Wide Field Camera 3 Instrument Handbook for Cycle 19 - Space ...

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14 Chapter 2: WFC3 Instrument Description Figure 2.4: IR Filter Wheel 2.3.3 Shutter Mechanism Integration times in the UVIS channel are controlled via a mechanical shutter blade very similar in design to the ACS/WFC shutter. Sitting directly behind the SOFA, the WFC3 UVIS shutter is a rotating disk about 12 inches in diameter; it is divided into four 90° quadrants, with alternating quadrants providing the blocking (i.e., there are two open and two closed positions). When the shutter is in the closed position initially, a commanded move of 90° places it into an open configuration; at the end of the exposure, another move of 90° places the shutter back into a closed position. Although the shutter can be operated in either a clockwise or counterclockwise direction, the current flight software always moves the blade in the same direction. For very short exposure times in the UVIS channel, there are minor issues with exposure time non-uniformity (Section 6.7.1) and blurring due to shutter-induced vibration (Section 6.9.5). There is no mechanical shutter in the IR channel; instead, the detector provides electronic shuttering. Dark-current measurements are obtained by using the BLANK, an opaque blocker in the filter wheel, which also is used to prevent the detector from viewing the Earth during occultations.
Detector Read-Out Modes and Dithering 15 2.4 Detector Read-Out Modes and Dithering The detectors in both channels offer subarray readout capability; see Section 6.4.4 (UVIS) and Section 7.4.4 (IR) for full details. The UVIS channel also allows 2×2 and 3×3 on-chip binning of full-frame images. Finally, a variety of dithering patterns can be requested using the Astronomer’s Proposal Tool (APT) software. Predefined patterns have been established to address common requirements, such as sub-pixel dithering to improve PSF sampling or dithering to achieve large areal coverage while also sampling the inter-chip gap (Appendix C). The post-observation pipeline software (see Appendix E, the WFC3 Data Handbook, and the MultiDrizzle Handbook) carries out appropriate calibration of data taken in all of these configurations, and offers the option of reconstructing dithered images with a drizzling algorithm. If the dither pattern incorporates non-integer pixel offsets, it can effectively improve the sampling of the point-spread function (PSF). The software can also handle mosaicked images according to a set of rules or associations, rectifying them onto a cartesian pixel coordinate system.
Page 1 and 2: Version 3.0 December 2010 Wide Fiel
Page 3 and 4: Table of Contents Acknowledgments .
Page 5 and 6: Table of Contents v 5.5 The WFC3 IR
Page 7 and 8: Table of Contents vii 7.8 IR Sensit
Page 9 and 10: Table of Contents ix Appendix C: Di
Page 11 and 12: xi Past Science IPT Members Elizabe
Page 13 and 14: CHAPTER 1: Introduction to WFC3 In
Page 15 and 16: WFC3 Quick Reference Guide 3 • UV
Page 17 and 18: Sources of Further Information 5 1.
Page 19 and 20: CHAPTER 2: WFC3 Instrument Descript
Page 21 and 22: Figure 2.1: Schematic optical layou
Page 23 and 24: Spectral Elements 11 elongation of
Page 25: Spectral Elements 13 Figure 2.3: UV
Page 29 and 30: Choosing Between Instruments 17 3.2
Page 31 and 32: 3.3.2 Field of View Comparison of W
Page 33 and 34: Comparison of WFC3 with Other HST I
Page 35 and 36: Comparison of WFC3 with Other HST I
Page 37 and 38: Preparing a Phase I Proposal 25 4.2
Page 39 and 40: 4.2.3 What Aperture or Subarray? Pr
Page 41 and 42: CHAPTER 5: WFC3 Detector Characteri
Page 43 and 44: The WFC3 UVIS Channel CCD Detectors
Page 45 and 46: WFC3 CCD Readout Formats 33 5.3 WFC
Page 47 and 48: WFC3 CCD Characteristics and Perfor
Page 61 and 62: 5.4.12 Crosstalk WFC3 CCD Character
Page 63 and 64: The WFC3 IR Channel Detector 51 Fig
Page 65 and 66: WFC3 IR Readout Formats 53 Figure 5
Page 67 and 68: WFC3 IR Readout Formats 55 Full-fra
Page 69 and 70: WFC3/IR Detector Characteristics an
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Specifying a UVIS Observation 65 6.
