TPF-C Technology Plan - Exoplanet Exploration Program - NASA

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Chapter 3 Figure 3-13. Optical layout and views of the High Contrast Imaging Testbed (HCIT). a side view of the testbed is shown in Figure 3-13. This facility is modular, allowing for integration of modules from a variety of sources and designed for remote observing, so that users from many institutions can be supported. JPL will schedule and support guest users commencing in 2005. Approach Empirical investigation and validation of core coronagraph technology is practical with HCIT. This testbed represents two essential subsystems of a high contrast instrument: wavefront retrieval and correction and coronagraphic control of diffracted light. The testbed will validate that an instrument can achieve and maintain contrast beyond 10 -10 (10 -9 in pre-Phase A) at the required inner working angle of the TPF coronagraph telescope. This constitutes a fundamental confirmation that phase and amplitude errors can be sensed, corrected, and held for the time period of extrasolar planet detection. Furthermore, it will validate software, diffraction models, and an error budget necessary to construct and operate a flight instrument. The HCIT development will consist of the following hardware thrusts: continued improvement in the deformable mirror and its performance; continued demonstration of wavefront sensing and control; and testing of apodizing masks and Lyot stops provided by government, industry, and 50
Optics and Starlight Suppression Technology academic sources. The testbed has been designed to accommodate a suitable subscale telescope and associated masks and stops such as those planned to be developed as part of the Industry Coronagraph Technology thrust. In addition, the HCIT can be used to correlate analyses provided by outside sources and can accommodate possible additional back-end subsystems. The testbed is in operation and has achieved contrasts in a half dark hole of better than 10 -8 . The testbed status and mapping to the technology gates is shown in Table 3-5. Table 3-5. TPF-C HCIT Testbed status and mapping to the technology gates Objectives Metric Status Planned Completion Date Demonstrate starlight suppression Demonstrate broadband starlight suppression 1 × 10 -9 (goal 1 × 10 -10 ) at a 4 λ/D inner working angle, at λ≈785 nm, stable for 1 hr 1 × 10 -9 (goal 1 × 10 -10 ) at a 4 λ/D inner working angle, over a 60 nm bandpass (goal 100 nm) with center wavelength between 0.5–0.8 µm A 9 × 10 -10 average contrast was achieved over the half-dark hole, including the 4 λ/D inner working angle, at λ=785 nm; measurement was repeatable; stability of the measurement better than 1 × 10 -10 /hr. A 5 × 10 -9 average contrast has been achieved over the half-dark hole, including the 4 λ/D inner working angle, over the wavelength band 800±20nm; repeatable measurement Tech Gate Q3 FY05 1 Q3 FY06 2 Validate optical modeling approach Starlight suppression performance predictions are consistent with actual testbed measurements An error budget of the HCIT is being developed. This will guide the plan for experimentation to support development of a deterministic model. Q4 FY06 3a Demonstrate mission feasibility Demonstrate through modeling that TPF-C can achieve the required contrast over the required optical bandwidth The next iteration of the flight baseline design concept is due on January 28. Modeling and analysis is due to be completed by the end of April. Q1 FY07 3b Progress to Date The testbed was aligned in a clean tent and became operational in ambient conditions in October 2002. Experiments with a 1764-actuator deformable mirror yielded contrast on the order of 10 -5 . Modeling suggested that better contrast was not attainable given the imperfections in this DM. In April 2003 the testbed was moved to a vacuum chamber. Wavefront sensing experiments commenced in June 2003 using a flat mirror as a surrogate for the DM. The first fully-functional 1024-actuator DM was installed in October 2003. Initial experiments using phase retrieval, a phase-only method, to sense and correct the wavefront, immediately yielded contrast of 2 × 10 -6 . Speckle nulling experiments commenced in December 2003. This technique, which uses science camera images to calculate the DM control, has the ability to compensate for amplitude errors over half the field. These experiments quickly drove the contrast to 7 × 10 -9 . In addition to the speckle nulling technique, two Lyot plane algorithms have been developed and tested. These 51
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JPL Publication 05-8 Technology Pla
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TECHNOLOGY PLAN TERRESTRIAL PLANET
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Recent Highlights Technical progres
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Figure i-4. Deformable mirror deliv
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Table of Contents Approvals........
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Page 16 and 17: Chapter 1 interferometry, continues
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Chapter 6 super computers and is us
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Chapter 7 7 Plan for Technology Dev
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Chapter 7 Figure 7-1. TPF-C Technol
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Chapter 7 Improvements to the DM ov
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Chapter 7 7.3 Error Budgets 7.3.1 D
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Chapter 7 7.4 Optics and Starlight
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Chapter 7 7.4.2 Apodizing Masks and
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Chapter 7 7.4.4 Wavefront Sensing a
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Chapter 7 7.4.6 Transmissive Optics
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Chapter 7 7.4.8 Scatterometer Scope
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Chapter 7 7.5 Structural, Thermal,
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Chapter 7 7.5.3 Precision Structura
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Chapter 7 model of TPF-C and should
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Chapter 7 7.5.6 Secondary Mirror To
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Chapter 7 7.5.8 Sub-scale EM Sunshi
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Chapter 7 7.6 Integrated Modeling a
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Chapter 7 7.7.3 Advanced Concepts:
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Chapter 8 134
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Appendices Appendix B: TPF-C Detail
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Appendices Appendix D: TPF-C Techno
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Appendices Appendix F: Acronym List
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Appendices RWA SAO SBIR SIM SM SMFA
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TPF-C Technology Plan - Exoplanet Exploration Program - NASA

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