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test_synthetic_data.py
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test_synthetic_data.py
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"""Use synthetic data to verify lightkurve detrending and signal recovery.
"""
from __future__ import division, print_function
from astropy.utils.data import get_pkg_data_filename
from astropy.stats.bls import BoxLeastSquares
import numpy as np
import pytest
from scipy import stats
from lightkurve.targetpixelfile import KeplerTargetPixelFile
from lightkurve.correctors import SFFCorrector, PLDCorrector
# See `data/synthetic/README.md` for details about these synthetic test files
filename_synthetic_sine = get_pkg_data_filename(
"data/synthetic/synthetic-k2-sinusoid.targ.fits.gz"
)
filename_synthetic_transit = get_pkg_data_filename(
"data/synthetic/synthetic-k2-planet.targ.fits.gz"
)
filename_synthetic_flat = get_pkg_data_filename(
"data/synthetic/synthetic-k2-flat.targ.fits.gz"
)
def test_sine_sff():
"""Can we recover a synthetic sine curve using SFF and LombScargle?"""
# Retrieve the custom, known signal properties
tpf = KeplerTargetPixelFile(filename_synthetic_sine)
true_period = np.float(tpf.hdu[3].header["PERIOD"])
true_amplitude = np.float(tpf.hdu[3].header["SINE_AMP"])
# Run the SFF algorithm
lc = tpf.to_lightcurve()
corrector = SFFCorrector(lc)
cor_lc = corrector.correct(
tpf.pos_corr2,
tpf.pos_corr1,
niters=4,
windows=1,
bins=7,
restore_trend=True,
timescale=0.5,
)
# Verify that we get the period within ~20%
pg = cor_lc.to_periodogram(
method="lombscargle", minimum_period=1, maximum_period=10, oversample_factor=10
)
ret_period = pg.period_at_max_power.value
threshold = 0.2
assert (ret_period > true_period * (1 - threshold)) & (
ret_period < true_period * (1 + threshold)
)
# Verify that we get the amplitude to within 10%
n_cad = len(tpf.time)
design_matrix = np.vstack(
[
np.ones(n_cad),
np.sin(2.0 * np.pi * cor_lc.time.value / ret_period),
np.cos(2.0 * np.pi * cor_lc.time.value / ret_period),
]
).T
ATA = np.dot(design_matrix.T, design_matrix / cor_lc.flux_err[:, None] ** 2)
least_squares_coeffs = np.linalg.solve(
ATA, np.dot(design_matrix.T, cor_lc.flux / cor_lc.flux_err ** 2)
)
const, sin_weight, cos_weight = least_squares_coeffs
fractional_amplitude = (sin_weight ** 2 + cos_weight ** 2) ** (0.5) / const
assert (fractional_amplitude > true_amplitude / 1.1) & (
fractional_amplitude < true_amplitude * 1.1
)
def test_transit_sff():
"""Can we recover a synthetic exoplanet signal using SFF and BLS?"""
# Retrieve the custom, known signal properties
tpf = KeplerTargetPixelFile(filename_synthetic_transit)
true_period = np.float(tpf.hdu[3].header["PERIOD"])
true_rprs = np.float(tpf.hdu[3].header["RPRS"])
true_transit_lc = tpf.hdu[3].data["NOISELESS_INPUT"]
max_depth = 1 - np.min(true_transit_lc)
# Run the SFF algorithm
lc = tpf.to_lightcurve().normalize()
corrector = SFFCorrector(lc)
cor_lc = corrector.correct(
tpf.pos_corr2,
tpf.pos_corr1,
niters=4,
windows=1,
bins=7,
restore_trend=False,
timescale=0.5,
)
# Verify that we get the transit period within 5%
pg = cor_lc.to_periodogram(
method="bls",
minimum_period=1,
maximum_period=9,
frequency_factor=0.05,
duration=np.arange(0.1, 0.6, 0.1),
)
ret_period = pg.period_at_max_power.value
threshold = 0.05
assert (ret_period > true_period * (1 - threshold)) & (
ret_period < true_period * (1 + threshold)
)
# Verify that we get the transit depth in expected bounds
assert (pg.depth_at_max_power >= true_rprs ** 2) & (
pg.depth_at_max_power < max_depth
)
def test_transit_pld():
"""Can we recover a synthetic exoplanet signal using PLD and BLS?"""
