixlin,pixsam,tarlon,tarlat,sublon,sublat,sunlon,sunlat,tardis,tarang,ltime,phase,emissn,incdnc\n')
for et in interval:
utc = spiceypy.et2utc(et, 'ISOC', 3)
for line in pixel_line:
for sample in pixel_sample:
pixelGeometry = pixel_geometry(et, sensor, line, sample, target, frame, observer=observer)
print(utc,line,sample,str(pixelGeometry)[1:-1].replace(',',' '))
o.write(f'{utc},{et},{line},{sample},{str(pixelGeometry)[1:-1].replace(" ","")}\n')
return
def analyseLineScan2(hdf5Files, hdf5Filenames):
# referenceFrame = "TGO_NOMAD_UVIS_OCC"
referenceFrame = "TGO_NOMAD_SO"
# referenceFrame = "TGO_SPACECRAFT"
fig, ax = plt.subplots(figsize=(FIG_X, FIG_Y))
for fileIndex, hdf5File in enumerate(hdf5Files):
print("Reading in file %i: %s" % (fileIndex + 1, obspaths[fileIndex]))
detectorDataAll = hdf5File["Science/Y"][:, :]
# binsAll = get_dataset_contents(hdf5File, "Bins")[0]
observationTimeStringsAll = hdf5File[
"Geometry/ObservationDateTime"][:, :]
centrePixelIndex = 200
detectorDataBin1 = detectorDataAll[:, 1, centrePixelIndex].flatten()
detectorDataBin2 = detectorDataAll[:, 2, centrePixelIndex].flatten()
detectorDataCentrePixel = np.mean((detectorDataBin1, detectorDataBin2),
axis=0)
print(
"max value = %0.0f, min value = %0.0f" %
(np.max(detectorDataCentrePixel), np.min(detectorDataCentrePixel)))
observationTimes = np.asfarray([
np.mean([sp.utc2et(time[0]),
sp.utc2et(time[1])])
for time in list(observationTimeStringsAll)
])
unitVectors = np.asfarray([
get_vector(datetime, referenceFrame)
for datetime in observationTimes
])
# marker_colour = np.log(detectorDataCentrePixel+1000).flatten()
marker_colour = np.log(detectorDataCentrePixel.flatten())
ax.set_xlim([-0.004, 0.004])
ax.set_ylim([-0.004, 0.004])
ax.set_xlabel("%s FRAME X" % referenceFrame)
ax.set_ylabel("%s FRAME Y" % referenceFrame)
ax.scatter(unitVectors[:, 0],
unitVectors[:, 1],
c=marker_colour,
vmin=np.log(200000),
alpha=0.5,
cmap="jet",
linewidths=0)
ax.set_aspect("equal")
circle1 = plt.Circle((0, 0), 0.0016, color='yellow', alpha=0.1)
ax.add_artist(circle1)
def plotBinStrengths(hdf5Files, hdf5Filenames, obspaths):
et_string_all = []
max_counts_all = []
relative_counts_all = []
for fileIndex, (hdf5File,
hdf5Filename) in enumerate(zip(hdf5Files, hdf5Filenames)):
print("%i/%i: Reading in file %s" %
(fileIndex, len(hdf5Filenames), hdf5Filename))
# et, et_string, max_counts, relative_counts = getOccultationReferenceCounts(hdf5File, hdf5Filename, 17859.0)
et_string, max_counts, relative_counts = getOccultationReferenceCounts(
hdf5File)
if len(relative_counts) == 4: #just take nominal 6 order data
et_string_all.append(et_string)
max_counts_all.append(max_counts)
relative_counts_all.append(relative_counts)
if np.min(relative_counts) < 0.9:
print(
"File %s has minimum relative counts of %0.2f (max counts = %0.0f)"
% (hdf5Filename, np.min(relative_counts), max_counts))
relative_counts_array = np.asfarray(relative_counts_all)
et_array = np.asfarray([sp.utc2et(string) for string in et_string_all])
fig, ax = plt.subplots(figsize=(15, 5))
plt.title("SO channel relative counts for each bin\nSearch string: %s" %
obspaths[0])
for bin_index in range(4):
plt.scatter(et_array,
relative_counts_array[:, bin_index],
label="Bin %i" % bin_index,
marker=".")
plt.xlabel("Ephemeris Time (s)")
plt.ylabel("Relative counts for each bin")
plt.legend()
plt.grid(True)
months = np.arange(4, 13, 1)
monthStarts = [
sp.utc2et(datetime(2018, month, 1).strftime("%Y-%m-%d"))
for month in months
]
monthNames = [datetime(2018, month, 1).strftime("%B") for month in months]
for monthStart, monthName in zip(monthStarts, monthNames):
plt.axvline(x=monthStart, color='k', linestyle='--')
plt.text(monthStart + 100000, 0.7, monthName)
def ephemeris_start_time(self):
inital_time = spice.utc2et(self.utc_start_time.isoformat())
# To get shutter end (close) time, subtract 2 seconds from the start time
updated_time = inital_time - 2
# To get shutter start (open) time, take off the exposure duration from the end time.
start_time = updated_time - self.exposure_duration
return start_time
def test_hga_angles():
spiops.load('/Users/mcosta/SPICE/BEPICOLOMBO/kernels/mk/bc_ops_local.tm')
(hga_az_el,
hga_earth) = spiops.hga_angles('MPO',
spiceypy.utc2et('2020-05-07T006:00:00'))
print(hga_az_el)
def jd2et(jd):
"""Convert Julian date to SPICE ephemeris time.
Ephemeris time is seconds past 2000.0.
UTC is assumed.
Parameters
----------
jd : string, float, or array
The Julian date. Strings will have higher precisions than
floats.
Returns
-------
et : float or array
Ephemeris time.
"""
global _spice_setup
if not _spice_setup:
_setup_spice()
if isinstance(jd, (list, tuple, np.ndarray)):
return [jd2et(x) for x in jd]
if isinstance(jd, float):
jd = "{:17.9f} JD".format(jd)
return spice.utc2et(jd)
def time2et(t):
"""Convert astropy `Time` to SPICE ephemeris time.
Ephemeris time is seconds past 2000.0.
Parameters
----------
t : astropy Time
The time. Must be convertable to the UTC scale.
Returns
-------
et : float or array
Ephemeris time.
"""
global _spice_setup
from .. import util
if not _spice_setup:
_setup_spice()
if util.date_len(t) > 0:
return [time2et(x) for x in t]
return spice.utc2et(t.utc.iso)
def __init__(self, file):
# Get the speed relative to MU69
file_tm = 'kernels_kem_prime.tm'
# Start up SPICE if needed
if (sp.ktotal('ALL') == 0):
sp.furnsh(file_tm)
utc_ca = '2019 1 Jan 05:33:00'
et_ca = sp.utc2et(utc_ca)
(st,lt) = sp.spkezr('New Horizons', et_ca, 'J2000', 'LT', 'MU69')
velocity = sp.vnorm(st[3:6])*u.km/u.s
# Save the velocity (relative to MU69)
self.velocity = velocity
# Save the name of file to read
self.file = file
# Save the area of the s/c
self.area_sc = (1*u.m)**2
return
def f_convert_utc_to_et(time_utc):
#Convert datetime object to str
time_utc_str = time_utc.strftime('%Y-%m-%dT%H:%M:%S')
#Convert UTC to ET
time_et = spiceypy.utc2et(time_utc_str)
return (time_et, time_utc_str)
def check(mk, time=False, report=False):
frames_to_check = False
if not time:
today = datetime.datetime.now()
time = today.strftime("%Y-%m-%dT%H:%M:%S")
frame_dict = gen_frame_dict(mk, report=report)
spiceypy.furnsh(mk)
et = spiceypy.utc2et(time)
for key in frame_dict.keys():
if frame_dict[key]['class'] == 4:
fname = frame_dict[key]['name']
try:
spiceypy.pxform(fname, 'J2000', et)
except SpiceyError:
frames_to_check = True
print( f'Frame {fname} not properly defined at {time}\n' +
f' NAME: {frame_dict[key]["name"]}\n' +
f' CLASS: {frame_dict[key]["class"]}\n' +
f' ID: {frame_dict[key]["id"]}\n' +
f' CENTER: {frame_dict[key]["center"]}\n' +
f' RELATIVE: {frame_dict[key]["relative"]}\n'
)
pass
spiceypy.kclear()
if not frames_to_check:
print(f'All {len(frame_dict)} frames are correct @ {time}')
return
def cal2et(date):
"""Convert calendar date to SPICE ephemeris time.
Ephemeris time is seconds past 2000.0.
UTC is assumed.
Parameters
----------
date : string or array
The date.
Returns
-------
et : float or array
Ephemeris time.
"""
from ..util import cal2iso
global _spice_setup
if not _spice_setup:
_setup_spice()
if isinstance(date, (list, tuple, np.ndarray)):
return [cal2et(x) for x in t]
return spice.utc2et(cal2iso(date))
def dataToPickle():
orbits_begin = {1:'2016-07-31T19:46:02',
2:'2016-09-23T03:44:48',
3:'2016-11-15T05:36:45',
4:'2017-01-07T03:11:30',
5:'2017-02-28T22:55:48',
6:'2017-04-22T19:14:57'}
file_dict = {}
metaKernel = 'juno_2019_v03.tm'
spice.furnsh(metaKernel)
start_time = datetime.datetime.strptime(orbits_begin[1],'%Y-%m-%dT%H:%M:%S')
end_time = datetime.datetime.strptime(orbits_begin[2],'%Y-%m-%dT%H:%M:%S')
data_folder = pathlib.Path(r'..\data\fgm')
p = re.compile(r'\d{7}')
for parent,child,files in os.walk(data_folder):
for name in files:
if name.endswith('.csv'):
file_path = os.path.join(data_folder,name)
search = p.search(name).group()
date = datetime.datetime.strptime(search,'%Y%j')
if date.date() >= start_time.date() and date.date() <= end_time.date():
iso_date = date.strftime('%Y-%m-%d')
if iso_date not in file_dict.keys():
file_dict[iso_date] = [file_path]
elif iso_date in file_dict.keys() and file_dict[iso_date] != file_path:
file_dict[iso_date].append(file_path)
for date in file_dict.keys():
fgmdf = pd.DataFrame(data={'TIME':[],'BX':[],'BY':[],'BZ':[],'LAT':[]})
save_date = datetime.datetime.strptime(date,'%Y-%m-%d')
file_list = file_dict[date]
for file in file_list:
temp = pd.read_csv(file)
datetime_list = temp['SAMPLE UTC']
time_list = [datetime.datetime.fromisoformat(i).strftime('%H:%M:%S') for i in datetime_list]
for index,time in enumerate(datetime_list):
position, lighttime = spice.spkpos('JUNO',spice.utc2et(time),'IAU_JUPITER','NONE','JUPITER')
vectorPos = spice.vpack(position[0],position[1],position[2])
radii,longitude,latitude = spice.reclat(vectorPos)
lat = latitude*spice.dpr()
if lat >= -10 and lat <= 10:
fgmdf = fgmdf.append({'TIME':time,'BX':temp['BX PLANETOCENTRIC'][index],'BY':temp['BY PLANETOCENTRIC'][index],'BZ':temp['BZ PLANETOCENTRIC'][index],'LAT':lat},ignore_index=True)
fgmdf = fgmdf.sort_values(by=['TIME'])
save_name = f'{save_date.strftime("%Y%m%d")}'
save_path = pathlib.Path(f'..\data\pickledfgm\jno_fgm_{save_name}.pkl')
pickledf = fgmdf.to_pickle(save_path)
print(f'Saved pickle {date}')
def cspice_utc2et(kernelfile, ctime):
spice_ver = spice.tkvrsn('TOOLKIT')
spice.furnsh(kernelfile)
kernels_loaded = spice.ktotal("ALL")
#print(kernels_loaded)
ntime = spice.utc2et(ctime.value)
#print(spice_ver)
return ntime
def cspice_utc2et(kernelfile, stimes, ttimes):
global ets, etx
nt = len(stimes)
ets = np.zeros(nt)
etx = np.zeros(nt)
spice_ver = spice.tkvrsn('TOOLKIT')
spice.furnsh(kernelfile)
kernels_loaded = spice.ktotal("ALL")
#print(kernels_loaded)
for i in range(0, nt):
sstr = stimes[i][:23]
tstr = ttimes[i][:23]
et1 = spice.utc2et(sstr)
et2 = spice.utc2et(tstr)
ets[i] = 0.5 * (et1 + et2)
for i in range(0, nt):
etx[i] = ets[i] - ets[0]
def cal2et(time, format='UTC', support_ker=False, unload=False):
"""
Converts UTC or Calendar TDB (CAL) time to Ephemeris Time (ET). Accepts
a single time or a lists of times. This function assumes that the support
kernels (meta-kernel or leapseconds) kernel has been loaded.
