TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 2 presence of zodiacal clouds 10–20 times as bright as our own without undue difficulty and that systems with this amount of emission, or considerably less, are likely to be common among mature solar-type stars. 2.6.2 Zodiacal Emission as a Source of Noise For a cryogenic nulling interferometer operating in an orbit near 1 AU the three dominant noise sources are (Angel and Woolf 1997; Beichman and Velusamy 1999): stellar light that leaks past the interferometric null because of the finite diameter of the star, S *,Leak ; emission from the local zodiacal dust, S LZ ; and emission from the exozodiacal dust in the target system that leaks past the interferometer, S EZ,Leak (Figure 2-8). At short wavelengths (
E X O P L A N E T S CIENCE Figure 2-8. The variation of signal-to-noise for planet detection as a function of exozodiacal brightness for three cases: TPF-I for large grain emission; TPF-I for small grain emission; and TPF-C. The parameter μ LZ is the ratio of surface brightness of the exozodiacal cloud in the habitable zone of a target star to that of our own zodiacal cloud. In the absence of more detailed information, the vertical optical depth of the exozodiacal dust in any system can be parameterized as a factor, μ EZ , times the optical depth of our Solar System's dust cloud. The emission from exozodiacal dust is then S EZ (r) = 2 μ EZ τ LZ (r) B ν (T(r)) Ω tel , where the factor of two accounts for the fact that in the exozodiacal case we are looking through the entire cloud and not from the vantage of the mid-plane as we do locally. By analogy with the local zodiacal cloud (Backman 1998), the vertical optical depth is assumed to fall off radially as τ LZ (r) = τ LZ (1 AU)r AU -0.3 . We also take T(r) = T 0 r AU β as the equilibrium temperature for grains heated by stellar radiation and emitting in the infrared. Typical 1-AU values of (T 0 , β) for large and small silicate grains are (255 K, –0.5) and (362 K, –0.4), respectively (Draine and Lee 1984; Backman and Paresce 1993; Beichman et al. 2006a). For reference, it is worth nothing that the integrated signal from a Solar-System-equivalent exozodiacal cloud is a few hundred times brighter than the signal from an Earth twin. The effect of exozodiacal emission is, however, reduced by the fringe pattern of the interferometer which attenuates the bright central portion of the exozodiacal disk. To account for this effect, we incorporate the fringe pattern of a particular nulling scheme, ξ(θ,ϕ), where θ and ϕ are the radial and azimuthal variables, respectively. In the simplified case of a face-on disk, the signal reaching the detector, S EZ, Leak , is then given by the integral of S EZ over the fringe pattern and the telescope solid angle: 27
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 26 and 27: C HAPTER 2 Table 2-2. Illustrative
Page 28 and 29: C HAPTER 2 Classical interferometry
Page 30 and 31: C HAPTER 2 trivial in the absence o
Page 32 and 33: C HAPTER 2 Figure 2-3. Simulated mi
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 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
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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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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