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UVIS Field Geometry 67 Figure 6.1:
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6.4.4 Subarrays and On-Chip Binning
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UVIS Field Geometry 71 target at th
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UVIS Spectral Elements 73 6.5 UVIS
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UVIS Spectral Elements 75 Table 6.2
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Figure 6.3: Integrated system throu
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UVIS Spectral Elements 81 UV Filter
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UVIS Spectral Elements 83 Table 6.3
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UVIS Spectral Elements 85 Figure 6.
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6.5.3 Ghosts UVIS Spectral Elements
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UVIS Optical Performance 89 Table 6
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UVIS Optical Performance 91 Figure
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UVIS Optical Performance 93 Table 6
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UVIS Optical Performance 95 Figure
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UVIS Exposure and Readout 97 (1.0,
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UVIS Sensitivity 99 contains 1402×
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6.9.3 Charge-Transfer Efficiency Ot
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UVIS Observing Strategies 103 6.10
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CHAPTER 7: IR Imaging with WFC3 In
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IR Field Geometry 107 The WFC3 IR d
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IR Field Geometry 109 The POS TARG
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IR Spectral Elements 111 Table 7.1:
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IR Spectral Elements 115 Wide-band
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IR Optical Performance 117 Table 7.
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IR Optical Performance 119 Figure 7
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IR Optical Performance 121 Table 7.
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IR Exposure and Readout 123 Inter-p
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IR Exposure and Readout 125 • the
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Table 7.8: Sample times of 1024×10
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IR Sensitivity 129 Table 7.9: Suppo
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Other Considerations for IR Imaging
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IR Observing Strategies 137 sub-pix
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IR Observing Strategies 139 Table 7
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CHAPTER 8: Slitless Spectroscopy wi
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Slitless Spectroscopy with the UVIS
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Slitless Spectroscopy with the IR G
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Slitless Spectroscopy with the IR G
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Sensitivities and Exposure-Time Est
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CHAPTER 9: WFC3 Exposure-Time Calcu
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Calculating Sensitivities from Tabu
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Calculating Sensitivities from Tabu
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Count Rates (Imaging) 157 Table 9.2
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9.4.2 Diffuse Sources Count Rates (
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The S/N ratio Σ achieved in exposu
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Sky Background 163 • I λ is the
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Sky Background 165 Figure 9.1: Sky
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Sky Background 167 Table 9.4: Appro
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Exposure-Time Calculation Examples
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Exposure-Time Calculation Examples
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Observatory Overheads 173 activitie
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Instrument Overheads 175 Table 10.1
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Instrument Overheads 177 IR paralle
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Orbit Use Examples 179 In the IR ch
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Orbit Use Examples 181 Table 10.4:
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Orbit Use Examples 183 Table 10.6:
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APPENDIX A: WFC3 Filter Throughputs
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Throughputs and S/N Ratio Data 187
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% Throughput 30 25 20 15 UVIS/F200L
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% Throughput UVIS/F225W Description
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% Throughput UVIS/F280N Description
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% Throughput UVIS/F350LP Descriptio
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% Throughput UVIS/F390M Description
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% Throughput UVIS/F475X Description
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% Throughput UVIS/F763M Description
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% Throughput UVIS/F850LP Descriptio
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% Throughput UVIS/FQ232N Descriptio
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% Throughput UVIS/FQ422M Descriptio
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% Throughput IR/F098M Description B
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% Throughput IR/F110W Description W
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% Throughput IR/F126N Description [
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% Throughput IR/F128N Description P
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% Throughput IR/F132N Description P
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% Throughput IR /F167N Description
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APPENDIX B: Geometric Distortion In
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UVIS Channel 277 See http://www.sts
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IR Channel 279 Figure B.3: Linear c
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APPENDIX C: Dithering and Mosaickin
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WFC3 Patterns 283 special-purpose m
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WFC3 Patterns 285 Table C.3:Steps i
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APPENDIX D: Bright-Object Constrain
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IR Channel 289 available. To use th
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IR Channel 291 Table D.4: Count Rat
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The STScI Reduction and Calibration
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The STScI Reduction and Calibration
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The SMOV Calibration Plan 297 Propo
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The Cycle 17 Calibration Plan 299 P
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The Cycle 18 Calibration Plan 301 P
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Glossary 303 FGS: Fine Guidance Sen
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Index A ACCUM mode UVIS 96 Aperture
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Index 307 UVIS/FQ634N 242 UVIS/FQ67
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Index 309 comparing HST instruments
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