TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 7 the instrumentation requirements and search strategies for TPF-I, and they will ultimately provide a theoretical framework for analysis of the mission data. 7.2 Phase A In Phase A the emphasis will be on specifying the detailed design of the optics of TPF-I, leading to the Preliminary Mission and System Review. The mission and system definition studies will refine the architecture so that it is ready for preliminary designs in Phase B. The overriding question to be resolved by the end of Phase A will be to define the capability of the mission and determine to what scale the observatory must be built. What volume of space should be searched for planets How large of a collecting area will be needed What angular resolution will be required Scaling the architecture and defining the scope of the mission will be necessary before TPF-I continues to Phase B, C, and D. 7.2.1 Priority 1: Frequency of Terrestrial Planets The scale of the TPF-I—the distance between the furthest collecting apertures of the interferometer—will determine the number of stars that are attainable. Defining the capability of a mission will involve a trade between the desire to explore a larger number of extrasolar planetary systems and the technological difficulty of building a larger observatory. To better understand this trade, preparatory science activities prior to Phase A will include detections of planets by a variety of techniques. Coupled with advances in astrophysical theory, these data (including transit detections of several-Earth mass planets from CoRoT for nearby stars) will provide improved estimates of the frequency of Earth-like planets. The programmatic implications will be wide-ranging. More certain knowledge of the frequency of Earths will not only help set the scale of the observatories but will later assist in setting priorities in the initial phases of the missions. 7.2.2 Priority 2: Target Stars The refined target list, to be developed for the mission during its Phase A, will assist in optimizing the trades (taking into account the expected performance limits) that will ultimately define the capability of TPF-I. The number of attainable target stars of different spectral types, their distances, and their detailed characteristics will largely determine the scientific return of each mission. This target list is more than just an output from a catalog search. There are many characteristics of stars that must be measured, and then carefully weighed in importance, before such a refined list can be constructed. All nearby stars should be well characterized before the target lists for TPF-I can be chosen. A refined target list, with the farthest target identified, will be needed in Phase A to set the scale of the observatory. The distance to the farthest planet in the survey will be determined by the size of the observatory (its angular resolution) and the area of its collecting apertures (its sensitivity). 162
F UTURE D EVELOPMENTS Table 7-1. Priorities of TPF-I Science Themes During Pre-Phase A and Phase A Priority Pre Phase A Phase A 1 Exozodiacal Dust Frequency of Terrestrial Planets 2 Frequency of Terrestrial Planets Target Stars 3 Target Stars Signs of Life 4 Signs of Life Exozodiacal Dust 7.2.3 Priority 3: Signs of Life In Phase A the details will need to be defined of the spectrometers, filters, dichroics, and operating wavelengths of various instruments within TPF-I. The instruments will be optimized for the detection of known biomarkers. Our understanding of biomarkers must have advanced sufficiently during Phase A to set requirements for the detailed instrument designs. The spectroscopic resolution is another key parameter that defines the scientific scope. Because the planet signals are very faint, the spectroscopic resolution translates very directly into a sensitivity requirement. How long does it take to perform spectroscopic follow-up of a significant number of detected planets The resolution needed is, of course, a question that must be answered using our best understanding of the geophysical, atmospheric, and astrobiological processes that may be present on planets that TPF-I detects. 7.2.4 Priority 4: Exozodiacal Dust Observations to characterize exozodiacal dust will continue to be important during Phase A and also in the phases through launch. Activities in this science theme will contribute to characterizing the stars in the list of target stars. 7.3 Phases B and C/D In Phase B, C, and D, preparatory science will emphasize the preparation of a mission whose capability is already well defined. Studies will emphasize further development of the target list, understanding the environment of the target stars, and determining the best strategy to maximize the scientific return of the mission. A coordinated program will continue to observe and characterize all potential target stars and to establish a standardized database and archive of measurements. The target lists will be refined and prioritized to identify target stars most likely to harbor Earth-like planets. Observations with SIM PlanetQuest will be a particularly important component of this final step of characterization. 163
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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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C HAPTER 2 Figure 2-6. The mid-infr
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C HAPTER 2 Lines of constant stella
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C HAPTER 2 presence of zodiacal clo
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C HAPTER 2 S EZ 2π ∫ θ max ∫
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C HAPTER 2 Figure 2-11. Observation
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C HAPTER 2 Figure 2-12. Models of t
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C HAPTER 2 Beichman, C. A., Fridlun
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C HAPTER 2 2.7.4 Suitable Targets E
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C HAPTER 2 Reach, W. T., Franz, B.
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C HAPTER 3 3.1.1 Darwin/TPF-I Prope
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C HAPTER 3 clouds or an OB associat
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C HAPTER 3 Figure 3-3. Three possib
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C HAPTER 3 the circumstellar disk,
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C HAPTER 3 Figure 3-6. (Left panel)
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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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Page 132 and 133: C HAPTER 5 a) c) b) d) IWA = 43 mas
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Page 145 and 146: T E C H N O L O G Y R OADMAP FOR TP
Page 173 and 174: F UTURE D EVELOPMENTS 7 Preparatory
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Page 183 and 184: T E C H N O L O G Y A DVISORY C O M
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Page 208 and 209: A PPENDIX E Appendix E TPF-I Review
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