2.3 Data Storage Requirements

The sizes of WFC3 data files (in MB) are given in Table 2.7. The following assumptions were made when calculating these sizes:

the ERR, DQ, SAMP, and TIME arrays are null in the raw files,
the SAMP and TIME arrays are null in the ima files,
IR images have the maximum of 16 MultiAccum readouts, and
images are full-frame and unbinned.

Table 2.7: Sizes of WFC3 data files.

Channel	Size of FITS file
	raw	ima	cal	drizzled
UVIS	35 MB		168 MB	217 MB
IR	34 MB	168 MB	17 MB	13 MB

The size of the drizzled image (_drz) is for a single image that is drizzled only for the purpose of performing geometric corrections and for combining the two UVIS chips. It assumes that the input and output image pixels are approximately the same size (drizzle scale parameter is 1.0).

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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

2.3 Data Storage Requirements

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