:param time: Input UTC or CAL time
:type time: Union[float, list]
:param format: Input format; 'UTC' or 'CAL'
:type format: str
:param unload: If True it will unload the input meta-kernel
:type unload: bool
:return: Output ET
:rtype: Union[str, list]
"""
out_list = []
if isinstance(time, str):
time = [time]
#
# We need to specify that is Calendar format in TDB. If it is UTC we need
# to load the support kernels
#
if support_ker:
spiceypy.furnsh(support_ker)
if format == 'CAL':
time[:] = [x.replace('T', ' ') for x in time]
time[:] = [x + ' TDB' for x in time]
for element in time:
try:
if format == 'UTC':
out_elm = spiceypy.utc2et(element)
elif format == 'CAL':
out_elm = spiceypy.str2et(element)
else:
out_elm = element
except:
out_elm = spiceypy.str2et(element)
out_list.append(out_elm)
if len(out_list) == 1:
out_time = out_list[0]
else:
out_time = out_list
if unload:
spiceypy.unload(support_ker)
return out_time
def test_Satellite_B():
"""Test that a Satellite-object correctly calculates internal epochs (consistent with sp.utc2et() )"""
# Make a Satellite-object and get the epochs
time = Time([2458337.8283571, 2458337.9], format='jd', scale='tdb')
obscode = '-95'
returnedEpochs = wis.Satellite(obscode, time).epochs
# Check epoch calcs are correct
for i, jd in enumerate(time.utc.jd):
assert returnedEpochs[i] == sp.utc2et('JD'+str(jd)), \
'Returned epoch [%r] does not match calculation from spiceypy [%r]' % (returnedEpochs[i] , jd)
def get_psp_positions(from_days, to_days, step=24):
now = datetime.now()
coords = list()
for i in range(from_days * 24, to_days * 24, step):
tspy = (now + timedelta(hours=i)).strftime('%Y-%m-%dT%H:%M:%S')
ts = spice.utc2et(tspy)
# -96 is the ID of PSP
pos, lt = spice.spkezp(-96, ts, 'ECLIPJ2000', 'NONE', 0)
x, y, z = pos
coords.append([x, y, z])
return f2i(coords)
def generateEphemeris(datesFile, bsp, dexxx, leapSec, nameFile):
#Load the asteroid and planetary ephemeris and the leap second (in order)
spice.furnsh(dexxx)
spice.furnsh(leapSec)
spice.furnsh(bsp)
#Values specific for extract all comments of header from bsp files (JPL, NIMA)
source = {'NIMA':(45, 'ASTEROID_SPK_ID ='), 'JPL':(74, 'Target SPK ID :')}
n, key = source['NIMA']
idspk = findIDSPK(n, key)
if idspk == '':
n, key = source['JPL']
idspk = findIDSPK(n, key)
#Read the file with dates
with open(datesFile, 'r') as inFile:
dates = inFile.read().splitlines()
n = len(dates)
#Convert dates from utc to et format
datesET = [spice.utc2et(utc) for utc in dates]
#Compute geocentric positions (x,y,z) for each date with light time correction
rAst, ltAst = spice.spkpos(idspk, datesET, 'J2000', 'LT', 'EARTH')
rSun, ltSun = spice.spkpos('SUN', datesET, 'J2000', 'NONE', 'EARTH')
elongation = [angle(rAst[i], rSun[i]) for i in range(n)]
data = [spice.recrad(xyz) for xyz in rAst]
distance, rarad, decrad = zip(*data)
#================= for graphics =================
tempFile = open('radec.txt', 'w')
for row in data:
tempFile.write(str(row[1]) + ' ' + str(row[2]) + '\n')
tempFile.close()
#================================================
ra = [ra2HMS(alpha) for alpha in rarad]
dec = [dec2DMS(delta) for delta in decrad]
#Convert cartesian to angular coordinates and save it in a ascii file
outFile = open(nameFile,'w')
outFile.write('\n\n Data Cal. UTC' + ' '.ljust(51) + 'R.A.__(ICRF//J2000.0)__DEC')
outFile.write(' '.ljust(43) + 'DIST (km)' + ' '.ljust(24) + 'S-O-A\n')
for i in range(n):
outFile.write(dates[i] + ' '.ljust(44) + ra[i] + ' ' + dec[i] + ' '.ljust(35))
outFile.write('{:.16E}'.format(distance[i]) + ' '.ljust(17))
outFile.write('{:.4f}'.format(elongation[i]) + '\n')
outFile.close()
def utc2obt(self, utc_string):
# Utc to Ephemeris time (seconds past J2000)
ephemeris_time = spiceypy.utc2et(utc_string)
# Ephemeris time to Obt
#return ephemeris_time
obt_string = spiceypy.sce2s(self.solar_orbiter_naif_id, ephemeris_time)
time_fields = re.search('\/(.*?):(\d*)', obt_string)
group = time_fields.groups()
try:
return int(group[0]) + int(group[1]) / 65536.
except Exception as e:
#logger.warning(str(e))
return 0
def getPosLabels(dataDict, num):
stamp = str(dataDict['DATETIME_ARRAY'][min(
range(len(dataDict['TIME_ARRAY'])),
key=lambda j: abs(dataDict['TIME_ARRAY'][j] - num))])
position, lighttime = spice.spkpos('JUNO', spice.utc2et(stamp),
'IAU_JUPITER', 'NONE', 'JUPITER')
vectorPos = spice.vpack(position[0], position[1], position[2])
radii, longitude, latitude = spice.reclat(vectorPos)
lat = f'{round(latitude*spice.dpr(),2)}$^o$ Lat'
dist = f'{round(radii/69911,3)} $R_j$'
return lat, dist
def create_targets_file(name, dates, bsp_object, bsp_planets, leap_Sec,
location):
# Load the asteroid and planetary ephemeris and the leap second (in order)
spice.furnsh(bsp_planets)
spice.furnsh(leap_Sec)
spice.furnsh(bsp_object)
# Values specific for extract all comments of header from bsp files (JPL, NIMA)
source = {
'NIMA': (45, 'ASTEROID_SPK_ID ='),
'JPL': (74, 'Target SPK ID :')
}
n, key = source['NIMA']
idspk = findIDSPK(n, key)
if idspk == '':
n, key = source['JPL']
idspk = findIDSPK(n, key)
# Convert dates from JD to et format. "JD" is added due to spice requirement
datesET = [spice.utc2et(jd + " JD") for jd in dates]
# Compute geocentric positions (x,y,z) for each date with light time correction
rAst, ltAst = spice.spkpos(idspk, datesET, 'J2000', 'LT', 'EARTH')
# Location
lon, lat, ele = location[0], location[1], location[2]
# Create targets file
output = os.path.join(os.getenv("DATA_DIR"), targets_file)
with open(output, 'w') as outFile:
for i, r_geo in enumerate(rAst):
# Convert from longitude, latitude, elevation to r(x,y,z)
r = geoTopoVector(lon, lat, ele, float(dates[i]))
#r_topo = r_geo - r
r_topo = [r_geo[0] - r[0], r_geo[1] - r[1], r_geo[2] - r[2]]
# Convert rectangular coordinates (x,y,z) to range, right ascension, and declination.
d, rarad, decrad = spice.recrad(r_topo)
# Transform RA and Decl. from radians to degrees and then to hexadecimal format.
ra = ra2HMS(np.degrees(rarad) / 15.0, 6)
dec = dec2DMS(np.degrees(decrad), 5)
# Save parameters in specific format
outFile.write(" " + ra + " " + dec + " " + dates[i] + " " + name +
"\n")
outFile.close()
return output
def utc2tai(utc, utc_end, deltat):
if utc_end is None:
utc_end = utc
if deltat is None:
deltat = 86400
if deltat <= 0:
utc_end = utc
deltat = 1
try:
tai_beg = sp.unitim(sp.utc2et(utc), 'et', 'tai')
tai_end = sp.unitim(sp.utc2et(utc_end), 'et', 'tai')
except sp.stypes.SpiceyError as ex:
raise GeometrySpiceError(ex.value)
tais = []
while tai_beg <= tai_end and len(tais) < 1e6:
tais.append(tai_beg)
tai_beg += deltat
return tais
def positionData(self):
# spice.furnsh(self.meta) #loads the meta kernel that will load all kernels needed
time = spice.utc2et(self.time)
self.position, lighttime = spice.spkpos(
'JUNO', time, 'IAU_JUPITER', 'NONE', 'JUPITER'
) #Finds the position in cartesian coords relative to jupiter
pos = spice.vpack(self.position[0], self.position[1],
self.position[2]) #Packs the position into a vector
self.distance, self.longitude, self.latitude = spice.reclat(
pos) #Finds radial dist, latitide and longitude
self.latitude *= spice.dpr()
self.distance /= 69911
def ephemeris_start_time(self):
"""
Returns the ephemeris_start_time of the image.
Expects spacecraft_clock_start_count to be defined. This should be a float
containing the start clock count of the spacecraft.
Expects spacecraft_id to be defined. This should be the integer Naif ID code
for the spacecraft.
Returns
-------
: float
ephemeris start time of the image.
"""
return spice.utc2et(
self.utc_start_time.strftime("%Y-%m-%d %H:%M:%S.%f"))
def ephemeris_start_time(self):
"""
Returns the ephemeris_start_time of the image.
Expects spacecraft_clock_start_count to be defined. This should be a float
containing the start clock count of the spacecraft.
