TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 4 Channel SNR 10.0 Channel SNR 1.38 / rotn # rotations 53 Planet signal rms Random noise Systematic noise 0.091 /s 0.042 /s 0.051 /s Local Zodi leak Stellar size leak Null floor leak photon noise photon noise photon noise 0.027 /s 0.033 /s 0.006 /s Planet signal rms Local Zodi leak Stellar size leak Null floor leak Null stability 0.091 /s 2.3E-08 71 /s 1.8E-05 106 /s 2.6E-05 3 /s 7.5E-07 at planet harmonics 1.3E-08 Amp-phase error ΔA Δφ / rad 0.13% 0.0011 Dynamic Control systems Fringe track Metrology Tip/tilt Shear Disturbances Beamtrain Static Coatings Reflectivity Alignment Beam combiner π phase sh Figure 4-5. Simplified TPF-I error budget for the signal-to-noise ratio (SNR) required for ozone detection at 10-μm wavelength. 4.2 Performance Models The two key performance models are described in this section: the Interferometer Performance Model (IPM) for predicting the SNR on a specified target; and the Star Count Model for estimating the number of targets that can be surveyed over the duration of the mission. 4.2.1 Interferometer Performance Model The TPF Interferometer Performance Model (IPM) is maintained as a series of Excel spreadsheets and is used both to estimate the performance of different architectures, and to derive the requirements for the baseline design. The spreadsheet performance model is run as a bottom-up calculation; that is, the overall performance is calculated based on the specified low-level inputs (as opposed to a top-down suballocation approach). The inputs can be adjusted and balanced until the desired output performance is obtained, at which point the input values assumed become the requirements on the instrument. 64
D ESIGN AND A R C H I T E C T U R E T RADE S TUDIES Total SNR Calculate all chans! 41.15 Weighted combination Channel # 21 Channel SNR Channel SNR Channel SNR Total time Calculate Chan # 21 32.41 days single chan! 9.22 2800000 s SNR sqrt(n) n Channel SNR # rotations Rotation time Chan # 21 1.23 / rotn 56 50000 s P / RSS(R,S) P R S Planet signal rms Random noise Systematic noise 8.05E-02 / s 5.52E-02 / s 3.50E-02 / s Cross-correlate sqrt[(A+B)/2T] RSS A B T Planet Template Planet vs time Detector noise Photon rate Rotation time Chop asymmetry Chop freq. terms equivalent / s 21.0 / s 2.83E+02 / s 50000 s 3.18E-02 / s 1.46E-02 / s D 2 + E RSS RSS sum Analysis Read noise LZ Detector gain 4/ read D 1.37E-02 / s Thermal Cross-terms Thermal 2.85E-03 / s 6.97E-05 / s 2.54E-02 / s 1.00E+00 / Hz Dark current EZ leak Stray Configuration E 2.85E-03 / s X-Array Co-phase 5/ s Stray 5.27E+01 / s 1 / Hz @ f chop Poln angle 1.00E+01 / s 2.27E-03 / s 2.53E-03 / s Stellar leak Amp & Phase Wavelength Ozone 1.44E+02 / s Other chop asymm. 1.86E-03 / s 9.74 um Calculate! 1.89E-02 / s Null floor Chop frequency Planet offset f chop 5.61E+00 / s 0.1 Hz 0.050 arcsec Analysis Analysis Analysis Planet per coll. Star per coll. EZ per coll. LZ per coll. EZ inc / pos angle Star diameter Noise coupling coeffs Configuration PSD(pol angle) 30 deg lat 30 deg 15 pc X-Array 9.39E-02 / s 1.01E+06 / s 1.04E+02 / s 7.13E+01 / s 30 deg 1.0 R sun 1.60E-03 rad rms Product Product Product Product Cross-correlation Planet flux Stellar flux EZ flux LZ flux Null power spectrum Planet power spectrum contributions Calculate! Convolution Product Product Analysis LZ brightness PSD(A+) PSD(φ+) Planet offset Collecting area Throughput Channel BW Interpolated Interpolated 4.32E+00 /Hz/m 2 /s/sr 1.3E-03 rms 1.1E-03 rms 0.050 arcsec 12.57 m 2 0.10 1.58E+12 Hz Interpolate! Solid angle Rotation time Configuration X-Array 1.4 (λ / D) 2 50000 s SNR Optics PSD Interpolation Wavelength Targets Spectral Variances Ozone Wavelength 9.74 um Ozone Config Planet signal Perturbation 9.74 um Error budget PSD(A+) PSD(φ+) Look-up Look-up s Figure 4-6. Full TPF-I Error Budget for a Single Spectral Channel 65
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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
Page 28 and 29: C HAPTER 2 Classical interferometry
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Page 32 and 33: C HAPTER 2 Figure 2-3. Simulated mi
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Page 36 and 37: C HAPTER 2 Figure 2-6. The mid-infr
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
Page 46 and 47: C HAPTER 2 Figure 2-12. Models of t
Page 48 and 49: C HAPTER 2 Beichman, C. A., Fridlun
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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
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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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