Correcting systematics#
Telescope data is always affected by noise contributed by the instrument.
The lightkurve.correctors
sub-package provides classes which offer
different strategies to remove such noise.
At the core of the package lies the generic RegressionCorrector
class.
It uses linear regression to correlate a light curve against a DesignMatrix
of column vectors which are known to correlate with additive noise components.
The CBVCorrector
, PLDCorrector
, and SFFCorrector
classes extend RegressionCorrector
by providing the user with pre-configured DesignMatrix
objects which are
known to be effective at removing different types of noise.
Cotrending Basis Vectors (CBV)#
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Loads TESS cotrending basis vectors, either from a directory of CBV files already saved locally if cbv_dir is passed, or else will retrieve the relevant files programmatically from MAST. |
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Loads Kepler or K2 cotrending basis vectors, either from a local directory cbv_dir or searches the public data archive at MAST <https://archive.stsci.edu>. |
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Class for removing systematics using Cotrending Basis Vectors (CBVs) from Kepler/K2/TESS. |
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Optimizes the correction by adjusting the L2-Norm (Ridge Regression) regularization penalty term, alpha, based on the introduced noise (over-fitting) and residual correlation (under-fitting) goodness metrics. |
Returns diagnostic plots to assess the most recent correction. |
Pixel Level Decorrelation (PLD)#
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Implements the Pixel Level Decorrelation (PLD) systematics removal method. |
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Returns a systematics-corrected light curve. |
Returns diagnostic plots to assess the most recent call to |
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Show different aperture masks used by PLD in the most recent call to |
Self Flat Fielding (SFF)#
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Special case of |
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Find the best fit correction for the light curve. |
Returns a diagnostic plot which visualizes what happened during the most recent call to |
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Returns a diagnostic plot which visualizes arclength vs flux from most recent call to |
Regression Corrector#
Remove noise using linear regression against a |
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Find the best fit correction for the light curve. |
Returns diagnostic plots to assess the most recent call to |
Creating a design matrix#
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A matrix of column vectors for use in linear regression. |
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Object which stores multiple design matrices. |
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A matrix of column vectors for use in linear regression. |
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A set of design matrices. |
A DesignMatrix has the following attributes:
Design matrix "X" to be used in RegressionCorrector objects |
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Matrix rank computed using |
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Tuple specifying the shape of the matrix as (n_rows, n_columns). |
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2D numpy array containing the matrix values. |
A DesignMatrix supports the following operations:
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Returns a new |
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Join two designmatrices, return a design matrix collection |
Returns a deepcopy of DesignMatrix |
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Returns a new |
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Visualize the design matrix values as an image. |
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Visualize the coefficient priors. |
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Returns a new |
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Returns a new |
Convert this dense matrix object to a |
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Emits |
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Abstract base class documenting the required structure of classes designed to remove systematic noise from light curves. |
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Returns a |
Returns plots which elucidate the most recent call to |