Expects spacecraft_id to be defined. This should be the integer Naif ID code
for the spacecraft.
Returns
-------
: float
ephemeris start time of the image.
"""
return spice.utc2et(
str(self.label['IsisCube']['Instrument']['StartTime']))
def printBoresights(angleSeparationA, angleSeparationB):
"""input manual rotation angles from SPICE kernels to calculate new and old boresight"""
oldSoBoresight = [0.0, 0.0, 1.0]
oldUVISBoresight = [0.0, 0.0, 1.0]
rotationMatrixSoUVIS = sp.pxform("TGO_NOMAD_SO", "TGO_NOMAD_UVIS_OCC",
sp.utc2et("2018 APR 01 00:00:00 UTC"))
oldSoBoresightUVIS = np.dot(oldSoBoresight, rotationMatrixSoUVIS.T)
oldBoresightSeparation = sp.vsep(oldUVISBoresight,
oldSoBoresightUVIS) * sp.dpr() * 60.0
print("oldBoresightSeparation")
print(oldBoresightSeparation)
print("angleSeparationB")
print(angleSeparationB)
#####SAVE THIS IT WORKS!!!######
newSoBoresightTGO = np.asfarray([
-1.0 * np.sin(angleSeparationB / sp.dpr()), \
np.sin(angleSeparationA / sp.dpr()) * np.cos(angleSeparationB / sp.dpr()), \
np.cos(angleSeparationA / sp.dpr()) * np.cos(angleSeparationB / sp.dpr())])
print("newSoBoresightTGO, vnorm = %0.6f" % sp.vnorm(newSoBoresightTGO))
print(newSoBoresightTGO)
newUVISBoresightTGO = np.asfarray(
[-0.922221097920913, -0.386613383297695, 0.006207330031467])
oldSoBoresightTGO = np.asfarray([-0.92156, -0.38819, 0.00618])
oldUVISBoresightTGO = np.asfarray(
[-0.92207347097, -0.3869614566418, 0.0064300242046])
oldNewSoBoresightSeparation = sp.vsep(newSoBoresightTGO,
oldSoBoresightTGO) * sp.dpr() * 60.0
print("oldNewSoBoresightSeparation")
print(oldNewSoBoresightSeparation)
oldNewUVISBoresightSeparation = sp.vsep(
newUVISBoresightTGO, oldUVISBoresightTGO) * sp.dpr() * 60.0
print("oldNewUVISBoresightSeparation")
print(oldNewUVISBoresightSeparation)
newSoUVISBoresightSeparation = sp.vsep(
newSoBoresightTGO, newUVISBoresightTGO) * sp.dpr() * 60.0
print("newSoUVISBoresightSeparation")
print(newSoUVISBoresightSeparation)
oldSoUVISBoresightSeparation = sp.vsep(
oldSoBoresightTGO, oldUVISBoresightTGO) * sp.dpr() * 60.0
print("oldSoUVISBoresightSeparation")
print(oldSoUVISBoresightSeparation)
def exact_leap_tests():
''' Tests time tick conversion for leap second values '''
epoch_lst = ['Y1966', 'Y1970', 'Y2000', 'J2000']
leap_dates = [datetime(1974, 1, 1), datetime(2006, 1, 1), datetime(2009, 1, 1)]
# Y1966 should not treat leap seconds differently
leap_tick = ff_time.date_to_tick(leap_dates[0], 'Y1966')
dates, leaps = ff_time.ticks_to_dates([leap_tick], 'Y1966')
assert(dates[0] == leap_dates[0])
assert(len(leaps) == 0)
# Test Y1970 epoch against exact leap seconds
for leap_date in leap_dates:
leap_tick = ff_time.date_to_tick(leap_date, 'Y1970')
dates, leaps = ff_time.ticks_to_dates([leap_tick-1, leap_tick], 'Y1970')
assert(len(leaps) == 1)
assert(dates[1] == leap_date)
# Test leap second values for 2000 epochs
# for epoch in ['Y2000', 'J2000']:
# for leap_date in leap_dates:
# leap_tick = ff_time.date_to_tick(leap_date, epoch)
# dates, leaps = ff_time.ticks_to_dates([leap_tick - 1, leap_tick], epoch)
# print (dates)
# # Only one leap second found, leap date = previous second,
# # and first date = last date (expected behavior)
# assert(len(leaps) == 1)
# assert(dates[0] == leap_date - timedelta(seconds=1))
# assert(dates[1] == leap_date)
# Test J2000 leap second dates against CSPICE epoch values
epoch = 'J2000'
for leap_date in leap_dates:
leap_tick = ff_time.date_to_tick(leap_date, epoch)
# Get fftime and CSPICE conversions
ts = leap_date.strftime('%Y %j %b %d %H:%M:%S.%f')
fftime_tick = FFTIME(ts, Epoch=epoch)._tick
spice_tick = spice.utc2et(leap_date.isoformat())
# Check that spice tick and fftime_tick are close
# (subtracting ofst_delta beforehand since epochs
# are defined differently)
comp = fftime_tick - ofst_delta
assert(np.isclose(comp, spice_tick, 0.1))
def getHdf5DetectorTemperature(hdf5File, obspath, channel):
print("Reading in file %s" %(obspath))
if channel == "so":
temperature_field = "FPA1_FULL_SCALE_TEMP_SO"
start_index = 1
end_index = 590
elif channel == "lno":
temperature_field = "FPA1_FULL_SCALE_TEMP_LNO"
start_index = 1
end_index = 40
hsk_time_strings = hdf5File["Housekeeping/DateTime"][start_index:end_index]
variable = hdf5File["Housekeeping/%s" %temperature_field][start_index:end_index]
hsk_time = [sp.utc2et(hsk_time_string) for hsk_time_string in hsk_time_strings]
return hsk_time, variable
def print_state(epoch):
et = sp.utc2et(epoch)
print()
print(epoch, et)
sc_from_moon = sp.spkez(-10003001, et, 'j2000', 'none', 301)[0]
print("Moon J2000", sc_from_moon)
sc_from_earth = sp.spkez(-10003001, et, 'j2000', 'none', 399)[0]
print("EME2000", sc_from_earth)
moon_from_earth = sp.spkez(301, et, 'j2000', 'none', 399)[0]
print("Moon from Earth:", moon_from_earth)
moon_from_emb = sp.spkez(301, et, 'j2000', 'none', 3)[0]
print("Moon from EMB:", moon_from_emb)
earth_from_emb = sp.spkez(399, et, 'j2000', 'none', 3)[0]
print("Earth from EMB:", earth_from_emb)
sum = -earth_from_emb + moon_from_emb + sc_from_moon
print("Sum: -earth_from_emb + moon_from_emb + sc_from_moon\n\t", sum)
print("Delta:", sum - sc_from_earth)
def __ClockDrift(self, enddate=False):
if self.name != 'MPO':
sclk_start = 0.0
sclk_end = 500000000
else:
sclk_start = 3.9631239807361E+13/65536
sclk_end = 700000000
#sclk_end = spiceypy.gdpool('SCLK_PARTITION_END_{}'.format(str(-1*self.id)),0,1000)[0]/65536
step = 10000.0
if not enddate:
et_end = self.time.getTime('finish','utc')
else:
et_end = spiceypy.utc2et(enddate)
sclk = []
ephtime = []
utctime = []
for i in np.arange(sclk_start, sclk_end, step):
sclk.append(i)
sclkdp = i*65536
et = spiceypy.sct2e(self.id, sclkdp)
ephtime.append(et)
utcstr = spiceypy.et2utc(et, 'C', 3)
utctime.append(utcstr)
dates = []
drift = []
for j in range(0,len(ephtime),1):
if ephtime[j] >= et_end:
break
drift.append((sclk[j]-sclk_start) - (ephtime[j] - ephtime[0]))
dates.append(ephtime[j])
self.clock_dates = dates
self.clock_drift = drift
return
def utc_to_scet(self, utc):
"""
Convert UTC ISO format to SCET time strings.
Parameters
----------
utc : `str`
UTC time string in ISO format e.g. '2019-10-24T13:06:46.682758'
Returns
-------
`str`
SCET time string
"""
# Utc to Ephemeris time (seconds past J2000)
ephemeris_time = spiceypy.utc2et(utc)
# Ephemeris time to Obt
return spiceypy.sce2s(SOLAR_ORBITER_ID, ephemeris_time)
def writeTimeLsToFile():
"""make list of time vs ls"""
SPICE_TARGET = "MARS"
SPICE_ABERRATION_CORRECTION = "None"
DATETIME_FORMAT = "%d/%m/%Y %H:%M"
from datetime import datetime, timedelta
linesToWrite = []
datetimeStart = datetime(2018, 3, 1, 0, 0, 0, 0)
for hoursToAdd in range(0, 24*31*12*3, 6): #3 years
newDatetime = (datetimeStart + timedelta(hours=hoursToAdd)).strftime(DATETIME_FORMAT)
ls = sp.lspcn(SPICE_TARGET, sp.utc2et(str(datetimeStart + timedelta(hours=hoursToAdd))), SPICE_ABERRATION_CORRECTION) * sp.dpr()
linesToWrite.append("%s\t%0.1f" %(newDatetime, ls))
writeOutput("Time_vs_Ls.txt", linesToWrite)
def get_posns(self,
obscode,
times,
center="Sun",
frame="J2000",
abcorr="NONE"):
""" """
# Convert the supplied time to the required format for spiceypy
# -----------------------------------------------
self.epochs = np.array(
[sp.utc2et('JD' + str(jdutc)) for jdutc in self.time.utc.jd])
# Evaluate the position of the satellite using the loaded kernels
# -----------------------------------------------
self.posns, self.ltts = sp.spkpos(obscode, self.epochs, frame, abcorr,
center) # [km, s]
self.posns = self.convert(posns=self.posns) # AU
self.ltts = self.convert(ltts=self.ltts) # Day
def get_posns(self,
obscode,
times,
center="Sun",
frame="J2000",
abcorr="NONE"):
"""
"""
# Convert the supplied time to the required format for spiceypy
# -----------------------------------------------
self.epochs = np.array(
[sp.utc2et('JD' + str(jdutc)) for jdutc in times.utc.jd])
# Get observatory posn for specific obs-code supplied
# NB: this is in fractions of an earth-radius
# So will probably need multiplying by 6378.1363/149597870.700 to get to AU
# -----------------------------------------------
self.obs_vec = ground_obscode_dict[obscode] * Rearth_km
# Use pxform to return the matrix that transforms position vectors from ITRF93 (not IAU_EARTH) frame to J2000 frame at specified epoch.
