/
customdetrend.py
628 lines (476 loc) · 21.1 KB
/
customdetrend.py
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
49
50
51
52
53
54
55
56
57
58
59
60
61
62
63
64
65
66
67
68
69
70
71
72
73
74
75
76
77
78
79
80
81
82
83
84
85
86
87
88
89
90
91
92
93
94
95
96
97
98
99
100
101
102
103
104
105
106
107
108
109
110
111
112
113
114
115
116
117
118
119
120
121
122
123
124
125
126
127
128
129
130
131
132
133
134
135
136
137
138
139
140
141
142
143
144
145
146
147
148
149
150
151
152
153
154
155
156
157
158
159
160
161
162
163
164
165
166
167
168
169
170
171
172
173
174
175
176
177
178
179
180
181
182
183
184
185
186
187
188
189
190
191
192
193
194
195
196
197
198
199
200
201
202
203
204
205
206
207
208
209
210
211
212
213
214
215
216
217
218
219
220
221
222
223
224
225
226
227
228
229
230
231
232
233
234
235
236
237
238
239
240
241
242
243
244
245
246
247
248
249
250
251
252
253
254
255
256
257
258
259
260
261
262
263
264
265
266
267
268
269
270
271
272
273
274
275
276
277
278
279
280
281
282
283
284
285
286
287
288
289
290
291
292
293
294
295
296
297
298
299
300
301
302
303
304
305
306
307
308
309
310
311
312
313
314
315
316
317
318
319
320
321
322
323
324
325
326
327
328
329
330
331
332
333
334
335
336
337
338
339
340
341
342
343
344
345
346
347
348
349
350
351
352
353
354
355
356
357
358
359
360
361
362
363
364
365
366
367
368
369
370
371
372
373
374
375
376
377
378
379
380
381
382
383
384
385
386
387
388
389
390
391
392
393
394
395
396
397
398
399
400
401
402
403
404
405
406
407
408
409
410
411
412
413
414
415
416
417
418
419
420
421
422
423
424
425
426
427
428
429
430
431
432
433
434
435
436
437
438
439
440
441
442
443
444
445
446
447
448
449
450
451
452
453
454
455
456
457
458
459
460
461
462
463
464
465
466
467
468
469
470
471
472
473
474
475
476
477
478
479
480
481
482
483
484
485
486
487
488
489
490
491
492
493
494
495
496
497
498
499
500
501
502
503
504
505
506
507
508
509
510
511
512
513
514
515
516
517
518
519
520
521
522
523
524
525
526
527
528
529
530
531
532
533
534
535
536
537
538
539
540
541
542
543
544
545
546
547
548
549
550
551
552
553
554
555
556
557
558
559
560
561
562
563
564
565
566
567
568
569
570
571
572
573
574
575
576
577
578
579
580
581
582
583
584
585
586
587
588
589
590
591
592
593
594
595
596
597
598
599
600
601
602
603
604
605
606
607
608
609
610
611
612
613
614
615
616
617
618
619
620
621
622
623
624
625
626
627
628
"""
UTF-8, Python 3
------------------
AltaiPony
------------------
Ekaterina Ilin, 2023, MIT License
This module contains custom detrending functions.
"""
import time
import copy
import numpy as np
import pandas as pd
from .altai import find_iterative_median, equivalent_duration
from .utils import sigma_clip
from .flarelc import FlareLightCurve
import astropy.units as u
from scipy.interpolate import UnivariateSpline, interp1d
from scipy import optimize
def custom_detrending(lc, spline_coarseness=30, spline_order=3,
savgol1=6., savgol2=3., pad=3, max_sigma=2.5,
longdecay=6,):
"""Custom de-trending for TESS and Kepler
short cadence light curves, including TESS Cycle 3 20s
cadence.
Parameters:
------------
lc : FlareLightCurve
light curve that has at least time, flux and flux_err
spline_coarseness : float
time scale in hours for spline points.
See fit_spline for details.
spline_order: int
Spline order for the coarse spline fit.
Default is cubic spline.
savgol1 : float
Window size for first Savitzky-Golay filter application.
Unit is hours, defaults to 6 hours.
savgol2 : float
Window size for second Savitzky-Golay filter application.
Unit is hours, defaults to 3 hours.
pad : 3
Outliers in Savitzky-Golay filter are padded with this
number of data points. Defaults to 3.
max_sigma : float
Outlier rejection threshold in sigma. Defaults to 2.5.
longdecay : int
Long decay time for outlier rejection. Defaults to 6.
