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An initial, coarse correction lightcurve will be produced and provided alongside each lightcurve extracted from the raw photometry. The ensemble correction method used is detailed here
The resulting ensemble fit curve for each target will also be provided for reference. The lightcurve correction code is available on github
An overview of the ensemble fitting is illustrated in the flowchart on the TASOC wiki page. Results of initial testing on simulated data are available at the TASOC wiki page.
In keeping with the Kepler lightcurve correction methods, CBVs will be provided for each CCD after the raw photometry targets have been processed. Additional area-defined CBVs will be provided for each CCD to reduce unintended fitting biases across the larger detector and attempt to capture localized focus effects.
Additional lightcurve corrections and data products may be provided based on working group feedback and requirements for automatic stellar classification.