# Rotate the observatory posn vec to the required frame ( the J2000 default means this would be EQUATORIAL)
#https://naif.jpl.nasa.gov/pub/naif/toolkit_docs/FORTRAN/spicelib/pxform.html
#https://spiceypy.readthedocs.io/en/v2.3.1/documentation.html#spiceypy.spiceypy.pxform
# -----------------------------------------------
self.obs_vec_rot = np.array([
np.dot(sp.pxform('ITRF93', frame, epoch), self.obs_vec)
for epoch in self.epochs
])
self.obs_vec_rot_AU = self.obs_vec_rot / au_km
# Get the position of the geocenter
# ( the default frame=J2000 & center=SUN means this would be HELIOCENTRIC EQUATORIAL)
# -----------------------------------------------
self.posns, self.ltts = sp.spkpos('399', self.epochs, frame, abcorr,
center)
self.posns = self.convert(posns=self.posns) # AU
self.ltts = self.convert(ltts=self.ltts) # Day
# Combine vectors to get the posn vec of the observatory
# ( the default frame=J2000 & center=SUN means this would be HELIOCENTRIC EQUATORIAL)
# -----------------------------------------------
self.hXYZ = self.obs_vec_rot_AU + self.posns
def get_Earth_Sun_coords(t, ABCORR):
"""
Get Earth (Geocentric) and solar (Heliocentric) ephemeris (km) relative to solar
system Barycenter at times t
"""
FRAME = 'J2000'
OBSERVER = '0' # Solar System Barycenter (SSB)
N = len(t)
# TODO: vectorize??
xyzEarth = np.empty((N, 3), np.float128)
xyzSun = np.empty((N, 3), np.float128)
ltEarth = np.empty(N)
ltSun = np.empty(N)
for i, t in enumerate(t):
# Ephemeris time (seconds since J2000 TDB)
et = spice.utc2et(str(t))
# Earth geocenter wrt SSB in J2000 coordiantes
xyzEarth[i], ltEarth[i] = spice.spkpos(OBSERVER, et, FRAME, ABCORR,
'earth')
# Sun heliocenter wrt SSB in J2000 coordiantes
xyzSun[i], ltSun[i] = spice.spkpos(OBSERVER, et, FRAME, ABCORR, '10')
return xyzSun, xyzEarth
import matplotlib.pyplot as plt # pyplot
from matplotlib.figure import Figure
import numpy as np
import spiceypy as sp
# HBT imports
import hbt
sp.furnsh('kernels_kem_ats.tm')
utc_start = "2019 1 Jan 06:40:00"
utc_end = "2019 1 Jan 07:20:00"
et_start = sp.utc2et(utc_start)
et_end = sp.utc2et(utc_end)
et_mid = (et_start + et_end)/2
num_dt = 500
et = hbt.frange(et_start, et_end, num_dt)
name_target = 'MU69'
name_observer = 'New Horizons'
dist = np.zeros(num_dt)
phase = np.zeros(num_dt)
for i,et_i in enumerate(et):
file_tm = file_tm_nightside # I have not really validated that nightside works. Results look dfft than expected.
side_str = 'nightside'
sp.furnsh(file_tm) # Start up SPICE
hour = 3600
day = 24 * hour
fs = 15 # General font size
if ('tcm22' in file_tm):
utc_ca = '2019 1 jan 07:00:00'
else:
utc_ca = '2019 1 jan 03:09:00' # MU69 C/A time. I got this from GV.
et_ca = sp.utc2et(utc_ca)
dt_tof = 180 # Time-of-flight uncertainty (halfwidth, seconds)
# Define the dates of the OpNavs. I have no time for these, but it probably doens't matter.
# Taken from MOL = Master Obs List spreadsheet 27-Mar-2017
utc_opnav = np.array(
[
# '16 Aug 2018',
'15 Sep 2018', '16 Sep 2018', '17 Sep 2018',
'24 Sep 2018', '25 Sep 2018', '26 Sep 2018',
'05 Oct 2018', '06 Oct 2018', '07 Oct 2018',
'15 Oct 2018', '16 Oct 2018', '17 Oct 2018',
'25 Oct 2018', '26 Oct 2018', '27 Oct 2018',
'04 Nov 2018', '05 Nov 2018', '06 Nov 2018',
def utcstr_to_spiceet(time):
"""passthrough to spiceypy.utc2et"""
if isinstance(time, bytes):
return spiceypy.utc2et(time.decode('utf-8'))
return spiceypy.utc2et(time)
def _get_et(self):
return spice.utc2et(self.utc)
def test_frame_mu69_sunflower():
"""
This is just a quick test routine to check that MU69 Sunflower frame is more-or-less working.
This program prints the RA/Dec of MU69's Y and Z axes, under a variety of different conditions.
No options.
Things to verify here:
- That the Z RA/Dec point toward the orbit pole RA/Dec in all cases.
Small deviations << 1 deg allowed
- That the Y RA/Dec point toward the Sun always for _ROT Frames.
(ie, Y RA/Dec changes with time.)
- That the Y RA/Dec point toward the Sun for the _INERT frames on 1 Jan 2015,
and slowly move after / before that, at roughly 1 deg/year.
(ie, Y RA/Dec is pretty much fixed)
16-Jan-2018. HBT verified that output values look pretty good.
"""
tms = ['kernels_sunflower.tm'] # Define the metakernel, which in turn calls the sunflower .tf frame
frames = ['2014_MU69_SUNFLOWER_ROT', '2014_MU69_SUNFLOWER_INERT']
utcs = ['1 Jan 2005 00:00:00', '1 Jan 2015 00:00:00']
frame_j2k = 'J2000'
# Get values from Simon Porter. See email from MRS ~16-Jan-2018.
# These RA/Dec values are also put into the .tf file which I have made.
ra_mu69_sp = 272.426110231801*hbt.d2r
dec_mu69_sp = 68.831520928192*hbt.d2r
# Define the MU69 Z axis. We will rotate this, and it should point in specified direction.
z_mu69 = [0, 0, 1] # MU69 +Z axis. It should point to the specified RA/Dec
y_mu69 = [0, 1, 0] # MU69 +Y axis. It should point away from the Sun
print("Simon Porter pole position:")
print("RA = {}, Dec = {}".format(ra_mu69_sp*hbt.r2d, dec_mu69_sp*hbt.r2d))
print("---")
# Loop over input parameters. For each combination, do a calculation, and print the output.
for tm in tms:
for frame in frames:
for utc in utcs:
sp.furnsh(tm)
et = sp.utc2et(utc)
mx = sp.pxform(frame, frame_j2k, et)
z_mu69_j2k = sp.mxv(mx, z_mu69)
(_, ra_z, dec_z) = sp.recrad(z_mu69_j2k)
y_mu69_j2k = sp.mxv(mx, y_mu69)
(_, ra_y, dec_y) = sp.recrad(y_mu69_j2k)
print("Metakernel: {}".format(tm))
print("UTC: {}".format(utc))
print("Frame: {}".format(frame))
print("Matrix: \n{}".format(mx))
print("Y RA = {}, Dec = {}".format(ra_y*hbt.r2d, dec_y*hbt.r2d))
print("Z RA = {}, Dec = {}".format(ra_z*hbt.r2d, dec_z*hbt.r2d))
print("\n---\n")
iof_ring = 1e-7
exptime = 30
mode = '4X4'
#mode = '1X1'
pos = (None, None)
#pos = (300, 700)
pos = (100, 200) # y, x in normal imshow() coordinates.
#dist_target = 0.01*u.au
dist_solar = 43.2*u.au # MU69 dist at encounter: 43.2 AU, from KEM Wiki page
do_psf = True # Flag: Do we convolve result with NH LORRI PSF?26.7 + 0.65
dt_obs = -22*u.day # Time relative to MU69 C/A
utc_ca = '2019 1 Jan 05:33:00'
et_ca = sp.utc2et(utc_ca)
et_obs = et_ca + dt_obs.to('s').value
utc_obs = sp.et2utc(et_obs, 'C', 0)
utc_obs_human = 'K{:+}d'.format(dt_obs.to('day').value)
vec,lt = sp.spkezr('2014 MU69', et_obs, 'J2000', 'LT', 'New Horizons')
vec_sc_targ = vec[0:3]
dist_target = np.sqrt(np.sum(vec_sc_targ**2))*u.km.to('AU')*u.au
arr = nh_make_simulated_image_lorri(do_ring=True,
dist_ring_smoothing = 1000*u.km,
iof_ring = iof_ring,
a_ring = (5000*u.km, 10000*u.km),
exptime = exptime,
mode = mode,
width_fov_rad = 5.7 * hbt.d2r
height_fov_rad = 0.15 * hbt.d2r
dt_slew = 30 # Time between slews
exptime = 10 # Exposure time, MVIC.
exp_per_footprint = 3 # Number of total exposures per pointing. ('3' for 2+1.)
frac_overlap = 0.92 # Fractional overlap between footprints
fs = 15 # General font size
utc_ca = '2019 1 Jan 07:00:00'
n_footprints = 27
et_ca = sp.utc2et(utc_ca)
et_start = et_ca + 30*minute
et_end = et_start + 30*minute
radius_image = 2500*u.km
radius_kbo = 20*u.km
radius_ring = 1000*u.km
radius_ring_km = radius_ring.to('km').value
radius_ring_km = np.array([150, 500, 1250])
#==============================================================================
# Set up the times for each exposure
#==============================================================================
# HBT imports
import hbt
file_tm = 'kernels_kem_prime.tm'
sp.furnsh(file_tm)
utc_limits_arr = ["2018 1 Dec 5:00", "2018 1 Dec 12:00"]
utc_limits_arr = ["2019 1 Jan 5:00", "2019 1 Jan 6:00"]
et_limits_arr = []
for utc in utc_limits_arr:
et_limits_arr.append(sp.utc2et(utc))
num_et = 100
et_arr = hbt.frange(et_limits_arr[0], et_limits_arr[1], num_et)
phase_arr = []
utc_arr = []
for et in et_arr:
(st, lt) = sp.spkezr('MU69', et, 'J2000', 'LT+S', 'New Horizons')
vec_sc_mu69 = st[0:3]
(st, lt) = sp.spkezr('MU69', et, 'J2000', 'LT+S', 'Sun')
vec_sun_mu69 = st[0:3]
else:
dt_s = float(file['ET']) - t0
m, s = divmod(dt_s, 60)
h, m = divmod(m, 60)
dt_str = "{:3d}h {:2d}m {:2d}s".format(int(h), int(m), int(s))
if (dt_s == 0): dt_str = '--'
dt_str = dt_str.replace(' 0h', '').replace(' 0m', '')
t0 = float(file['ET'])
# Create a super-short version of the filename (cut out the ApID)
file_trunc = file['Shortname'].replace('lor_', '').replace('_0x630_sci', '').\
replace('_0x633_sci', '').replace('_opnav', '').replace('.fit', '')
utc_trunc = sp.et2utc(sp.utc2et(file['UTC']),'C', 0)
# Print a line of the table, to the screen and the file
line = "{:>3}/{:<3}: {:>3}, {:>3}, {}, {}, {}, {:6.3f},{:>12s}, {:.1f} deg, {:<9}".format(int(i),
int(num_files), int(i_group),
int(i_file), file_trunc, file['Format'], utc_trunc,
file['Exptime'], (dt_str), file['Phase']*hbt.r2d, file['Target'])
print(line)
lines_out.append(line)
arr = hbt.read_lorri(file['Filename'], bg_method = 'Polynomial', bg_argument = 4, frac_clip = 1)
arr = hbt.remove_brightest(arr, 0.99)
arr = -hbt.remove_brightest(-arr, 0.99)
def get_fits_info_from_files_lorri(path,
file_tm = "/Users/throop/gv/dev/gv_kernels_new_horizons.txt", pattern=''):
"Populate an astropy table with info from the headers of a list of LORRI files."