Return:
-------
FlareLightCurve with detrended_flux attribute
"""
dt = np.mean(np.diff(lc.time.value))
# fit a spline to the general trends
lc1, model = fit_spline(lc, spline_order=spline_order,
spline_coarseness=spline_coarseness)
# replace for next step
lc1.flux = lc1.detrended_flux.value
# removes strong and fast variability on 5 day to 4.8 hours
# simple sines are probably because rotational variability is
# either weak and transient or strong and persistent on the timescales
lc2 = remove_sines_iteratively(lc1)
# choose a 6 hour window
w = int((np.rint(savgol1 / 24. / dt) // 2) * 2 + 1)
# use Savitzy-Golay to iron out the rest
lc3 = lc2.detrend("savgol", window_length=w, pad=pad)
# choose a three hour window
w = int((np.rint(savgol2 / 24. / dt) // 2) * 2 + 1)
# use Savitzy-Golay to iron out the rest
lc4 = lc3.detrend("savgol", window_length=w, pad=pad,
max_sigma=max_sigma,longdecay=longdecay)
# find median value
lc4 = find_iterative_median(lc4)
# replace for next step
lc4.flux = lc4.detrended_flux.value
# remove exopential fringes that neither spline,
# nor sines, nor SavGol can remove.
lc5 = remove_exponential_fringes(lc4)
return lc5
def detrend_savgol(lc, max_sigma=2.5, longdecay=6,
w=121, break_tolerance=10, **kwargs):
"""New detrending with savgol filter.
Parameters:
-----------
max_sigma: float>0
sigma clipping threshold
longdecay: int
adding masked datapoints to the tail if
multiple outliers occur in a row
w : odd int
window length for savgol filter
break_tolerance : int
If there are large gaps in time, flatten will split the flux into several sub-lightcurves and apply savgol_filter to each individually. A gap is defined as a period in time larger than break_tolerance times the median gap. To disable this feature, set break_tolerance to None.
kwargs : dict
keyword arguments to feed LightCurve.flatten()
"""
# fill missing cadences
lc = interpolate_missing_cadences(lc)
# normalize
lcn = lc.normalize()
# sigma clip
m = sigma_clip(lcn.flux.value, max_sigma=2.5, longdecay=6)
# convert bool to int
mask = ~m * 1
# from Appaloosa:
# convert mask to start and stop
reverse_counts = np.zeros_like(lcn.flux.value, dtype='int')
for k in range(2, len(lcn.flux.value)):
reverse_counts[-k] = (mask[-k]
* (reverse_counts[-(k-1)]
+ mask[-k]))
# find flare start where values in reverse_counts switch from 0 to >=N3
# SET N3=2 because we care about all longer outliers!
istart_i = np.where((reverse_counts[1:] >= 2) &
(reverse_counts[:-1] - reverse_counts[1:] < 0))[0] + 1
# use the value of reverse_counts to determine how many points away stop is
istop_i = istart_i + (reverse_counts[istart_i])
# get a list of masked candidates to extrapolate
candidates = list(zip(istart_i, istop_i))
# save the flare flux
fluxold = lcn.flux
# remove the flares candidates for now
lcn.flux[mask] = np.nan
# SAVGOL APPLIED HERE
# https://docs.lightkurve.org/reference/api/lightkurve.LightCurve.flatten.html?highlight=flatten#lightkurve.LightCurve.flatten
# flatten with light curve
# set break_tolerance to 10 by default, i.e. 20 min in a 2min cadence LC
lcrsf = lcn.flatten(window_length=w, break_tolerance=break_tolerance) #replace with 6h or 3h window
# cycle over all candidates
for i, j in candidates:
# span the data
mask_ij = np.arange(i,j)
# linearinterpolate below the flare
interpolation_ij = np.interp(lcn.time.value[mask_ij],
[lcn.time.value[i],lcn.time.value[j]],
[lcn.flux.value[i],lcn.flux.value[j]])
# plt.plot(lcn.time.value[mask], fill)
# plt.plot(lcn.time.value[mask], x)
# plt.scatter( [lcn.time.value[mask[0]],lcn.time.value[mask[-1]]],
# [lcn.flux.value[mask[0]-1],lcn.flux.value[mask[-1]+1]])
# fill in the masked data again
lcrsf.flux[mask_ij] = fluxold[mask_ij] / interpolation_ij
# deugging helper lines:
# %matplotlib inline
# plt.figure(figsize=(15,4))
# plt.plot(lcrsf.time.value, lcrsf.flux.value, color="k")
# # plt.plot(lcrsf2.time.value, lcrsf2.flux.value, color="grey")
# plt.plot(lcn.time.value, lcn.flux.value + 0.02, color="r")
# plt.scatter(lcn.time[mask].value, lcn.flux[mask].value)
# # plt.xlim(1945,1946)
# # plt.ylim(0.98,1.03)
# finally remove interpolated values
# first, set them to NaNs
lcrsf.flux[np.where(lcrsf.interpolated.value==1)[0]] = np.nan
# then remove
lcrsf = lcrsf.remove_nans()
return lcrsf
def remove_sines_iteratively(flcd, niter=5, freq_unit=1/u.day,
maximum_frequency=12.,
minimum_frequency=0.2,
max_sigma=3.5, longdecay=2):
"""Iteratively remove strong sinusoidal signal
from light curve. Each iteration calculates a Lomb-Scargle
periodogram and LSQ-fits a cosine function using the dominant
frequency as starting point.
