E.8 The Cycle 21 Calibration Plan

The Cycle 21 calibration plan is summarized in WFC3 ISR 2014-07. It was executed from November 2013 through October 2014.

The calibration programs comprising this plan are listed in Table E.9. The proposals and observation dates can be viewed by entering the Proposal ID into the HST Program Information webpage.

The Cycle 21 calibration plan was designed to:

continue to maintain and update the standard reference files (biases, darks, linearity, CTE traps)
continue to monitor the instrument (throughput, gain, hysteresis, bad/hot pixels, filter transmission, IR blobs, grism calibration, CTE decline, stability of post-flash)
improve photometric precision (CTE correction, IR flat fields, dynamic range, IR persistence)
improve astrometric precision (spatial scans, DGEO files)
enhance UV calibration (flat fields, post-flash and CTE correction)
improve our understanding of IR persistence, IR blobs and the CSM, anomalous QE in CCD pixels

The results of these calibration programs will be documented in Instrument Science Reports on the WFC3 website at:
http://www.stsci.edu/hst/instrumentation/wfc3/documentation/instrument-science-reports-isrs

Table E.9: Cycle 21 Calibration Programs

Proposal ID	Title
13554	UVIS anneal
13555	UVIS bowtie monitor
13556	UVIS CCD daily monitor A
13557	UVIS CCD daily monitor B
13558	UVIS CCD daily monitor C
13559	UVIS CCD un-flashed monitor
13560	UVIS post-flash monitor
13561	UVIS CCD gain stability
13562	IR dark monitor
13563	IR linearity monitor
13564	IR gain monitor
13565	UVIS CTI monitor (EPER)
13566	UVIS CTE monitor (star cluster)
13567	CTE characterization with post-flashed darks
13568	Characterization of the charge-level dependence of CTE losses
13569	Characterization of UVIS traps with CI
13570	UVIS & IR geometric distortion
13571	High precision astrometry
13572	IR persistence model tests
13573	Trapping mitigation in spatial scan observations of exosolar planets
13574	WFC3 contamination & stability monitor
13575	WFC3 UVIS & IR photometry
13576	IR grisms: cross check sensitivity function of hot and cool stars
13577	UVIS grisms: flux calibration
13578	UVIS grisms: wavelength calibration
13579	IR grisms: flux calibration
13580	IR grisms: wavelength calibration
13581	IR grisms: sky characterization
13582	Calibration of the IR grism wavelength ZPs
13583	UV flats spatial scan
13584	UV flat field validation
13585	CCD anomalous QE pixels
13586	UVIS internal flats
13587	IR internal flats
13588	CSM monitor with earth flats
13624	Monitoring Persistence after scanned grism observations
13625	Characterizing persistence following scanned grism observations
13627	Timing verification for spatial scan observations

«Previous Next»

