9.4 STSDAS, STSCI_PYTHON and Astropy

STSCI/IRAF has been deprecated as described in the 2018 STScI Newsletter. To ease this transition for long-time IRAF users, a number of IRAF routines have been ported to python and documented via a set of Jupyter Notebook Tutorials, located in a Central Repository. The WFC3 team continues to develop tools aimed at the user community. New tools will continue to be added. We note that many of the software tools that are useful for analyzing HST data can now be found in the Astropy (the current community-supported Python Astronomy package) library of python modules.

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WFC3 Data Handbook
- • Acknowledgments
- • What's New in This Revision
- 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 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
  - • 7.11 IR Photometry Errors
  - • 7.12 References
- Chapter 8: Persistence in WFC3 IR
- Chapter 9: WFC3 Data Analysis
  - • 9.1 Photometry
  - • 9.2 Astrometry
  - • 9.3 Spectroscopy
  - • 9.4 STSDAS, STSCI_PYTHON and Astropy
  - • 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

9.4 STSDAS, STSCI_PYTHON and Astropy

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