Parameters:
------------
flcd : FlareLightCurve
light curve from which to remove
niter : int
Maximum number of iterations.
freq_unit : astropy.units
unit in which maximum_frequency and minimum_frequency
are given
maximum_frequency: float
highest frequency to calculate the Lomb-Scargle periodogram
minimum_frequency: float
lowest frequency to calculate the Lomb-Scargle periodogram
max_sigma : float
Passed to altaipony.utils.sigma_clip.
Above this value data points
are flagged as outliers.
longdecay : 2
altaipony.utils.sigma_clip expands the mask for series
of outliers by sqrt(length of series). Longdecay doubles
the mask expansion in the decay phase of what may be flares.
Return:
-------
FlareLightCurve with detrended_flux attribute
"""
# define cosine function
def cosine(x, a, b, c, d):
return a * np.cos(b * x + c) + d
# make a copy of the original LC
flcd.flux = flcd.flux.value
flcd.flux_err = flcd.flux_err.value
flct = copy.deepcopy(flcd)
# iterate over chunks
for le, ri in flct.find_gaps().gaps:
# again make a copy of the chunk to manipulate safely
flc = copy.deepcopy(flct[le:ri])
# find median of LC
flc = find_iterative_median(flc)
# mask flares
mask = sigma_clip(flc.flux.value, max_sigma=3.5, longdecay=2)
# how many data points comprise the fastest period at maximum_frequency?
full_fastest_period = 1. / maximum_frequency / np.nanmin(np.diff(flc.remove_nans().time.value))
# only remove sines if LC chunk is larger than one full period of the fastest frequency
if flc.flux.value.shape[0] > full_fastest_period:
n = 0 # start counter
snr = 3 # go into while loop at least once
# iterate while there is signal, but not more than n times
while ((snr > 1) & (n < niter)):
t = time.process_time()
# mask NaNs and outliers
cond = np.invert(np.isnan(flc.time.value)) & np.invert(np.isnan(flc.flux.value)) & mask
# calculate periodogram
pg = flc[cond].to_periodogram(freq_unit=freq_unit,
maximum_frequency=maximum_frequency,
minimum_frequency=minimum_frequency)
# fit sinusoidal
p, p_cov = optimize.curve_fit(cosine, flc.time.value[cond], flc.flux.value[cond],
p0=[np.nanstd(flc.flux.value),
2*np.pi*pg.frequency_at_max_power.value,
0, np.nanmean(flc.flux.value)], ftol=1e-6)
t1 = time.process_time()
# replace with de-trended flux but without subtracting the median
flc.flux = flc.flux.value - cosine(flc.time.value, p[0], p[1], p[2], 0.)
# update SNR
snr = pg.flatten().max_power
# bump iterator
n += 1
tf = time.process_time()
# print(snr, n, tf-t, tf-t1, t1-t)
# replace the empty array with the fitted detrended flux
flcd.detrended_flux[le:ri] = flc.flux.value
return flcd
def remove_exponential_fringes(flcd, demask=10, max_sigma=3.5, longdecay=2):
"""Remove exponential fringes from light curve chunks.
Parameters:
-----------
flcd : FlareLightCurve
Mostly de-trended light curves
with possibly fringy fringes that need a haircut.
demask : int
fraction of light curve to keep in the fit even it
deviates from the median, applied to the end and start
of each light curve chunk.
max_sigma : float
Passed to altaipony.utils.sigma_clip.
Above this value data points
are flagged as outliers.
longdecay : 2
altaipony.utils.sigma_clip expands the mask for series
of outliers by sqrt(length of series). Longdecay doubles
the mask expansion in the decay phase of what may be flares.