# Retrieve the custom, known signal properties
tpf = KeplerTargetPixelFile(filename_synthetic_transit)
true_period = np.float(tpf.hdu[3].header["PERIOD"])
true_rprs = np.float(tpf.hdu[3].header["RPRS"])
true_transit_lc = tpf.hdu[3].data["NOISELESS_INPUT"]
max_depth = 1 - np.min(true_transit_lc)
# Run the PLD algorithm on a first pass
corrector = PLDCorrector(tpf)
cor_lc = corrector.correct()
pg = cor_lc.to_periodogram(
method="bls",
minimum_period=1,
maximum_period=9,
frequency_factor=0.05,
duration=np.arange(0.1, 0.6, 0.1),
)
# Re-do PLD with the suspected transits masked
cor_lc = corrector.correct(cadence_mask=~pg.get_transit_mask()).normalize()
pg = cor_lc.to_periodogram(
method="bls",
minimum_period=1,
maximum_period=9,
frequency_factor=0.05,
duration=np.arange(0.1, 0.6, 0.1),
)
# Verify that we get the period within ~5%
ret_period = pg.period_at_max_power.value
threshold = 0.05
assert (ret_period > true_period * (1 - threshold)) & (
ret_period < true_period * (1 + threshold)
)
# Verify that we get the transit depth in expected bounds
assert (pg.depth_at_max_power >= true_rprs ** 2) & (
pg.depth_at_max_power < max_depth
)
def test_sine_pld():
"""Can we recover a synthetic sine wave using PLD and LombScargle?"""
# Retrieve the custom, known signal properties
tpf = KeplerTargetPixelFile(filename_synthetic_sine)
true_period = np.float(tpf.hdu[3].header["PERIOD"])
true_amplitude = np.float(tpf.hdu[3].header["SINE_AMP"])
# Run the PLD algorithm
corrector = tpf.to_corrector("pld")
cor_lc = corrector.correct()
# Verify that we get the period within ~20%
pg = cor_lc.to_periodogram(
method="lombscargle", minimum_period=1, maximum_period=10, oversample_factor=10
)
ret_period = pg.period_at_max_power.value
threshold = 0.2
assert (ret_period > true_period * (1 - threshold)) & (
ret_period < true_period * (1 + threshold)
)
# Verify that we get the amplitude to within 20%
n_cad = len(tpf.time)
design_matrix = np.vstack(
[
np.ones(n_cad),
np.sin(2.0 * np.pi * cor_lc.time.value / ret_period),
np.cos(2.0 * np.pi * cor_lc.time.value / ret_period),
]
).T
ATA = np.dot(design_matrix.T, design_matrix / cor_lc.flux_err[:, None] ** 2)
least_squares_coeffs = np.linalg.solve(
ATA, np.dot(design_matrix.T, cor_lc.flux / cor_lc.flux_err ** 2)
)
const, sin_weight, cos_weight = least_squares_coeffs
fractional_amplitude = (sin_weight ** 2 + cos_weight ** 2) ** (0.5) / const
assert (fractional_amplitude > true_amplitude / 1.1) & (
fractional_amplitude < true_amplitude * 1.1
)
def test_detrending_residuals():
"""Test the detrending residual distributions"""
# Retrieve the custom, known signal properties
tpf = KeplerTargetPixelFile(filename_synthetic_flat)
# Run the SFF algorithm
lc = tpf.to_lightcurve()
corrector = SFFCorrector(lc)
cor_lc = corrector.correct(
tpf.pos_corr2, tpf.pos_corr1, niters=10, windows=5, bins=7, restore_trend=True
)
# Verify that we get a significant reduction in RMS
cdpp_improvement = lc.estimate_cdpp() / cor_lc.estimate_cdpp()
assert cdpp_improvement > 10.0
# The residuals should be Gaussian-"ish"
# Table 4.1 of Ivezic, Connolly, Vanerplas, Gray 2014
anderson_threshold = 1.57
resid_n_sigmas = (cor_lc.flux - np.mean(cor_lc.flux)) / cor_lc.flux_err
A_value, _, _ = stats.anderson(resid_n_sigmas)
assert A_value ** 2 < anderson_threshold
n_sigma = np.std(resid_n_sigmas)
assert n_sigma < 2.0
corrector = tpf.to_corrector("pld")
cor_lc = corrector.correct(restore_trend=False)
cdpp_improvement = lc.estimate_cdpp() / cor_lc.estimate_cdpp()
assert cdpp_improvement > 10.0
resid_n_sigmas = (cor_lc.flux - np.mean(cor_lc.flux)) / cor_lc.flux_err
A_value, crit, sig = stats.anderson(resid_n_sigmas)
assert A_value ** 2 < anderson_threshold
n_sigma = np.std(resid_n_sigmas)
assert n_sigma < 2.0
def test_centroids():
"""Test the estimate centroid method."""
for fn in (
filename_synthetic_sine,
filename_synthetic_transit,
filename_synthetic_flat,
):
tpf = KeplerTargetPixelFile(fn)
xraw, yraw = tpf.estimate_centroids()
xnorm = xraw - np.median(xraw)
ynorm = yraw - np.median(yraw)
xposc = tpf.pos_corr2 - np.median(tpf.pos_corr2)
yposc = tpf.pos_corr1 - np.median(tpf.pos_corr1)
rmax = np.max(np.sqrt((xnorm.value - xposc) ** 2 + (ynorm.value - yposc) ** 2))
# The centroids should agree to within a hundredth of a pixel.
assert rmax < 0.01