TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 2 Table 2-2. Illustrative Properties of a TPF-I Observatory Concept* Parameter Telescopes 4-Telescope Dual Chopped Bracewell Design Four 4-m diameter telescopes, diffraction limited at 2 μm operating at 40 K Array size 60–150 m center-to-center of outer telescope in linear array Baseline range 40–100 m Wavelength range 6.5–15 µm, with the goal of 6.5–18 µm Angular resolution (maximum) 50–75 milli-arcseconds Field-of-view 1 arcsec at 12 µm Spectral resolution Δλ/λ 25 with a goal of 50 Sensitivity 0.35 µJ at 12 µm Number of stars 150 Biomarkers H 2 O and O 3 with a goal of also measuring CO 2 and CH 4 Field of regard ±45° of anti-Sun direction Orbit L2 Halo orbit Mission duration 5 years baseline with a goal of 10 years Mission launch 2019 with Heavy-class launch vehicle, Delta 4050H *Further details are available in Appendix B Visitations Multiple visits per star will be required to achieve required completeness, to distinguish it from background objects, to determine its orbit, and to study a planet along its orbit. TPF-I must be capable of making at least 3 visits to each star to meet the completeness and other requirements. Multiple Planets After the completion of the required number of visitations defined above, TPF-I should be able to characterize a planetary system as complex as our own with three terrestrial-sized planets assuming each planet is individually bright enough to be detected. Orbit Determination After the completion of the required number of visitations defined above, TPF-I shall be able to localize the position of a planet orbiting in the habitable zone with an accuracy of 10% of the semi-major axis of the planet’s orbit. This accuracy may degrade to 25% in the presence of multiple planets. 12
E X O P L A N E T S CIENCE 25 mag, 10 billion 17.5 mag, 10 million Figure 2-1. The Solar System seen from 10 pc illustrates the challenge of TPF-C and TPF-I, where the Earth-Sun contrast is 10 7 in the mid-infrared and 10 10 in the visible. (Traub and Jucks 2002) 2.1.2 Observing Modes Imaging The interferometer will be capable of imaging in the nulling mode and in the classical mode of constructive interference. This is to meet major science goals in the areas of: • Star and planet formation and early evolution. • Stellar and planetary death and cosmic recycling. • The formation, evolution, and growth of black holes. • Galaxy formation and evolution over cosmic time. Nulling • Sensitivity: A point source of 1 μJy should be detectable with a signal divided by noise (S/N) of 5 in one hour’s integration time • Baseline Lengths: Maximum 200 meters 13
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 and 16: I NTRODUCTION 1 Introduction Over 2
Page 17 and 18: I NTRODUCTION et al. 2004), and res
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 28 and 29: C HAPTER 2 Classical interferometry
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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
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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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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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