"""
def twoexps(x, a, b, c, d, e, f, g):
return a * np.exp(b * (c - x)) + d * np.exp(e * (f - x)) + g
flct = copy.deepcopy(flcd)
# initiate a detrended flux array
flct.detrended_flux = np.full_like(flct.flux.value, np.nan)
for le, ri in flct.find_gaps().gaps:
f_ = copy.deepcopy(flct[le:ri])
# mask outliers
mask = sigma_clip(f_.flux.value, max_sigma=max_sigma, longdecay=longdecay)
ff = f_[mask]
# get the median as a guess for the least square fit
median = np.nanmedian(ff.it_med.value)
# get noise level from the fully
std = np.nanstd(ff.flux.value)
# demask the fringes because they are otherwise likely to be
# masked by sigma clipping
mask[:len(f_.flux.value) // demask] = 1
mask[-len(f_.flux.value) // demask:] = 1
ff = f_[mask]
# get the amplitude of the fringes
sta, fin = ff.flux.value[0] - median, ff.flux.value[-1] - median
# don't fit the fringes if they not even there
# i.e. smaller than global noise of outlier-free LC
noleft = np.abs(sta) < std
noright = np.abs(fin) < std
# adjust the LSQ function to number of fringes
# also fix time offset
# only end of LC chunk fringes
if (not noright) & (noleft):
def texp(x, d, e, g):
return twoexps(x, 0., 0., 0., d, e, ff.time.value[-1], g)
p0 = [fin, -10., median]
# only start of LC chunk fringes
if (not noleft) & (noright):
def texp(x, a, b, g):
return twoexps(x, a, b, ff.time.value[0], 0., 0., 0., g)
p0 = [sta, 10., median]
# no fringes at all
if (noleft) & (noright):
def texp(x, g):
return twoexps(x, 0., 0., 0., 0., 0., 0., g)
p0 = [median]
# both sides of LC chunk fringe
if (not noleft) & (not noright):
def texp(x, a, b, d, e, g):
return twoexps(x, a, b, ff.time.value[0], d, e, ff.time.value[-1], g)
p0 = [sta, 10., fin, -10., median]
# do the LSQ fit
p, p_cov = optimize.curve_fit(texp, ff.time.value, ff.flux.value,
p0=p0, sigma=np.full_like(ff.flux.value, std),
absolute_sigma=True, ftol=1e-6)
# Remove the fit from the LC
# median + full flux - model
nflux = p[-1] + ff.flux.value - texp(ff.time.value, *p)
# replace NaNs in detrended flux with solution
flcd.detrended_flux[le:ri][mask] = nflux
# re-introduce outliers and flare candidates
flcd.detrended_flux[le:ri][~mask] = flcd.flux[le:ri][~mask].value
return flcd
def estimate_detrended_noise(flc, mask_pos_outliers_sigma=2.5,
std_window=100, ):
flcc = copy.deepcopy(flc)
flcc = flcc.find_gaps()
for (le, ri) in flcc.gaps:
flcd = copy.deepcopy(flcc[le:ri])
mask = sigma_clip(flcd.detrended_flux.value, max_sigma=mask_pos_outliers_sigma, longdecay=2)
flcd.detrended_flux[~mask] = np.nan
# apply rolling window std and interpolate the masked values
flcd.detrended_flux_err[:] = pd.Series(flcd.detrended_flux.value).rolling(std_window,
center=True,
min_periods=1).std().interpolate().values
# and refine it:
flcd = find_iterative_median(flcd)
# make a copy first
filtered = copy.deepcopy(flcd.detrended_flux.value)
# get right bound of flux array
tf = filtered.shape[0]
# pick outliers
mask = sigma_clip(filtered, max_sigma=mask_pos_outliers_sigma, longdecay=2)
filtered[~mask] = np.nan
# apply rolling window std and interpolate the masked values
flcc.detrended_flux_err[le:ri]= pd.Series(filtered).rolling(std_window,
center=True,
min_periods=1).std().interpolate().values
# make it a series again so that formatting is consistent
flcc.detrended_flux_err = pd.Series(flcc.detrended_flux_err)
return flcc
def fit_spline(flc, spline_coarseness=30, spline_order=3):
"""Do a spline fit on a coarse sampling of data points.
