TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 1 Figure 1-2. Artist's Impression of the Terrestrial Planet Finder Interferometer as a cryogenic nulling interferometer consisting of four 3.5-m telescopes deployed on separate spacecraft with baselines in excess of 100 m (Figure 1-2). With TPF-I astronomers will be capable of characterizing planets and their atmospheres with the goal of identifying habitable or life-bearing planets around more that 150 nearby stars. Ultimately, the detection and characterization of Earth-like planets and the search for life will require coordinated observations at optical and infrared wavelengths as well as dynamical measurements to determine planetary mass. Table 1-1 summarizes the measurements enabled by different planet-finding missions and how the mid-infrared observations of the interferometric version of the Terrestrial Planet Finder (TPF-I) fit into a broad vision of exo-planetology. Accomplishing the complete characterization of nearby planets is the unifying goal of TPF-I (which is being studied jointly with the TPF-I project by NASA and the Darwin project by the European Space Agency) and its sibling missions, the visible light coronagraph TPF-C and the astrometric mission Space Interferometry Mission (SIM)/Planetquest. 1.1 Purpose and Scope This document is a collaborative effort between the TPF-I Science Working Group (SWG) and the TPF-I Project. Although the charter of the SWG was to advise NASA on science requirements and priorities, their advice also greatly influenced technical research within the project — in particular the project’s ongoing reassessment of the interferometer architecture and the flow-down of science requirements to technical objectives. The science requirements and objectives are described by the SWG in the opening Chapters on Exoplanet Science (Chapter 2) and Transforming Astrophysics with TPF-I (Chapter 3). This work builds on earlier SWG reports (ExNPS 1996; Beichman et al. 1999; Beichman et al. 2002; Lawson 2
I NTRODUCTION et al. 2004), and restates the scientific case for TPF-I, assesses suitable target stars and relevant wavelengths for observation, and summarizes recent results on the zodiacal emission that can impact detection of planets. The compelling general astrophysics that will be possible with TPF-I is described in Chapter 3; the balance between increased astrophysics capability and increased cost will be addressed at a later phase in the project. Through the stated science requirements and technical interchange meetings, the SWG was also influential in determining the architecture of the interferometer, described in detail in Chapter 4. The results of an extensive investigation of different architectures and the sources of systematic noise sources are presented and discussed. Chapter 4 also describes the baseline X-array architecture selected for detailed study as well as describing briefly a structurally connected option with limited capability. The two subsequent chapters of this document consist primarily of contributions by TPF-I project members and provide a current view of progress with interferometer design studies (Chapter 5) and laboratory demonstrations of nulling interferometry and formation flying (Chapter 6). Included here are sections summarizing progress in critical testbed activities undertaken by the TPF-I project and reported on at various TPF-I Science Working Group meetings. Laboratory nulling has reached a broad-band level approaching 10 -5 that is arguably within a factor of 2 needed for the TPF-I flight system. Chapter 6 also presents a summary of a technology roadmap developed by the TPF-I project The concluding chapters resume with recommendations by the SWG for future studies. Chapter 7 includes a prioritized list of future scientific investigations, and Chapter 8 discusses the potential for international collaboration on TPF-I/Darwin in the context of concluding remarks. Table 1-1. Synergy of Missions in the Navigator Program Parameter SIM TPF-C TPF-I Orbital Parameters Stable orbit in habitable zone Measurement Measurement Measurement Characteristics for Habitability Planet temperature Estimate Estimate Measurement Temperature variability due to Measurement Measurement Measurement eccentricity Planet radius Cooperative Cooperative Measurement Planet albedo Cooperative Cooperative Cooperative Planet mass Measurement Estimate Estimate Surface gravity Cooperative Cooperative Cooperative Atmospheric and surface Cooperative Measurement Measurement composition Time-variability of composition Measurement Measurement Presence of water Measurement Measurement Solar System Characteristics Influence of other planets, orbit co-planarity Measurement Estimate Estimate Comets, asteroids, and zodiacal dust Measurement Measurement Indicators of Life Atmospheric biomarkers Measurement Measurement Surface biosignatures, e.g. red edge Measurement of vegetation ``Measurement'' indicates a directly measured quantity from a mission; ``Estimate'' indicates that a quantity that can be estimated from a single mission; and ``Cooperative'' indicates a quantity that is best determined cooperatively using data from several missions. (Beichman et al. 2006) 3
Page 1 and 2: JPL Publication 07-1 Terrestrial Pl
Page 3: Abstract Over the past two years, t
Page 7 and 8: Acknowledgements Twenty-two represe
Page 9 and 10: Table of Contents 1 Introduction...
Page 11 and 12: 4.8.3 Post-Nulling Calibration.....
Page 13 and 14: 6.4.5 Double Fourier Interferometry
Page 15: I NTRODUCTION 1 Introduction Over 2
Page 19 and 20: I NTRODUCTION Standard Interferomet
Page 21: I NTRODUCTION 1.4 References Angel,
Page 24 and 25: C HAPTER 2 0.7 to 1.5 AU scaled by
Page 26 and 27: C HAPTER 2 Table 2-2. Illustrative
Page 28 and 29: C HAPTER 2 Classical interferometry
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Page 34 and 35: C HAPTER 2 would be in atmospheres
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Page 38 and 39: C HAPTER 2 Lines of constant stella
Page 40 and 41: C HAPTER 2 presence of zodiacal clo
Page 42 and 43: C HAPTER 2 S EZ 2π ∫ θ max ∫
Page 44 and 45: C HAPTER 2 Figure 2-11. Observation
Page 46 and 47: C HAPTER 2 Figure 2-12. Models of t
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
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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
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C HAPTER 3 Figure 3-9: Simulated im
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C HAPTER 3 3.3 Conclusions Darwin/T
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C HAPTER 3 Nguyen, H. T., Kallivaya
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D ESIGN AND A R C H I T E C T U R E
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C HAPTER 5 Heavy launch vehicle. Th
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C HAPTER 5 5.3.2 Combiner Spacecraf
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C HAPTER 5 5.3.5 Beam Transfer betw
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C HAPTER 5 Figure 5-8. Control sche
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C HAPTER 5 Figure 5-9. First sectio
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C HAPTER 5 Figure 5-9 shows the fir
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C HAPTER 5 5.4.4 Shear Metrology Sh
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C HAPTER 5 Figure 5-15. TPF-I Fligh
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C HAPTER 5 secondary mirror along t
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C HAPTER 5 a) c) b) d) IWA = 43 mas
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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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TPF-I SWG Report - Exoplanet Exploration Program - NASA

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