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Kepler Guest Observer Program

PyKE Primer - 7. Walk-through Examples

PyKE is a suite of python software tools developed to reduce and analyze Kepler light curves, TPFs, and FFIs. PyKE tools provide the user with flexibility to tune pixel extraction and artifact mitigation for the scientific potential of individual target data. These examples provide use cases and reduction examples for the reader to follow. Data users are encouraged to experiment with the tunable input parameters for each tool. The procedures outlined in this section will not be optimal for all science, and it will ultimately be up to the user to determine what parameter values optimize scientific return.

PyKE tasks can be called and controlled i) directly from the command line within the PyRAF environment, ii) entirely through GUI-driven operation using the epar function on the command line within the PyRAF environment, or iii) as standalone python scripts called from the command line of a unix/linux shell. For the sake of clarity in these walkthroughs, we provide uniformly the PyRAF GUI task invocations. To get started on each walkthrough - in an xterm (not an OS X terminal window), run the following command in the directory where you have downloaded your Kepler data:
   % mkiraf
setting the terminal type to xterm when asked. Then startup PyRAF and load the PyKE tools in the Kepler package by entering the following commands
   % pyraf
      --> kepler
To execute any task in GUI mode, type epar <taskname>, e.g.
      --> epar kepdraw

  1. Extract and cotrend new light curves from Target Pixel Files
  2. Mitigate motion and focus artifacts by redefining the optimal aperture
  3. Subjective light curve cotrending using basis vectors
  4. Removing stellar astrophysics and quarter stitching
  5. Mitigate motion artifacts by correlating detrended flux with target centroids

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Editor: Martin Still
NASA Official: Jessie Dotson
Last Updated: Jan 11, 2013
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