Parameters:
------------
flc : FlareLightCurve
spline_coarseness : int
spline_order : int
order of spline fit
Return:
--------
FlareLightCurve with new flux attribute
"""
flc = flc[np.where(np.isfinite(flc.flux.value))]
flcp = copy.deepcopy(flc)
flcp = flcp.find_gaps()
flux_med = np.nanmedian(flcp.flux.value)
n = int(np.rint(spline_coarseness /
24 /
(flcp.time.value[1] - flcp.time.value[0]))) #default 30h window
k = spline_order
# print(n)
#do a first round
model = np.full_like(flcp.flux.value, np.nan)
for le, ri in flcp.gaps:
rip = flcp.flux[le:ri].value.shape[0] + le
t, f = np.zeros((rip - le)//n+2), np.zeros((rip - le)//n+2)
if (rip - le)//n == 0:
flcp.detrended_flux[le:ri] = flcp.flux.value[le:ri]
elif (rip - le)//n > 0:
news, news_mod = (rip - le)//n, (rip - le)%n
t[1:-1] = np.mean(flcp.time.value[le:rip - news_mod].reshape(news, n), axis=1)
f[1:-1] = np.median(flcp.flux.value[le:rip - news_mod].reshape(news, n), axis=1)
t[0], t[-1] = flcp.time.value[le], flcp.time.value[rip-1]
f[0], f[-1] = flcp.flux.value[le], flcp.flux.value[rip-1]
# if the LC chunk is too short, skip spline fit
if t.shape[0] <= k:
flcp.detrended_flux[le:ri] = flcp.flux.value[le:ri]
# otherwise fit a spline
else:
p3 = UnivariateSpline(t, f, k=k, s=0)
flcp.detrended_flux[le:ri] = flcp.flux.value[le:ri] - p3(flcp.time.value[le:ri]) + flux_med
model[le:ri] = p3(flcp.time.value[le:ri])
return flcp, model
def measure_flare(flc, sta, sto):
"""Give start and stop indices into a de-trended
light curve, calculate flare properties assuming that
what's inbetween is a flares, and add the result
to FlareLightCurve.flares.
Parameters:
-------------
flc : FlareLightCurve
de-trended light curve
sta : int
start index of flare
sto : int
stop index of flare
"""
# get ED
ed_rec, ed_rec_err = equivalent_duration(flc, sta, sto, err=True)
# get amplitude
ampl_rec = np.max(flc.detrended_flux.value[sta:sto]) / flc.it_med.value[sta] - 1.
# get cadence numberspip l
cstart = flc.cadenceno.value[sta]
cstop = flc.cadenceno.value[sto]
# get time stamps
tstart = flc.time.value[sta]
tstop = flc.time.value[sto]
# add result to flare table
newline = pd.Series(
{'ed_rec': ed_rec,
'ed_rec_err': ed_rec_err,
'ampl_rec': ampl_rec,
'istart': sta,
'istop': sto,
'cstart': cstart,
'cstop': cstop,
'tstart': tstart,
'tstop': tstop,
'dur': tstop - tstart,
'total_n_valid_data_points': flc.flux.value.shape[0]
})
flc.flares = pd.concat([flc.flares, newline.to_frame().T], ignore_index=True)
return
def interpolate_missing_cadences(lc, **kwargs):
"""Interpolate missing cadences in
light curve, skipping larger gaps in data.
Parameters:
-----------
lc : FlareLightCurve
the light curve
kwargs : dict
keyword arguments to pass to find_gaps method
Return:
-------
interpolated FlareLightCurve
"""
# find gaps that are too big to be interpolated with a good conscience
gaps = lc.find_gaps().gaps
# set up interpolated array
time, flux, flux_err, newcadence = [], [], [], []
# interpolate within each gap
for i, j in gaps:
# select gap
gaplc = lc[i:j]
# get old cadence
oldx = gaplc.cadenceno.value
# cadenceno are complete in uncorrected flux,
# so we fill in the removed cadences
newx = np.arange(gaplc.cadenceno.value[0], gaplc.cadenceno.value[-1])
newcadence.append(newx)
# interpolate flux error
f = interp1d(oldx, gaplc.flux_err.value)
flux_err.append(f(newx))
# interpolate time
f = interp1d(oldx, gaplc.time.value)
time.append(f(newx))
# interpolate flux
f = interp1d(oldx, gaplc.flux.value)
flux.append(f(newx))
# stitch together new light curve
newlc = FlareLightCurve(time=np.concatenate(time),
flux=np.concatenate(flux),
flux_err=np.concatenate(flux_err),
targetid=lc.targetid)
# add new cadence array
newcadenceno = np.concatenate(newcadence)
newlc["cadenceno"] = newcadenceno
# flag values that have been interpolated in the new light curve
newvals = np.sort(list(set(newcadenceno) - set(lc.cadenceno.value)))
newvalindx = np.searchsorted(newcadenceno, newvals)
newlc["interpolated"] = 0 # not interpolated values
newlc.interpolated[newvalindx] = 1 # interpolated values
return newlc