8.4 References

Bergeron, L. E. and Dickinson, M. E. 2003, Removal of Cosmic Ray persistence from Science Data using the Post-SAA Darks, NICMOS ISR 2003-010

Dahlen, T., 2013, WFC3/IR Internal Flat Fields, WFC3 ISR 2013-04

Hilbert, B. and Petro, L., 2012, WFC3/IR Dark Current Stability, WFC3 ISR 2012-11.

Hilbert, B., 2012, WFC3/IR Reference Pixel Characterization #1: Comparison of Bias Subtraction Methods, WFC3 ISR 2012-05.

Hilbert, B and McCullough, P., 2010, WFC3 SMOV Results: IR Channel Dark Current, Readnoise, and Background Signal, WFC3 ISR 2009-21.

Long, K., S. Baggett, S.M., MacKenty, J.W., and Riess, A.G., 2012, Characterizing persistence in the IR detector within the Wide Field Camera 3 instrument on the Hubble Space Telescope, Proceedings of the SPIE, 8442, 84421W-9

Long, K. S., Baggett, S. M., and MacKenty, J. W. 2013a, Characterizing Persistence in the WFC3 IR Channel: Finite Trapping Times, WFC3 ISR 2013-06

Long, K. S., Baggett, S. M., and MacKenty, J. W. 2013b, Characterizing Persistence in the WFC3 IR Channel: Observations of Omega Cen, WFC3 ISR 2013-07

Long, K. S. 2013, Characterizing Persistence in the WFC3 IR Channel: A revised model, WFC3 ISR 2013-08

Long, L.S, Baggett S.M., and MacKenty, J.W., Persistence in the WFC3 IR Detector: Spatial Variations, WFC3 ISR 2015-16

Robberto, M., C. Hanley, and I. Dashevsky, 2002, The reference pixels on the WFC3 IR detectors, WFC3 ISR 2002-06.

Smith, R.M., Zavodny, M., Rahmer, G. and Bonati, M., 2008a, A theory for image persistence in HgCdTe photodiodes, Proceedings of the SPIE, 7021, 70210J-1

Smith, R. M., Zavodny, M., Rahmer, G., Bonati, M., 2008b, Calibration of image persistence in HgCdTe photodiodes, Proceedings of the SPIE, 7021, 70210K-1

Sunnquist,B., Mack,J., Khandrika, H., Asteroids in the WFC3/IR Frontier Fields Images, WFC3 ISR 2017-18

Thatte, D., Dahlen, T. et al., 2009, NICMOS Data Handbook, version 8.0, pg 1.

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WFC3 Data Handbook
- • Acknowledgments
- Preface
  - • Handbook Structure
  - • Typographic Conventions
- Chapter 1: WFC3 Instruments
  - • 1.1 Instrument Overview
  - • 1.2 The UVIS Channel
  - • 1.3 The IR Channel
- Chapter 2: WFC3 Data Structure
  - • 2.1 Types of WFC3 Files
  - • 2.2 WFC3 File Structure
  - • 2.3 Data Storage Requirements
  - • 2.4 Headers and Keywords
- Chapter 3: WFC3 Data Calibration
  - • 3.1 The calwf3 Data Processing Pipeline
  - • 3.2 UVIS Data Calibration Steps
  - • 3.3 IR Data Calibration Steps
  - • 3.4 Pipeline Tasks
  - • 3.5 Manual Recalibration of WFC3 Data
- Chapter 4: WFC3 Images: Distortion Correction and AstroDrizzle
- Chapter 5: WFC3-UVIS Sources of Error
  - • 5.1 Gain and Read Noise
  - • 5.2 Bias Subtraction
  - • 5.3 Dark Current and Hot Pixels
  - • 5.4 UVIS Flat Fields
  - • 5.5 Image Anomalies
  - • 5.6 Generic Detector and Camera Properties
  - • 5.7 UVIS Photometry Errors
  - • 5.8 WFC3 References
- Chapter 6: WFC3 UVIS Charge Transfer Efficiency - CTE
  - • 6.1 Overview
  - • 6.2 CTE Losses And Background
  - • 6.3 The Nature Of CTE Losses
  - • 6.4 The Pixel-Based Model
  - • 6.5 Empirical Corrections
  - • 6.6 Dealing With CTE Losses in WFC3 UVIS Images
  - • 6.7 Sink Pixels
  - • 6.8 References
- Chapter 7: WFC3 IR Sources of Error
  - • 7.1 WFC3 IR Error Source Overview
  - • 7.2 Gain
  - • 7.3 WFC3 IR Bias Correction
  - • 7.4 WFC3 Dark Current and Banding
  - • 7.5 Blobs
  - • 7.6 Detector Nonlinearity Issues
  - • 7.7 Count Rate Non-Linearity
  - • 7.8 IR Flat Fields
  - • 7.9 Pixel Defects and Bad Imaging Regions
  - • 7.10 Time Variable Background Contamination
  - • 7.11 IR Photometry Errors
  - • 7.12 References
- Chapter 8: Persistence in WFC3 IR
- Chapter 9: WFC3 Data Analysis
  - • 9.1 WFC3 Data Analysis
  - • 9.2 Astrometry
  - • 9.3 Spectroscopy
  - • 9.4 STSDAS and STSCI_PYTHON Software
  - • 9.5 Specific Tools for the Analysis of WFC3
  - • 9.6 References
- Chapter 10: WFC3 Spatial Scan Data
  - • 10.1 Analysis of Scanned Data
  - • 10.2 IR Scanned Data
  - • 10.3 UVIS Scanned Data
  - • 10.4 References

8.4 References

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