import numpy as np
import spiceypy as sp
import glob
import astropy
from astropy.io import fits
from astropy.table import Table
import astropy.table
import math
import hbt
# For testing:
# file = '/Users/throop/Data/NH_Jring/data/jupiter/level2/lor/all/lor_0035020322_0x630_sci_1.fit' # 119 deg phase as per gv
# file = '/Users/throop/Data/NH_Jring/data/jupiter/level2/lor/all/lor_0034599122_0x630_sci_1.fit' # 7 deg phase, inbound
# t = hbt.get_fits_info_from_files_lorri(file)
# Flags: Do we do all of the files? Or just a truncated subset of them, for testing purposes?
DO_TRUNCATED = False
NUM_TRUNC = 100
# We should work to standardize this, perhaps allowing different versions of this function
# for different instruments.
d2r = np.pi /180.
r2d = 1. / d2r
sp.furnsh(file_tm)
# *** If path ends with .fit or .fits, then it is a file not a path. Don't expand it, but read it as a single file.
if (('.fits' in path) or ('.fit' in path)):
file_list = path
files = [file_list]
else:
dir_data = path
#dir_data = '/Users/throop/data/NH_Jring/data/jupiter/level2/lor/all'
# Start up SPICE
# Get the full list of files
# List only the files that match an (optional) user-supplied pattern, such as '_opnav'
file_list = glob.glob(dir_data + '/*' + pattern + '.fit')
files = np.array(file_list)
indices = np.argsort(file_list)
files = files[indices]
# Read the JD from each file. Then sort the files based on JD.
jd = []
for file in files:
hdulist = fits.open(file)
jd.append(hdulist[0].header['MET'])
hdulist.close()
fits_met = [] # new list (same as array)
fits_startmet= []
fits_stopmet = []
fits_exptime = [] # starting time of exposure
fits_target = []
fits_reqdesc = []
fits_reqcomm = [] # New 9-Oct-2018
fits_reqid = [] # New 9-Oct-2018
fits_spcinst0= []
fits_spcutcjd= []
fits_naxis1= []
fits_naxis2 = []
fits_sformat = [] # Data format -- '1x1' or '4x4'
fits_spctscx = [] # sc - target, dx
fits_spctscy = [] # dy
fits_spctscz = [] # dz
fits_spctcb = [] # target name
fits_spctnaz = [] # Pole angle between target and instrument (i.e., boresight rotation angle)
fits_rsolar = [] # (DN/s)/(erg/cm^2/s/Ang/sr), Solar spectrum. Use for resolved sources.
if (DO_TRUNCATED):
files = files[0:NUM_TRUNC]
#files_short = np.array(files)
#for i in range(files.size):
# files_short = files[i].split('/')[-1] # Get just the filename itself
# Set up one iteration variable so we don't need to create it over and over
num_obs = np.size(files)
i_obs = np.arange(num_obs)
print("Read " + repr(np.size(files)) + " files.")
for file in files:
print("Reading file " + file)
hdulist = fits.open(file)
header = hdulist[0].header
keys = header.keys()
fits_met.append(header['MET'])
fits_exptime.append(header['EXPTIME'])
fits_startmet.append(header['STARTMET'])
fits_stopmet.append(header['STOPMET'])
fits_target.append(header['TARGET'])
fits_reqdesc.append(header['REQDESC'])
fits_reqcomm.append(header['REQCOMM'])
fits_reqid.append(header['REQID'])
fits_spcinst0.append(header['SPCINST0'])
fits_spcutcjd.append( (header['SPCUTCJD'])[3:]) # Remove the 'JD ' from before number
fits_naxis1.append(header['NAXIS1'])
fits_naxis2.append(header['NAXIS2'])
fits_spctscx.append(header['SPCTSCX'])
fits_spctscy.append(header['SPCTSCY'])
fits_spctscz.append(header['SPCTSCZ'])
fits_spctnaz.append(header['SPCTNAZ'])
fits_sformat.append(header['SFORMAT'])
fits_rsolar.append(header['RSOLAR']) # NB: This will be in the level-2 FITS, but not level 1
hdulist.close() # Close the FITS file
#print object
#print "done"
# Calculate distance to Jupiter in each of these
# Calc phase angle (to Jupiter)
# Eventually build backplanes: phase, RA/Dec, etc.
# Eventually Superimpose a ring on top of these
# ** Not too hard. I already have a routine to create RA/Dec of ring borders.
# Eventually overlay stars
# Q: Will there be enough there?
# Eventually repoint based on stars
# ** Before I allow repointing, I should search a star catalog and plot them.
# Convert some things to numpy arrays. Is there any disadvantage to this?
met = np.array(fits_met)
jd = np.array(fits_spcutcjd, dtype='d') # 'f' was rounding to one decimal place...
naxis1 = np.array(fits_naxis1)
naxis2 = np.array(fits_naxis2)
target = np.array(fits_target) # np.array can use string arrays as easily as float arrays
instrument = np.array(fits_spcinst0)
dx_targ = np.array(fits_spctscx)
dy_targ = np.array(fits_spctscy)
dz_targ = np.array(fits_spctscz)
desc = np.array(fits_reqdesc)
reqid = np.array(fits_reqid)
reqcomm = np.array(fits_reqcomm)
met0 = np.array(fits_startmet)
met1 = np.array(fits_stopmet)
exptime = np.array(fits_exptime)
rotation = np.array(fits_spctnaz)
sformat = np.array(fits_sformat)
rotation = np.rint(rotation).astype(int) # Turn rotation into integer. I only want this to be 0, 90, 180, 270...
rsolar = np.array(fits_rsolar)
files_short = np.zeros(num_obs, dtype = 'U60')
# Now do some geometric calculations and create new values for a few fields
dist_targ = np.sqrt(dx_targ**2 + dy_targ**2 + dz_targ**2)
phase = np.zeros(num_obs)
utc = np.zeros(num_obs, dtype = 'U30')
et = np.zeros(num_obs)
subsclat = np.zeros(num_obs) # Sub-sc latitude
subsclon = np.zeros(num_obs) # Sub-sc longitude
name_observer = 'New Horizons'
frame = 'J2000'
abcorr = 'LT+S'
# Note that using light time corrections alone ("LT") is
# generally not a good way to obtain an approximation to an
# apparent target vector: since light time and stellar
# aberration corrections often partially cancel each other,
# it may be more accurate to use no correction at all than to
# use light time alone.
# Fix the MET. The 'MET' field in fits header is actually not the midtime, but the time of the first packet.
# I am going to replace it with the midtime.
# *** No, don't do that. The actual MET field is used for timestamping -- keep it as integer.
# met = (met0 + met1) / 2.
# Loop over all images
for i in i_obs:
# Get the ET and UTC, from the JD. These are all times *on s/c*, which is what we want
et[i] = sp.utc2et('JD ' + repr(jd[i]))
utc[i] = sp.et2utc(et[i], 'C', 2)
# Calculate Sun-Jupiter-NH phase angle for each image
(st_jup_sc, ltime) = sp.spkezr('Jupiter', et[i], frame, abcorr, 'New Horizons') #obs, targ
(st_sun_jup, ltime) = sp.spkezr('Sun', et[i], frame, abcorr, 'Jupiter')
ang_scat = sp.vsep(st_sun_jup[0:3], st_jup_sc[0:3])
phase[i] = math.pi - ang_scat
# phase[i] = ang_scat
files_short[i] = files[i].split('/')[-1]
# Calc sub-sc lon/lat
mx = sp.pxform(frame,'IAU_JUPITER', et[i])
st_jup_sc_iau_jup = sp.mxv(mx, st_jup_sc[0:3])
(radius,subsclon[i],subsclat[i]) = sp.reclat(st_jup_sc[0:3]) # Radians
(radius,subsclon[i],subsclat[i]) = sp.reclat(st_jup_sc_iau_jup) # Radians
# Stuff all of these into a Table
t = Table([i_obs, met, utc, et, jd, files, files_short, naxis1, naxis2, target, instrument,
dx_targ, dy_targ, dz_targ, reqid,
met0, met1, exptime, phase, subsclat, subsclon, naxis1,
naxis2, rotation, sformat, rsolar, desc, reqcomm],
names = ('#', 'MET', 'UTC', 'ET', 'JD', 'Filename', 'Shortname', 'N1', 'N2', 'Target', 'Inst',
'dx', 'dy', 'dz', 'ReqID',
'MET Start', 'MET End', 'Exptime', 'Phase', 'Sub-SC Lat', 'Sub-SC Lon', 'dx_pix',
'dy_pix', 'Rotation', 'Format', 'RSolar', 'Desc', 'Comment'))
# Define units for a few of the columns
t['Exptime'].unit = 's'
t['Sub-SC Lat'].unit = 'degrees'
# Create a dxyz_targ column, from dx dy dz. Easy!
t['dxyz'] = np.sqrt(t['dx']**2 + t['dy']**2 + t['dz']**2) # Distance, in km
return t
def nh_find_simulated_rings_lorri():
# =============================================================================
# Now go thru the synthetic ring images.
# Load and stack the synthetic implanted images.
# Load and stack the original 'raw' frames
# Difference them, and see if we can find a ring in there.
# =============================================================================
dir_porter = '/Users/throop/Dropbox/Data/NH_KEM_Hazard/Porter_Sep17/'
dir_synthetic = '/Users/throop/Dropbox/Data/NH_KEM_Hazard/synthetic/'
do_subpixel = False # Flag: Do we use sub-pixel shifting when doing the flattening?
# It is slower and in theory better, but in reality makes a trivial difference.
# Start up SPICE
file_kernel = 'kernels_kem.tm'
sp.furnsh(file_kernel)
# Load the images into a table
images_raw = image_stack(dir_porter)
images_syn = image_stack(dir_synthetic, do_force=False)
stretch = astropy.visualization.PercentileInterval(95)
plt.set_cmap('Greys_r')
# =============================================================================
# If desired, do a one-time routine for the synthetic images:
# extract the I/F and ring size from the filenames, and append that to the table.
# This routine should be run after creating new synthetic images (e.g., adding an I/F value)
# =============================================================================
DO_APPEND = False
if (DO_APPEND):
t_syn = images_syn.t
num_images_syn = (np.shape(t_syn))[0]
iof_ring = np.zeros(num_images_syn, dtype=float)
size_ring = np.zeros(num_images_syn, dtype='U30')
for i in range(num_images_syn):
f = t_syn['filename_short'][i]
m = re.search('ring_(.*)_iof(.*)_K', f) # Call regexp to parse it.
iof_ring[i] = eval(m.group(2))
size_ring[i] = m.group(1)
t_syn['size_ring'] = size_ring
t_syn['iof_ring'] = iof_ring
images_syn.t = t_syn
images_syn.save() # Save the whole pickle archive (including images and table) back to disk
data_raw = images_raw.data
data_syn = images_syn.data
t_raw = images_raw.t
t_syn = images_syn.t
num_images_raw = (np.shape(t_raw))[0]
num_images_syn = (np.shape(t_syn))[0]
# Look up the time offset, from the image title. (Would be better to have it stored in table, but this will do.)
match = re.search('_K(.*)d', t_syn['filename_short'][0])
dt_ca = ((match.group(1)*u.day).to('s')) # Weird: we don't need .value here. I can't explain it.
utc_ca = '2019 1 Jan 05:33'
et_ca = sp.utc2et(utc_ca)
et_obs = et_ca + dt_ca
# Set the pixel scale
vec,lt = sp.spkezr('2014 MU69', et_obs, 'J2000', 'LT', 'New Horizons')
vec_sc_targ = vec[0:3]
dist_target_km = (sp.vnorm(vec_sc_targ)*u.km).value
scale_pix_lorri_1x1_rad = 0.3*hbt.d2r / 1024
scale_pix_lorri_4x4_rad = scale_pix_lorri_1x1_rad * 4
scale_pix_km_dict = {'1X1' : scale_pix_lorri_1x1_rad * dist_target_km,
'4X4' : scale_pix_lorri_4x4_rad * dist_target_km} # We are
# Create a bunch of possible image sets, based on various parameters
# Indices for 'raw' images
indices_sep17_raw = t_raw['et'] > sp.utc2et('15 sep 2017') # The positon of MU69 has changed a few pixels.
