E.13 The Cycle 26 Calibration Plan

The Cycle 26 calibration plan was executed from November 2018 through October 2019. The individual programs are listed in Table E.14 and are described in more detail on the WFC3 Calibration Plan webpage. Following the link to Cycle 26 Calibration, a similar table may be found with direct links to the phase II programs and observation dates. This information may alternately be accessed via the HST Program Information webpage by entering the Proposal ID.

The WFC3 Cycle 26 section also links to a PDF presentation summarizing WFC3 usage and comparing the Cycle 26 plan with the prior cycle. This document contains more details on the calibration justification and in many cases includes supporting figures with the latest results from regular monitoring.

The Cycle 26 calibration plan was designed to:

Maintain and update the standard reference files (biases, darks, linearity, CTE traps, UVIS anomalous QE pixels, post-flash)
Monitor the health of the instrument (throughput, gain, hysteresis, bad/hot pixels, sink pixels, CTE decline, stability of the post-flash LED, filter transmission, state of the CSM, number of IR blobs, wavelength and flux stability of the grisms)
Support new initiatives and obtain supplemental (non-routine) calibration data

In this cycle, two new calibration programs will supplement the standard monitoring data. These programs (15585, 15581) were designed to:

Cross-calibrate the HST focus values derived from the OTA Focus monitor (based on UVIS/F410M observations) with the focus values derived empirically from the WFC3/UVIS PSF database, which has many more F606W observations
Characterize the decay of IR persistence at short time-scales (t <300 sec), where the observed residual signal deviates from the current power-law model

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.14: The Cycle 26 Calibration Programs

Program ID	Title
15567	WFC3 UVIS Anneal
15568	WFC3 UVIS Bowtie Monitor
15569	WFC3 UVIS CCD Daily Monitor (Darks and Biases) Part 1
15570	WFC3 UVIS CCD Daily Monitor (Darks and Biases) Part 2
15571	WFC3 UVIS CCD Daily Monitor (Darks and Biases) Part 3
15572	WFC3 UVIS CCD Unflashed (CTE) Monitor
15573	WFC3 UVIS Post-flash Monitor
15574	WFC3 UVIS CCD Gain Stability
15575	WFC3 UVIS CTI Monitor (EPER)
15576	WFC3 UVIS CTE Monitor (star cluster)
15577	WFC3 Characterization of UVIS traps with Charge Injection
15578	WFC3 IR Dark Monitor
15579	WFC3 IR Linearity Monitor
15580	WFC3 IR Gain Monitor
15581	WFC3 Short-term IR Persistence
15582	WFC3 UVIS & IR Photometry
15583	WFC3 UVIS Contamination Monitor (staring and scans)
15584	WFC3 UVIS Shutter Monitoring
15585	WFC3 Focus Cross-Calibration
15586	WFC3 IR Grism Wavelength Calibration
15587	WFC3 IR Grism Flux/trace Calibration
15588	WFC3 UVIS Grism Wavelength Calibration
15589	WFC3 UVIS Pixel-to-Pixel QE Variations via Internal Flats
15590	WFC3 UVIS Internal Flats
15591	WFC3 IR Internal Flats
15592	WFC3 CSM Monitor with Earth Flats
15593	WFC3 Astrometric Scale Monitoring

«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.13 The Cycle 26 Calibration Plan

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