Ground to on-orbit alignment study of the WFIRST wide-field channel and resulting changes in the telescope architecture

Hagopian, John G.; Armani, Nerses V.; Bartusek, Lisa; Casey, Tom; Conturie, Y.; Gao, Ge; Jurling, Alden S.; Marx, Cathy; Marzouk, Joe; Pasquale, Bert A.; Smith, J. Scott; Tang, Hong; Whipple, A. L.

doi:10.1117/12.2280333

Cited by 2 publications

(5 citation statements)

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“…Alignment trade studies during Phase-A [8] also indicated the advantage of including 3-DOF actuation on the WFC F1. This is the baseline for the Phase-B as has been shown in the Figure 5 block diagram.…”

Section: Wfc Fold Mirror 1 Assembly Actuation Mechanismmentioning

confidence: 96%

“…At this point, it is assumed that wavefront sensing will verify the alignments to a given residual value. [8] To prevent compensation moving beyond the range of the actuators, various components may be biased with shimming to achieve system performance once on orbit. It is highly undesirable in the actual I&T procedure to "re-do" shims following a verification test, so performance allocations are based on the "worst-case" of having to use only mechanized compensators.…”

Section: Phase 2: Fem Modeling Testing and Pre-launch Biasing Allotmentsmentioning

confidence: 99%

“…• The implementation of the WFC Fold Mirror 1 and Focal Plane Assembly actuation mechanisms • The loss of the Integral Field Channel Instrument from the payload As will be seen, the combined efforts of the WFIRST team in Phase-A on these key trades [8] have resulted in significant risk reduction for the WFIRST program to make the Phase-B design as robust and future-proof as possible.…”

Section: Introduction and Current Statusmentioning

confidence: 99%

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Optical design and predicted performance of the WFIRST phase-b imaging optics assembly and wide field instrument

Pasquale

Casey²,

Marx

et al. 2018

Current Developments in Lens Design and Optical Engineering XIX

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Now in Phase-B, the architecture of the Wide-Field Infra-Red Survey Telescope (WFIRST) payload has matured since 2013 to accommodate various opto-mechanical constraints. Based on a 2.4-meter aperture Forward Optical Assembly (FOA), the Imaging Optics Assembly (IOA) provides corrected optical fields to each on-board instrument. Using a Three Mirror Anastigmat (TMA) optical design, the Wide-Field Channel (WFC) provides ~1/3-square degree of instantaneous field coverage at 0.11 arcsecond pixel scale. The WFC as-built predictive analysis anticipates near diffraction-limited imaging over a focal plane of 300.8 million pixels, operating in seven panchromatic bands between 0.48 -2.0µm, or a 1-octive multi-spectral imaging mode from ~0.95-1.93µm. The IOA provides the Coronagraph Instrument (CGI) a collimated beam with very specific wavefront constraints. We present configuration changes since 2013 that improved interfaces, improved testability, and reduced technical risk. We provide an overview of our Integrated Modeling results, performed at an unprecedented level for a phase-A study, to illustrate performance margins with respect to static wavefront error, jitter, and thermal drift.

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Section: Wfc Fold Mirror 1 Assembly Actuation Mechanismmentioning

confidence: 96%

Section: Phase 2: Fem Modeling Testing and Pre-launch Biasing Allotmentsmentioning

confidence: 99%

Section: Introduction and Current Statusmentioning

confidence: 99%

See 1 more Smart Citation

Optical design and predicted performance of the WFIRST phase-b imaging optics assembly and wide field instrument

Pasquale

Casey²,

Marx

et al. 2018

Current Developments in Lens Design and Optical Engineering XIX

Self Cite

View full text Add to dashboard Cite

show abstract

“…Interested readers can consult the literature for a more detailed review of the design and design history of the observatory. [20][21][22][23] RST is a 2.4 meter primary obscured three mirror anastigmat telescope design. The three powered mirrors are all simple conics, with two fold mirrors in the path to WFI, seen in Fig.…”

Section: Rst Optical Overviewmentioning

confidence: 99%

“…WFE numbers for the four filters that were unable to be tested due to limited interferometer wavelengths will be obtained via focus diverse phase retrieval, similar to how Webb and other telescopes have been aligned in orbit. 21,[41][42][43][44] The measured results discussed in the previous section will be used as sanity checks against the numbers obtained through phase retrieval.…”

Section: Flight Performance Predictionsmentioning

confidence: 99%

Science filter performance summary for the Roman Space Telescope Wide Field Instrument

Cromey,

Von Handorf,

Pedroncelli

et al. 2023

UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts XI

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The Wide Field Instrument (WFI) on NASA's Roman Space Telescope has eight filters on a large filter wheel that are key to enabling the science missions of the observatory. These filters have completed their journey from individual components to fully integrated elements in the optical element wheel assembly (EWA), and have been characterized in terms of their transmittance, wavefront impact, and other key performance characteristics. This paper will summarize their capabilities and performance, demonstrating their ability to deliver top-quality science on orbit.

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Ground to on-orbit alignment study of the WFIRST wide-field channel and resulting changes in the telescope architecture

Cited by 2 publications

References 1 publication

Optical design and predicted performance of the WFIRST phase-b imaging optics assembly and wide field instrument

Optical design and predicted performance of the WFIRST phase-b imaging optics assembly and wide field instrument

Science filter performance summary for the Roman Space Telescope Wide Field Instrument

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