# We can't blindly co-add between sep and pre-sep
indices_jan17_raw = t_raw['et'] < sp.utc2et('1 sep 2017')
indices_rot0_raw = t_raw['angle'] < 180 # One rotation angle
indices_rot90_raw = t_raw['angle'] > 180 # The other rotation angle
indices_10sec_raw = np.logical_and( t_raw['exptime'] < 10, t_raw['exptime'] > 5 )
indices_20sec_raw = np.logical_and( t_raw['exptime'] < 20, t_raw['exptime'] > 10 )
indices_30sec_raw = np.logical_and( t_raw['exptime'] < 30, t_raw['exptime'] > 20 )
indices_1x1_raw = t_raw['naxis1'] == 1024
indices_4x4_raw = t_raw['naxis1'] == 256
indices_30sec_4x4_raw = np.logical_and(indices_4x4_raw, indices_30sec_raw) # 94
# Indices for synthetic images
indices_ring_small_syn = t_syn['size_ring'] == 'small'
indices_ring_large_syn = t_syn['size_ring'] == 'large'
indices_iof_1em7_syn = t_syn['iof_ring'] == 1e-7
indices_iof_3em7_syn = t_syn['iof_ring'] == 3e-7
indices_iof_1em6_syn = t_syn['iof_ring'] == 1e-6
indices_iof_1em5_syn = t_syn['iof_ring'] == 1e-5
indices_iof_1em4_syn = t_syn['iof_ring'] == 1e-4
indices_small_1em7_syn = np.logical_and(indices_iof_1em7_syn, indices_ring_small_syn)
indices_small_3em7_syn = np.logical_and(indices_iof_3em7_syn, indices_ring_small_syn)
indices_small_1em6_syn = np.logical_and(indices_iof_1em6_syn, indices_ring_small_syn)
indices_small_1em5_syn = np.logical_and(indices_iof_1em5_syn, indices_ring_small_syn)
indices_small_1em4_syn = np.logical_and(indices_iof_1em4_syn, indices_ring_small_syn)
indices_large_1em7_syn = np.logical_and(indices_iof_1em7_syn, indices_ring_large_syn)
indices_large_3em7_syn = np.logical_and(indices_iof_3em7_syn, indices_ring_large_syn)
indices_large_1em6_syn = np.logical_and(indices_iof_1em6_syn, indices_ring_large_syn)
indices_large_1em5_syn = np.logical_and(indices_iof_1em5_syn, indices_ring_large_syn)
indices_large_1em4_syn = np.logical_and(indices_iof_1em4_syn, indices_ring_large_syn)
# Choose which indiex. ** THIS IS WHERE WE SET THE RING TO USE!!
indices_raw = indices_30sec_4x4_raw.copy() # 94 of 344
indices_syn = indices_small_1em6_syn.copy() # 94 of 752
# Now take the first half of the synthetic indices, and the second half of the raw ones
# This is to assure that we are using different images for the two stacks! Otherwise, the results are trivial.
frames_max = int(np.sum(indices_raw) / 2) # Total number of frames (94)
w = np.where(indices_raw)[0]
indices_raw[w[frames_max]:] = False # De-activate all frames *below* frames_max
w = np.where(indices_syn)[0]
indices_syn[:w[frames_max]] = False # De-activate all frames above frames_max
# Set the indices
images_raw.set_indices(indices_raw)
images_syn.set_indices(indices_syn)
# Do the flattening
arr_raw = images_raw.flatten(do_subpixel=do_subpixel)
arr_syn = images_syn.flatten(do_subpixel=do_subpixel)
# arr_raw_sub = images_raw.flatten(do_subpixel=True)
# arr_syn_sub = images_syn.flatten(do_subpixel=True)
# Extract various fields from the data table. We can look up from any of the images -- they should be all the same.
t_syn = images_syn.t # Get the data table
iof_ring = t_syn[indices_syn]['iof_ring'][0]
size_ring = t_syn[indices_syn]['size_ring'][0]
exptime = t_syn[indices_syn]['exptime'][0]
# The two flattened images need some offsetting. Do that.
shift = ird.translation(arr_raw, arr_syn)['tvec']
# shift = np.round(shift).astype('int')
# arr_syn_shift = np.roll(np.roll(arr_syn, int(round(shift[0])), axis=0), int(round(shift[1])), axis=1)
arr_syn_shift = scipy.ndimage.shift(arr_syn, shift, order=5) # This allows sub-pixel shifts, apparently. *NO*!
# a = arr_syn.copy()
# a_05_05 = scipy.ndimage.shift(arr_syn, (0.5, 0.5), order=5) # Ugh. 0.5, 0.5 and 1, 1 are *exactly* the same.
# a_1_05 = scipy.ndimage.shift(arr_syn, (1, 0.5), order=5)
# a_1_1 = scipy.ndimage.shift(arr_syn, (1, 1), order=5)
# a_1_15 = scipy.ndimage.shift(arr_syn, (1, 1.5), order=5)
# a_1_0 = scipy.ndimage.shift(arr_syn, (1, 0), order=5)
# a_05_0 = scipy.ndimage.shift(arr_syn, (0.5, 0), order=5)
arr_diff = arr_syn_shift - arr_raw
pos = (images_raw.y_pix_mean*4, images_raw.x_pix_mean*4)
# Set the binning width of the radial profiles
binning_pix = 5
# Extract the radial profiles
(dist_pix_1d, profile_1d_median) = get_radial_profile_circular(arr_diff, pos, method='median', width=binning_pix)
(dist_pix_1d, profile_1d_mean) = get_radial_profile_circular(arr_diff, pos, method='mean', width=binning_pix)
str_title = ('Synthetic ring - raw, I/F = {:.0e}, {}, {} x {:.1f}s'.format(
iof_ring, size_ring, frames_max, exptime))
plt.imshow(stretch(arr_diff))
plt.title(str_title)
plt.plot(pos[1], pos[0], marker='.', color='red')
plt.show()
# Set the scale for the effective mode of these observations. Many are taken as 4x4, but we've rebinned to 1x1
if (np.shape(arr_raw)[0] == 1024):
scale_mode = '1X1'
else:
scale_mode = '4X4'
scale_pix_km = scale_pix_km_dict[scale_mode]
# Make a plot of the radial profile. Don't plot the innermost bin. It is useless, since it has so few pixels in it.
hbt.figsize((12,8))
plt.plot(dist_pix_1d[1:] * scale_pix_km, profile_1d_median[1:], label = 'Annulus median', alpha = 0.7)
# plt.plot(dist_pix_1d[1:] * scale_pix_km, profile_1d_mean[1:], label = 'Mean', alpha = 0.2)
plt.xlabel('Distance [km]')
plt.ylabel('DN per pixel')
plt.title(str_title + ', binning = {}'.format(binning_pix))
plt.xlim((0,30000))
# Set the y axis range. This is really stupid. Can't matplotlib figure this out itself?
ax = plt.gca()
lims = ax.get_xlim()
i = np.where( (dist_pix_1d * scale_pix_km > lims[0]) & (dist_pix_1d*scale_pix_km < lims[1]) )[0]
ax.set_ylim( profile_1d_median[i].min(), profile_1d_median[i].max() )
plt.legend()
plt.show()
plt.savefig()
# These data files were obtained from
# http://naif.jpl.nasa.gov/pub/naif/generic_kernels
LEAP_SECOND_FILE = "data/naif0011.tls"
EPHEMERIDES_FILE = "data/de432s.bsp"
if __name__ == "__main__":
# Script expects first argument to be a UTC timestamp
if len(sys.argv) > 1:
input_utc = sys.argv[1]
else:
input_utc = "2000-01-01T00:00:00" # default for testing
# Load the necessary data files
sp.furnsh([LEAP_SECOND_FILE, EPHEMERIDES_FILE])
# Convert UTC to ephemeris time
epoch = sp.utc2et(input_utc)
# State (position and velocity in cartesian coordinates)
# of EARTH as seen from SUN in the ecliptic J2000 coordinate frame.
state, lt, = sp.spkezr("EARTH", epoch, "ECLIPJ2000", "NONE", "SUN")
# Show the output
print("Input time = {}".format(input_utc))
print("")
print("# Position of the Earth in the heliocentric ecliptic (J2000) frame")
print("X = {} km".format(state[0]))
print("Y = {} km".format(state[1]))
print("Z = {} km".format(state[2]))
print("")
print("# Velocity of the Earth in the same frame")
print("dX = {} km/s".format(state[3]))
print("dY = {} km/s".format(state[4]))
print("dZ = {} km/s".format(state[5]))
def nh_ort_track4_flyby(dir_in=None, dir_out=None, name_trajectory = 'prime'):
#%%%
# dir_in = '/Users/throop/
# dir_in = '/Users/throop/data/ORT4/throop/ort4_bc3_10cbr2_dph/'
stretch_percent = 99
stretch = astropy.visualization.PercentileInterval(stretch_percent)
# dir_data = os.path.expanduser('~/Data/')
# dir_in git
do_compress = False # Do we use .gzip compression on the Track-4 input grids?
# If we used compression on the track4_calibrate routine, we must use it here too.
# dir_track4 = os.path.join(dir_data, name_ort, 'throop', 'track4')
if do_compress:
files = glob.glob(os.path.join(dir_in, '*.grid4d.gz'))
else:
files = glob.glob(os.path.join(dir_in, '*.grid4d'))
files = glob.glob(os.path.join(dir_in, '*.dust.pkl'))
# Alphabetize file list
files = sorted(files)
plt.set_cmap('plasma')
utc_ca = '2019 1 Jan 05:33:00'
dt_before = 1*u.hour
dt_after = 1*u.hour
# area_sc = (1*u.m)**2
frame = '2014_MU69_SUNFLOWER_ROT'
name_target = 'MU69'
origin = 'lower' # Required plotting order for imshow
name_observer = 'New Horizons'
hbt.figsize((8,6))
hbt.set_fontsize(12)
dt = 1*u.s # Sampling time through the flyby. Astropy units.