WFC3 Instrument Handbook
- • Acknowledgments
- Chapter 1: Introduction to WFC3
  - • 1.1 New for Cycle 33
  - • 1.2. Overview
  - • 1.3 Key Features of WFC3
  - • 1.4 WFC3 Quick Reference Guide
  - • 1.5 Special Considerations for Cycle 33
  - • 1.6 Sources of Further Information
  - • 1.7 The WFC3 Instrument Team at STScI
- Chapter 2: WFC3 Instrument Description
- Chapter 3: Choosing the Optimum HST Instrument
- Chapter 4: Designing a Phase I WFC3 Proposal
  - • 4.1 Phase I and Phase II Proposals
  - • 4.2 Preparing a Phase I Proposal
- Chapter 5: WFC3 Detector Characteristics and Performance
- Chapter 6: UVIS Imaging with WFC3
  - • 6.1 WFC3 UVIS Imaging
  - • 6.2 Specifying a UVIS Observation
  - • 6.3 UVIS Channel Characteristics
  - • 6.4 UVIS Field Geometry
  - • 6.5 UVIS Spectral Elements
  - • 6.6 UVIS Optical Performance
  - • 6.7 UVIS Exposure and Readout
  - • 6.8 UVIS Sensitivity
  - • 6.9 Charge Transfer Efficiency
  - • 6.10 Other Considerations for UVIS Imaging
  - • 6.11 UVIS Observing Strategies
- Chapter 7: IR Imaging with WFC3
  - • 7.1 WFC3 IR Imaging
  - • 7.2 Specifying an IR Observation
  - • 7.3 IR Channel Characteristics
  - • 7.4 IR Field Geometry
  - • 7.5 IR Spectral Elements
  - • 7.6 IR Optical Performance
  - • 7.7 IR Exposure and Readout
  - • 7.8 IR Sensitivity
  - • 7.9 Other Considerations for IR Imaging
  - • 7.10 IR Observing Strategies
- Chapter 8: Slitless Spectroscopy with WFC3
- Chapter 9: WFC3 Exposure-Time Calculation
  - • 9.1 Overview
  - • 9.2 The WFC3 Exposure Time Calculator - ETC
  - • 9.3 Calculating Sensitivities from Tabulated Data
  - • 9.4 Count Rates: Imaging
  - • 9.5 Count Rates: Slitless Spectroscopy
  - • 9.6 Estimating Exposure Times
  - • 9.7 Sky Background
  - • 9.8 Interstellar Extinction
  - • 9.9 Exposure-Time Calculation Examples
- Chapter 10: Overheads and Orbit Time Determinations
  - • 10.1 Overview
  - • 10.2 Observatory Overheads
  - • 10.3 Instrument Overheads
  - • 10.4 Orbit Use Examples
- Appendix A: WFC3 Filter Throughputs
  - • A.1 Introduction
  - A.2 Throughputs and Signal-to-Noise Ratio Data
    - • UVIS F200LP
    - • UVIS F218W
    - • UVIS F225W
    - • UVIS F275W
    - • UVIS F280N
    - • UVIS F300X
    - • UVIS F336W
    - • UVIS F343N
    - • UVIS F350LP
    - • UVIS F373N
    - • UVIS F390M
    - • UVIS F390W
    - • UVIS F395N
    - • UVIS F410M
    - • UVIS F438W
    - • UVIS F467M
    - • UVIS F469N
    - • UVIS F475W
    - • UVIS F475X
    - • UVIS F487N
    - • UVIS F502N
    - • UVIS F547M
    - • UVIS F555W
    - • UVIS F600LP
    - • UVIS F606W
    - • UVIS F621M
    - • UVIS F625W
    - • UVIS F631N
    - • UVIS F645N
    - • UVIS F656N
    - • UVIS F657N
    - • UVIS F658N
    - • UVIS F665N
    - • UVIS F673N
    - • UVIS F680N
    - • UVIS F689M
    - • UVIS F763M
    - • UVIS F775W
    - • UVIS F814W
    - • UVIS F845M
    - • UVIS F850LP
    - • UVIS F953N
    - • UVIS FQ232N
    - • UVIS FQ243N
    - • UVIS FQ378N
    - • UVIS FQ387N
    - • UVIS FQ422M
    - • UVIS FQ436N
    - • UVIS FQ437N
    - • UVIS FQ492N
    - • UVIS FQ508N
    - • UVIS FQ575N
    - • UVIS FQ619N
    - • UVIS FQ634N
    - • UVIS FQ672N
    - • UVIS FQ674N
    - • UVIS FQ727N
    - • UVIS FQ750N
    - • UVIS FQ889N
    - • UVIS FQ906N
    - • UVIS FQ924N
    - • UVIS FQ937N
    - • IR F098M
    - • IR F105W
    - • IR F110W
    - • IR F125W
    - • IR F126N
    - • IR F127M
    - • IR F128N
    - • IR F130N
    - • IR F132N
    - • IR F139M
    - • IR F140W
    - • IR F153M
    - • IR F160W
    - • IR F164N
    - • IR F167N
- Appendix B: Geometric Distortion
  - • B.1 Overview
  - • B.2 UVIS Channel
  - • B.3 IR Channel
- Appendix C: Dithering and Mosaicking
  - • C.1 Why Mosaicking and Dithering are Needed
  - • C.2 WFC3 Patterns
- Appendix D: Bright-Object Constraints and Image Persistence
  - • D.1 UVIS Channel
  - • D.2 IR Channel
- Appendix E: Reduction and Calibration of WFC3 Data
  - • E.1 Overview
  - • E.2 The STScI Reduction and Calibration Pipeline
  - • E.3 The SMOV Calibration Plan
  - • E.4 The Cycle 17 Calibration Plan
  - • E.5 The Cycle 18 Calibration Plan
  - • E.6 The Cycle 19 Calibration Plan
  - • E.7 The Cycle 20 Calibration Plan
  - • E.8 The Cycle 21 Calibration Plan
  - • E.9 The Cycle 22 Calibration Plan
  - • E.10 The Cycle 23 Calibration Plan
  - • E.11 The Cycle 24 Calibration Plan
  - • E.12 The Cycle 25 Calibration Plan
  - • E.13 The Cycle 26 Calibration Plan
  - • E.14 The Cycle 27 Calibration Plan
  - • E.15 The Cycle 28 Calibration Plan
  - • E.16 The Cycle 29 Calibration Plan
  - • E.17 The Cycle 30 Calibration Plan
  - • E.18 The Cycle 31 Calibration Plan
  - • E.19 The Cycle 32 Calibration Plan
- • Glossary

E.8 The Cycle 21 Calibration Plan

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