1. JWST Time-Series Pipeline Nikole K. Lewis STScI

2. Data Pipeline for Transiting Exoplanets The foundation for the Spitzer and Hubble data pipelines were put in place well before the discovery of the first transiting exoplanet in 2000. – Most transiting exoplanet observers start with raw or basic calibrated data and use homegrown code. – Spitzer has dedicated a fair amount of effort in recent years to supporting time-series observations. JWST must provide a data pipeline and data products that support the needs of time-series observations!

3. Time-Series Pipeline Ground Rules: – Don’t apply any corrections that can’t easily be undone such that sensitivity of the solution to the correction can be tested. – Flag, but do not correct, questionable data. – Absolute calibration is not required. – Model-based corrections should be viewed with caution. – Because of long temporal baseline, much ‘self- calibration’ can be performed. – Data products should not represent averages of individual frames/ramps or a sum over the entire exposure.

4. ‘Vanilla’ Time-Series NIR Spectroscopic Pipeline Raw Integrations Level 1B Ramps to Slopes Level 2A Photometric/Spectral Extraction Level 2B Level 3 ‘Drizzle’ Products

5. TSO Pipeline: Level 1B Raw Integrations Pipeline StepsData Products Raw Integrations Level 2A

6. TSO Pipeline: Level 2A Mask Bad PixelsSaturation CheckSubtract Super BiasReference Pixel CorrectionApply linearity correctionSubtract DarkJump Detection/Fit the ramp Calibrated Ramps (ADU) DQ 2D array Calibrated Ints. (ADU/s) 2D Pixel Saturation Limit 2D Super Bias Mean Ref Pix Val 3D Coefficients 3D Dark Frame Algorithms

7. TSO Pipeline: The IPC Correction What is the IPC Correction? The IPC correction violates the following ground rules for the TSO pipeline: – Don’t apply any corrections that can’t easily be undone such that sensitivity of the solution to the correction can be tested. TSO pipeline requires non-IPC corrected reference files

8. TSO Pipeline: Saturation Ground Rule: Flag, but do not correct, questionable data. Many transiting exoplanet observers will push on saturation limits to access brightest host stars and achieve the highest SNR. Need to advise on potential corrections beyond nominal half-well limit. Saturation Check DQ 2D array 2D Pixel Saturation Limit

9. TSO Pipeline: Bias Subtraction Subtractive steps are important in setting the appropriate relative flux level. Non-IPC corrected bias frames should be used (~1% percent difference, Gaussian noise) Subtract Super Bias 2D Super Bias

10. Many transiting exoplanet observations will be taken with small subarrays that do not incorporate many/any reference pixels. In small sample case, simple mean of the reference pixels should be removed. – More complicated schemes are difficult to reverse/track effect of during analysis. TSO Pipeline: Reference Pixel Correction/ Bias Drift Reference Pixel Correction Mean Ref Pix Val

11. A necessary evil. Needed to avoid under/overestimating the magnitude of relative features in time-series data. User will need to consider propagating uncertainties in correction into final results. TSO Pipeline: Non-Linearity Correction Apply linearity correction 3D Coefficients

12. TSO Pipeline: Dark Subtraction Subtractive steps important to set relative flux level. Non-IPC corrected dark frames should be used. – Correlated noise in difference between IPC and non- IPC darks (~5% effect) Calibrated ramps are an extremely useful data product that many will use as analysis starting point (basic calibrated data). Subtract Dark Calibrated Ramps (ADU) 3D Dark Frame

13. Observations of bright host stars will necessitate the use of a small number of groups. – Limited jump detection with nominal methods Could use deviations in PSF shape or temporal stack – Small sample for ramp fitting, instead use simple ‘last minus first’ methodology to set ADU/s TSO Pipeline: Sample up the Ramp Jump Detection/Fit the ramp Calibrated Ints. (ADU/s) Algorithms

14. TSO Pipeline: Level 2B Calibrated Ints. (ADU/s) Background/sky subtractionWavelength CalibrationSensitivity/Flat CorrectionSpectral Extraction Sigma Clip + Hist Algorithms 2/3D Flat ‘Frame’ Algorithms Sky/Background Value (ADU/s) 2D wavelength map per Int. Calibrated Ints (ADU/s) Spectral Orders per Integration

15. TSO Pipeline: Background Subtraction Remember subtractive steps are important. Serves as a catch-all (sky, remaining bias/dark offsets, etc.) Current methodology uses single value, may need to evolve to deal with ‘striping’. Background/sky subtraction Sigma Clip + Hist Sky/Background Value (ADU/s)

16. Optimal wavelength calibration procedures will vary based on instrument. Stellar spectrum may provide additional information to the user. – WFC3 observations of transiting exoplanets were used to refine the wavelength solution (e.g. Wilkins et al. (2011)). TSO Pipeline: Wavelength Calibration Wavelength Calibration Algorithms 2D wavelength map per Int.

17. Possibly an unnecessary step since division steps will not affect relative measurements. Potential drifts in stellar centroid/trace will necessitate this correction. Wavelength dependence is important! TSO Pipeline: Sensitivity/Flat Correction Sensitivity/Flat Correction 2/3D Flat ‘Frame’ Calibrated Ints (ADU/s)

18. Spectral extraction methodologies/algorithms will be instrument specific. Simple extraction methods that provide easy traceability/replication are best for pipeline. Uncertainties will need to be flagged. TSO Pipeline: Spectral Extraction Spectral Extraction Algorithms Spectral Orders per Integration

19. TSO Pipeline: Quick-look Data Products Stacking data into a single product for the entire exposure is of little utility (no drizzle). Simply summing across all wavelengths and presenting relative ADU/s as a function of time is far more useful. White Light Curve (function of time) Spectral Orders per Integration

20. Time tagging What sets limits on accuracy of time tags? – 10 microsecond precision on frame time – Onboard time tags (UTC) are generated every 10.74 s, with 64 ms accuracy – Corrections to onboard clock can be applied on 12hr contact intervals. Linear corrections applied on 1.024 s intervals ( with 0.5 ms accuracy). Onboard clock cannot drift by more than 1 s from true UTC time in 24 hour period (requirement and likely worse case scenario) TSO Time Tagging and Fits File Formatting Module

21. Time tagging Bottom line: 64 ms onboard clock sampling rate is limiter to time-tagging accuracy. Time-tags will be associated with each ‘group’ in data products and available in several flavors (BJD_TT, HJD). TSO Time Tagging and Fits File Formatting Module

22. Fits File Formatting Current plan is to deliver one fits file per exposure w/time-tags as an extension (ala Kepler). For 2 day long exposure each fits file would be 35 GB and level 1-3 data products would be on the order of 180 GB. For a more nominal transit observation each fits file would be on the order of a few GB. TSO Time Tagging and Fits File Formatting Module

23. Key Take Away Points Efforts are currently underway to construct a ‘Vanilla’ TSO pipeline that will generate data products of the most utility for time-series observations. Current plan is for the Pipeline (python code) to be available for download to allow reprocessing of data. Additional tools/resources will be available for necessary ‘non-pipeline’ processing.