# Create an output table, Astropy format
t = Table(names = ['trajectory', 'speed', 'q_dust', 'albedo', 'rho',
'tau_max', 'tau_typical', 'iof_max', 'iof_typical'],
dtype = ['U30', float, float, float, float,
float, float, float, float] )
# Start up SPICE if needed. Unload old kernels just as a safety precaution.
sp.unload('kernels_kem_prime.tm')
sp.unload('kernels_kem_alternate.tm')
sp.furnsh(f'kernels_kem_{name_trajectory}.tm')
do_short = False
if do_short:
files = files[0:4]
i=3
file = files[i]
num_files = len(files)
name_run = dir_out.split('/')[-2]
#%%%
for i,file in enumerate(files):
#%%%
print(f'Starting file {i}/{len(files)}')
grid = nh_ort_track4_grid(file) # Load the grid from disk. Uses gzip, so it is quite slow (10 sec/file)
print(f'Loading file {file}')
# Load the trajectory parameters
et_ca = int( sp.utc2et(utc_ca) ) # Force this to be an integer, just to make output cleaner.
et_start = et_ca - dt_before.to('s').value
et_end = et_ca + dt_after.to('s').value
grid.frame = frame
grid.name_target = name_target
grid.name_trajectory = name_trajectory
# And call the method to fly through it!
# The returned density values etc are available within the instance variables, not returned explicitly.
grid.fly_trajectory(name_observer, et_start, et_end, dt)
# If the first time thru loop, make plot of our path through the system
do_plots_geometry = True
if (do_plots_geometry and (i==0)):
grid.plot_trajectory_geometry()
# Make slice plots thru the grid
do_plot_slices_xyz = False
if do_plot_slices_xyz:
hbt.fontsize(8)
hbt.figsize((20,5))
grid.plot(axis_sum=0)
grid.plot(axis_sum=1)
grid.plot(axis_sum=2)
hbt.fontsize(10)
# Make a plot of optical depth
do_plot_tau = True
if do_plot_tau:
grid.plot_tau()
# =============================================================================
# Make some plots of count rate vs. time!
# =============================================================================
# Make a plot of the instantaneous count rate
hbt.figsize((10,15))
# Make a plot of the actual density that we give to Doug Mehoke
# Define a list of colors. This is so we can use colors= argument to set
# a marker to show grain size, rather than let plot() auto-assign.
# colors = plt.rcParams['axes.prop_cycle'].by_key()['color'] # This is the default color iterator.
colors = ['antiquewhite',
'tomato',
'blueviolet',
'skyblue',
'gold',
'darkcyan',
'thistle',
'olive',
'red',
'sienna',
'deepskyblue',
'lightsalmon',
'pink',
]
# 'aqua']
# 'antiquewhite4', 'aqua', 'aquamarine4', 'black', 'blue', 'blueviolet',
# 'brown1', 'chartreuse1', 'darkgreen', 'darkorange1', 'dodgerblue1', 'lightpink', 'magenta']
# Make a plot of dust number density. This is straight out of the grid, and for comparison with MRS.
vals_fiducial = [1e-10, 1e-8, 1e-6,1e-4, 1e-2, 1e-0]
plt.subplot(3,1,1)
for j,s in enumerate(grid.s):
plt.plot(grid.delta_et_t, grid.number_t[j],
label = 's={:.2f} mm'.format(s),
color=colors[j])
plt.legend()
plt.title('Dust number density'.format(grid.area_sc))
plt.xlabel('ET from C/A')
plt.yscale('log')
plt.ylim((1e-10, 1e2)) # Match to MRS.
plt.axvline(0, color='black', alpha=0.05)
plt.ylabel(r'Dust,, # km$^{-3}$')
for val in vals_fiducial:
plt.axhline(val, color='black', alpha=0.05)
# Make a plot of impact rate. This assumes a s/c area.
plt.subplot(3,1,2)
for j,s in enumerate(grid.s): # 's' is dust size
plt.plot(grid.delta_et_t, grid.number_sc_t[j],
label = f's={s:.2f} mm',
color=colors[j])
plt.title('Impact rate, A={}'.format(grid.area_sc))
plt.yscale('log')
plt.xlabel('ET from C/A')
plt.legend()
plt.ylabel(r'Dust, # Impacts sec$^{{-1}}$')
# Make a plot of the cumulative count rate. Mark grain sizes here too.
plt.subplot(3,1,3)
for j,s in enumerate(grid.s): # Loop over size
plt.plot(grid.delta_et_t, grid.number_sc_cum_t[j], # Main plot line
label = 's={:.2f} mm'.format(s), color=colors[j])
plt.plot([grid.delta_et_t[-1]], [grid.number_sc_cum_t[j,-1].value], # Circle to indicate grain size
markersize=(7-j)*2, marker = 'o', # Use same color as prev line!
color=colors[j])
hbt.figsize(5,5)
plt.legend()
plt.title('Number of impacts (cumulative), A={}'.format(grid.area_sc))
plt.xlabel('ET from C/A')
plt.yscale('log')
plt.ylabel('# of Impacts')
plt.axhline(y = 1, linestyle = '--', alpha = 0.1)
plt.tight_layout()
plt.show()
# Make a plot of size distibution.
# Make two curves: one for n(r) for the entire grid, and one for n(r) that hits s/c
# Now add an entry to the table. This is a table that lists all of the results --
# e.g., max_tau, count rate etc
# One line per grid.
t.add_row(vals=[grid.name_trajectory, grid.speed, grid.q, grid.albedo, grid.rho,
grid.tau_max, grid.tau_typ,
grid.iof_max, grid.iof_typ])
# Get size dist along path
number_path = grid.number_sc_cum_t[:,-1].value
# Take the full particle grid, and sum along all spatial axes, leaving just the size axis left.
number_grid = np.sum(np.sum(np.sum(grid.density, axis=1), axis=1), axis=1)
# Normalize the size dists both
number_grid = hbt.normalize(number_grid)
number_path = hbt.normalize(number_path)
plt.plot(grid.s, number_path, label = 'Along s/c path')
plt.plot(grid.s, number_grid, label = 'In grid, total')
plt.yscale('log')
plt.xscale('log')
plt.ylim( (hbt.minval(np.array([number_grid, number_path]))/2, 1) )
plt.xlabel('Radius [mm]')
plt.ylabel('Particle number [arbitrary]')
plt.legend(loc = 'lower right')
plt.show()
# Output the dust population for this run to a file. This is the file that Doug Mehoke will read.
grid.output_trajectory(name_run=name_run, do_positions=False, dir_out=dir_out)
print('---')
#%%%
# Print the table
t.pprint(max_width=-1)
# Save the table as output
file_out = os.path.join(dir_out, f'nh_{name_trajectory}_track4_table.pkl')
lun = open(file_out, 'wb')
pickle.dump(t,lun)
lun.close()
print(f'Wrote: {file_out}')
#%%%
# Now that all files have been created, compress results into an archive (.tar.gz) for Doug Mehoke
inits_track4 = 'hbt'
# if 'hamilton' in files[0]:
# inits_track3 = 'dph'
# if 'kauf' in files[0]:
# inits_track3 = 'dk'
file_out = f'{name_trajectory}_{name_run}_{inits_track4}_n{num_files}.tgz'
str = f'cd {dir_out}; tar -czf {file_out} *{name_trajectory}*.dust'
_ = subprocess.Popen(str, shell=True)
print(str)
print(f'Wrote: {dir_out}/{file_out}')
def __init__(self, master, size_window):
self.master = master # This is the handle to the main Tk widget. I have to use it occasionally to
# set up event handlers, so grab it and save it.
self.size_window = size_window # Save the size of the whole Tk window, in pixels.
# Open the image stack
# self.stretch_percent = 90
# self.stretch = astropy.visualization.PercentileInterval(self.stretch_percent) # PI(90) scales to 5th..95th %ile.
#
name_ort = 'ORT4'
# name_ort = 'ORT2_OPNAV'
if (name_ort == 'ORT1'):
self.reqids_haz = ['K1LR_HAZ00', 'K1LR_HAZ01', 'K1LR_HAZ02', 'K1LR_HAZ03', 'K1LR_HAZ04']
# self.reqids_haz = ['K1LR_HAZ03', 'K1LR_HAZ01', 'K1LR_HAZ02']
self.reqid_field = 'K1LR_MU69ApprField_115d_L2_2017264'
self.dir_data = '/Users/throop/Data/ORT1/throop/backplaned/'
if (name_ort == 'ORT2'):
self.reqids_haz = ['K1LR_HAZ00', 'K1LR_HAZ01', 'K1LR_HAZ02', 'K1LR_HAZ03', 'K1LR_HAZ04']
# self.reqids_haz = ['K1LR_HAZ03', 'K1LR_HAZ01', 'K1LR_HAZ02']
self.reqid_field = 'K1LR_MU69ApprField_115d_L2_2017264'
self.dir_data = '/Users/throop/Data/ORT2/throop/backplaned/'
if (name_ort == 'ORT3'):
self.reqids_haz = ['K1LR_HAZ00', 'K1LR_HAZ01', 'K1LR_HAZ02', 'K1LR_HAZ03', 'K1LR_HAZ04']
self.reqid_field = 'K1LR_MU69ApprField_115d_L2_2017264'
self.dir_data = '/Users/throop/Data/ORT3/throop/backplaned/'
if (name_ort == 'ORT4'):
self.reqids_haz = ['K1LR_HAZ00', 'K1LR_HAZ01', 'K1LR_HAZ02', 'K1LR_HAZ03']
self.reqid_field = 'K1LR_MU69ApprField_115d_L2_2017264'
self.dir_data = '/Users/throop/Data/ORT4/throop/backplaned/'
if (name_ort == 'ORT2_OPNAV'):
self.dir_data = '/Users/throop/Data/ORT2/throop/backplaned/'
dirs = glob.glob(self.dir_data + '/*LR_OPNAV*') # Manually construct a list of all the OPNAV dirs
self.reqids_haz = []
for dir_i in dirs:
self.reqids_haz.append(os.path.basename(dir_i))
self.reqids_haz = sorted(self.reqids_haz)
self.reqid_field = 'K1LR_MU69ApprField_115d_L2_2017264'
# Set the edge padding large enough s.t. all output stacks will be the same size.
# This value is easy to compute: loop over all stacks, and take max of stack.calc_padding()[0]
self.padding = 61 # Amount to pad the images by. This is the same as the max drift btwn all images in stacks
self.zoom = 4 # Sub-pixel zoom to apply when shifting images. 1 for testing; 4 for production.
self.num_image = 0 # Which stack number to start on.
self.zoom_screen = 1 # 'Screen zoom' amount to apply. This can be changed interactively.
