TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 4 shading. The formation-flying system must carefully maintain the position and pointing of the collector spacecraft to ensure that the beams are delivered to the correct locations on the combiner. The Emma architecture has a number of attractive features, but also has some disadvantages: Pros: Cons: + Simplified collector – Increased combiner spacecraft complexity No deployable optics Compact sun-shade – Smaller maximum array size – Increased demands on formation flying + Flexible collector array geometry – No collector standalone observing + Increased sky coverage – Stray light from collector sunshades + Smaller minimum array size The Emma concept has been pursued by the Alcatel study group for Darwin, and it has now become the subject of a design study at JPL. a) b) Combiner ~ 1 km Allowed solar illumination angles Collector Combiner Collector Allowed solar illumination angles Figure 4-10. (a) Classic co-planar architecture, (b) the out-of-plane Emma concept. 72
D ESIGN AND A R C H I T E C T U R E T RADE S TUDIES 4.6 Beam Combiner Design In nulling interferometry, excess starlight is blocked using an interferometric cancellation technique, improving the star-to-planet contrast ratio to enable planet detection over an observation time typically of several hours. To reduce the stellar leakage signal to a level comparable to the zodiacal background the nuller should be capable of reaching null depths of at least 10 -5 . To reach deep nulls, a number of parameters must be controlled, some inside the nuller and some in other associated systems. An important feature of a successful nulling beam combiner will be identical treatment of both input beams in terms of phase shifts, reflections and transmissions, angles of incidence, polarizations, etc. Different nuller designs are being tested in the laboratory and in the field. A modified Mach-Zehnder design (MMZ) has been deployed on the Keck telescopes, and this design seeks to achieve a high degree of symmetry in the beam combination by causing each input beam to be both transmitted once and reflected once from nearidentical beamsplitters (this design achieved 2 million to 1 laser nulls at 10.6 μm). A different design (also using conventional beamsplitters), the rooftop nuller, was built at JPL for SIM and achieved high performance nulls (laser transient nulls at 633 nm near 10 -6 and 18% bandwidth redlight nulls of 10 -4 ) in the visible waveband. A newer concept, the fiber beam combiner is currently being tested in the laboratory for deployment on a large ground-based telescope. This design seeks to achieve high beam symmetry by dispensing with the beamsplitters and combining the incoming beams directly on the tip of a single-mode optical fiber, and this design has already achieved laser nulls of 10 5 in the visible. Bright outputs Beamsplitter 4 Common mirrors Nulled outputs Inner mirror Input beams Beamsplitter 1 Outer mirror Figure 4-11. Modified Mach-Zehnder nuller used on Keck Telescopes. 73
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JPL Publication 07-1 Terrestrial Pl
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Abstract Over the past two years, t
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Acknowledgements Twenty-two represe
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Table of Contents 1 Introduction...
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4.8.3 Post-Nulling Calibration.....
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6.4.5 Double Fourier Interferometry
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I NTRODUCTION 1 Introduction Over 2
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I NTRODUCTION et al. 2004), and res
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I NTRODUCTION Standard Interferomet
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I NTRODUCTION 1.4 References Angel,
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C HAPTER 2 0.7 to 1.5 AU scaled by
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C HAPTER 2 Table 2-2. Illustrative
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C HAPTER 2 Classical interferometry
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C HAPTER 2 trivial in the absence o
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C HAPTER 2 Figure 2-3. Simulated mi
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C HAPTER 2 would be in atmospheres
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Page 38 and 39: C HAPTER 2 Lines of constant stella
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Page 42 and 43: C HAPTER 2 S EZ 2π ∫ θ max ∫
Page 44 and 45: C HAPTER 2 Figure 2-11. Observation
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Page 48 and 49: C HAPTER 2 Beichman, C. A., Fridlun
Page 50 and 51: C HAPTER 2 2.7.4 Suitable Targets E
Page 52 and 53: C HAPTER 2 Reach, W. T., Franz, B.
Page 54 and 55: C HAPTER 3 3.1.1 Darwin/TPF-I Prope
Page 56 and 57: C HAPTER 3 clouds or an OB associat
Page 58 and 59: C HAPTER 3 Figure 3-3. Three possib
Page 60 and 61: C HAPTER 3 the circumstellar disk,
Page 62 and 63: C HAPTER 3 Figure 3-6. (Left panel)
Page 64 and 65: C HAPTER 3 Continuum interferometry
Page 66 and 67: C HAPTER 3 Figure 3-9: Simulated im
Page 68 and 69: C HAPTER 3 3.3 Conclusions Darwin/T
Page 70 and 71: C HAPTER 3 Nguyen, H. T., Kallivaya
Page 73 and 74: D ESIGN AND A R C H I T E C T U R E
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Page 114 and 115: C HAPTER 5 Heavy launch vehicle. Th
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Page 118 and 119: C HAPTER 5 5.3.5 Beam Transfer betw
Page 120 and 121: C HAPTER 5 Figure 5-8. Control sche
Page 122 and 123: C HAPTER 5 Figure 5-9. First sectio
Page 124 and 125: C HAPTER 5 Figure 5-9 shows the fir
Page 126 and 127: C HAPTER 5 5.4.4 Shear Metrology Sh
Page 128 and 129: C HAPTER 5 Figure 5-15. TPF-I Fligh
Page 130 and 131: C HAPTER 5 secondary mirror along t
Page 132 and 133: C HAPTER 5 a) c) b) d) IWA = 43 mas
Page 134 and 135: C HAPTER 5 planets found. Figure 5-
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C HAPTER 5 30 25 5 M earth 3 M eart
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C HAPTER 5 5.8.4 Angular Resolution
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C HAPTER 5 Table 5-3. Angular Resol
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C HAPTER 5 The optimization works b
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T E C H N O L O G Y R OADMAP FOR TP
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F UTURE D EVELOPMENTS 7 Preparatory
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F UTURE D EVELOPMENTS • To comple
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F UTURE D EVELOPMENTS Table 7-1. Pr
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D ISCUSSION AND C ONCLUSION 8 Discu
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Appendices 167
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T E C H N O L O G Y A DVISORY C O M
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F L I G H T S YSTEM C ONFIGURATION
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F L I G H T S YSTEM C ONFIGURATION
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A PPENDIX C 2. Identical FACS fligh
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A PPENDIX C 2. Recall that the coef
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A PPENDIX C Once the formation has
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A PPENDIX C Figure C-3. Example of
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A PPENDIX C Figure C-4. FAST Flight
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A PPENDIX C The “true” time of
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A PPENDIX C References Cohen, S., a
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A PPENDIX D DC DCB DM DM DOCS DOD D
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A PPENDIX D NaCl NAR NASA NASTRAN N
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A PPENDIX E Appendix E TPF-I Review
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A PPENDIX F Alice Quillen, Universi
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A PPENDIX F Figure 3-1 - Original f
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