self.is_blink = False # Blinking mode is turned off by default
self.dt_blink = 300 # Blink time in ms
# Start up SPICE if needed
if (sp.ktotal('ALL') == 0):
sp.furnsh('kernels_kem_prime.tm')
# Set the RA/Dec of MU69. We could look this up from SPICE but it changes slowly, so just keep it fixed for now.
self.radec_mu69 = (4.794979838984583, -0.3641418801015417)
# Set the CA time. Roughly doing this is fine.
self.et_ca = sp.utc2et('2019 1 Jan 05:33:00')
# Boolean. For the current image, do we subtract the field frame, or not?
self.do_subtract = True
hbt.set_fontsize(20)
# Set the stretch range, for imshow. These values are mapped to black and white, respectively.
self.vmin_diff = -1 # Range for subtracted images
self.vmax_diff = 2
self.vmin_raw = -1 # Range for raw images (non-subtracted)
self.vmax_raw = 1000
# Restore the stacks directly from archived pickle file, if it exists
self.file_save = os.path.join(self.dir_data,
f'stacks_blink_{name_ort}_n{len(self.reqids_haz)}_z{self.zoom}.pkl')
if os.path.isfile(self.file_save):
self.restore()
else:
# If no pickle file, load the stacks from raw images and re-align them
# Load and stack the field images
print("Stacking field images")
self.stack_field = image_stack(os.path.join(self.dir_data, self.reqid_field)) # The individual stack
self.stack_field.align(method = 'wcs', center = self.radec_mu69)
(self.img_field, self.wcs_field) =\
self.stack_field.flatten(zoom=self.zoom, padding=self.padding) # Save the stacked image and WCS
# Load and stack the Hazard images
self.img_haz = {} # Output dictionary for the stacked images
self.stack_haz = {} # Output dictionary for the stacks themselves
self.wcs_haz = {} # Output dictionary for WCS for the stacks
for reqid in self.reqids_haz:
self.stack_haz[reqid] = image_stack(os.path.join(self.dir_data, reqid)) # The individual stack
self.stack_haz[reqid].align(method = 'wcs', center = self.radec_mu69)
(self.img_haz[reqid], self.wcs_haz[reqid]) =\
self.stack_haz[reqid].flatten(zoom=self.zoom, padding=self.padding)
# Put them in a dictionary
# Save the stacks to a pickle file, if requested
yn = input("Save stacks to a pickle file? ")
if ('y' in yn):
self.save()
# Set the sizes of the plots -- e.g., (15,15) = large square
figsize_image = (15,15)
self.fig1 = Figure(figsize = figsize_image) # <- this is in dx, dy... which is opposite from array order!
self.ax1 = self.fig1.add_subplot(1,1,1,
label = 'Image') # Return the axes
plt.set_cmap('Greys_r')
self.canvas1 = FigureCanvasTkAgg(self.fig1,master=master)
self.canvas1.show()
# Put objects into appropriate grid positions
self.canvas1.get_tk_widget().grid(row=1, column=1, rowspan = 1)
# Define some keyboard shortcuts for the GUI
# These functions must be defined as event handlers, meaning they take two arguments (self and event), not just one.
master.bind('q', self.quit_e)
master.bind('<space>', self.toggle_subtract_e)
master.bind('=', self.prev_e)
master.bind('-', self.next_e)
master.bind('h', self.help_e)
master.bind('?', self.help_e)
master.bind('<Left>', self.prev_e)
master.bind('<Right>', self.next_e)
master.bind('s', self.stretch_e)
master.bind('b', self.blink_e)
master.bind('t', self.blink_set_time_e)
master.bind('#', self.blink_set_sequence_e)
master.bind('z', self.zoom_screen_up_e)
master.bind('Z', self.zoom_screen_down_e)
master.bind('x', self.clear_current_objects_e)
master.bind('X', self.clear_all_objects_e)
master.bind('=', self.scale_max_up_e)
master.bind('+', self.scale_max_down_e)
master.bind('-', self.scale_min_up_e)
master.bind('_', self.scale_min_down_e)
master.bind('S', self.save_output_e)
self.canvas1.get_tk_widget().bind("<Button 1>", self.click_e)
# Set the initial image index
self.reqid_haz = self.reqids_haz[self.num_image] # Set it to 'K1LR_HAZ00', for instance.
# Initialize the list of found objects for each stack
# There is a list of objects for each individual stack (ie, for each frame in the blink)
self.list_objects = {}
for reqid_i in self.reqids_haz:
self.list_objects[reqid_i] = [] # Each entry here will be something like [(x, y, dn), (x, y, dn)]
# Initialize a set of matplotlib 'line' objects for the image.
# These correspond to the 'objects' above, which are really just points
self.list_lines = {}
for reqid_i in self.reqids_haz:
self.list_lines[reqid_i] = [] # Each entry here will be a list of plot objects, of type 'line'
# Set a list of frame numbers to animate. For default, do them all.
self.list_index_blink = hbt.frange(0, len(self.reqids_haz)-1) # List of indices ( [1, 2, 3] )
self.list_index_blink_str = ' '.join(np.array(self.list_index_blink).astype(str)) # Make into string ('1 2 3')
self.index_blink = 0 # where in the list of indices do we start? Current index.
# Plot the image
self.plot()
def make_table_grid_positions():
"""
This is a one-off utility function for MRS.
In it, I just do a flyby of MU69, and output the X Y Z grid indices (as well as positions and timestamps).
I don't output density at all -- just the s/c positions.
I do this for both prime and alternate trajectories.
This is just because he hasn't integrated SPICE into his grid code.
This function is stand-alone. It doesn't rely on the grid class.
It is included in this file because it directly relates to the grids.
"""
#%%%
name_trajectory = 'alternate' # ← Set this to 'prime' or 'alternate'
# name_trajectory = 'prime' # ← Set this to 'prime' or 'alternate'
hbt.unload_kernels_all()
frame = '2014_MU69_SUNFLOWER_ROT'
name_observer = 'New Horizons'
name_target = 'MU69'
sp.furnsh(f'kernels_kem_{name_trajectory}.tm')
# Get the OD version. This might not work.
# files = hbt.list_kernels_loaded()
# for file in files:
# if
# file_in = '/Users/throop/Data/ORT2/throop/track4/ort2-ring_v2.2_q2.0_pv0.10_rho0.22.grid4d.gz'
# file_in = '/Users/throop/Data/ORT5/throop/deliveries/tuna9k/ort5_None_y3.0_q3.5_pv0.70_rho1.00.dust.txt'
file_in = '/Users/throop/Data/ORT5/kaufmann/deliveries/chr3-tunacan10k/chr3-0003' + \
'/y3.0/beta1.0e+00/subset00/model.array2'
# file_in = '/Users/throop/Data/ORT5/throop/deliveries/tuna9k/ort5_None_y3.0_q3.5_pv0.70_rho1.00.dust.pkl' #250km
# file_in = '/Users/throop/Data/ORT5/throop/deliveries/dph-sunflower10k/ort5_None_y2.2_q2.5_pv0.05_rho0.46.dust.pkl' #500km
file_in = '/Users/throop/Data/ORT5/throop/deliveries/dph-tunacan3.5kinc55/ort5_None_y2.2_q2.5_pv0.05_rho0.46.dust.pkl' #500km
grid = nh_ort_track4_grid(file_in) # Load the grid from disk. Uses gzip, so it is quite slow (10 sec/file)
resolution_km = int(grid.resolution_km[0])
utc_ca = '2019 1 Jan 05:33:00'
dt_before = 1*u.hour
dt_after = 1*u.hour
dt = 1*u.s # Sampling time through the flyby. Astropy units.
et_ca = int( sp.utc2et(utc_ca) ) # Force this to be an integer, just to make output cleaner.
et_start = et_ca - dt_before.to('s').value
et_end = et_ca + dt_after.to('s').value
grid.frame = frame
grid.name_target = name_target
grid.name_trajectory = name_trajectory
# And call the method to fly through it!
# The returned density values etc are available within the instance variables, not returned explicitly.
grid.fly_trajectory(name_observer, et_start, et_end, dt)
# Make plots
hbt.figsize((9,9))
hbt.fontsize(12)
plt.subplot(3,2,1)
plt.plot(grid.bin_x_t)
plt.ylabel('X Bin #')
plt.title(f'MU69, Trajectory = {name_trajectory}, frame = {frame}')
plt.subplot(3,2,3)
plt.plot(grid.bin_y_t)
plt.ylabel('Y Bin #')
plt.subplot(3,2,5)
plt.plot(grid.bin_z_t)
plt.ylabel('Z Bin #')
plt.xlabel('Timestep #')
t_t = grid.et_t - np.mean(grid.et_t)
bin_t = range(len(t_t))
plt.subplot(3,2,2)
plt.axhline(0, color='pink')
plt.axvline(0, color='pink')
plt.plot(t_t, grid.x_t)
plt.ylabel('X [km]')
plt.xlabel('t [sec]')
plt.subplot(3,2,4)
plt.axhline(0, color='pink')
plt.axvline(0, color='pink')
plt.plot(t_t, grid.y_t)
plt.ylabel('Y [km]')
plt.subplot(3,2,6)
plt.axhline(0, color='pink')
plt.axvline(0, color='pink')
plt.plot(t_t, grid.z_t)
plt.ylabel('Z [km]')
plt.xlabel('Time from C/A [sec]')
plt.tight_layout()
# Save the plot to a file
file_out = f'positions_trajectory_{name_trajectory}.png'
path_out = os.path.join(dir_out, file_out)
plt.savefig(path_out)
print(f'Wrote: {path_out}')
plt.show()
# Make a table
arr = {'bin' : bin_t,
'delta_et' : t_t,
'X_km' : grid.x_t,
'Y_km' : grid.y_t,
'Z_km' : grid.z_t,
'Bin_X' : grid.bin_x_t,
'Bin_Y' : grid.bin_y_t,
'Bin_Z' : grid.bin_z_t}
t = Table(arr, names=['bin', 'delta_et', 'X_km', 'Y_km', 'Z_km', 'Bin_X', 'Bin_Y', 'Bin_Z'],
dtype=['int', 'int', 'float', 'float', 'float', 'int', 'int', 'int'])
# Save the table to a file
file_out = f'positions_trajectory_{name_trajectory}_res{resolution_km}.txt'
path_out = os.path.join('/Users/throop/Data/ORT5', file_out)
t.write(path_out, format = 'ascii.csv', overwrite=True)
print(f'Wrote: {path_out}')
vmax = 100 # For vertical scaling
dpi = 50 # Size of the output picture. 200 for cathy. 50 for web. 100 for high-res web.
file_out_base = os.path.join(dir_frames, f'movie_w{width}_d{dpi}_{cmap}')
file_out_gif = f'{file_out_base}_n{len(reqids)}_f{fps}.gif'
for i,reqid_i in enumerate(reqids):
# Convert from DOY to calendar day
file_out_frame = f'{file_out_base}_{i:03}.png'
doy = reqid_i.split('_')[-1][-3:]
et = sp.utc2et(f'2018::{doy} 12:00:00')
utc = sp.timout(et, "Month DD, YYYY", 20)
utc = utc.replace(' 0', ' ')
# Draw the frame
f = plt.figure(frameon=False, figsize=(10, 5), dpi=dpi) # Change dpi to change output size
# f.patch.set_facecolor('pink')
canvas_width, canvas_height = f.canvas.get_width_height()
ax = f.add_axes([0, 0, 1, 1])
ax.axis('off')
# ax.set_facecolor('pink')
plt.subplot(1,2,1)
ax = plt.gca()
# ax.set_facecolor('pink')