TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 5 5.8.4 Angular Resolution and Imaging The imaging properties of nulling arrays are discussed in Section 4.9. Angular resolution—essentially the width of the main peak in the point spread function—is distinct from the IWA discussed in Section 5.8. A key feature of the stretched X-array is its excellent angular resolution, resulting from the long imaging baselines. Figure 5-25 compares synthesized dirty maps for the regular X-array 2:1 and the stretched X- array 6:1. The IWA is the same in each case, but the angular resolution is improved by a factor of 3. The angular resolution scales linearly with wavelength and is inversely proportional to the array size, as illustrated in Table 5-3. High angular resolution is highly desirable for (1) separating the contributions of multiple planets; (2) rapid and unambiguous orbit determinations; and (3) discrimination against lumps in the exozodiacal disk. For previous arrays with relatively poor angular resolution, image deconvolution was considered to be a major issue, since there can be substantial overlap between the PSFs of different sources. Sidelobes and satellite peaks can combine to produce false peaks or mutually cancel and prevent detection. The greatly enhanced angular resolution of the stretched X-array (Fig. 5-25b) minimizes these overlaps, and it should go a long way to retiring these issues. Figure 5-25. (a) Dirty map of two planets (indicated by the × symbols), synthesized from multichannel observations of an X-array 2:1 array configuration (70 × 35 m); (b) Equivalent dirty map for the stretched X-array 6:1 configuration (210 × 35 m). 124
<strong>TPF</strong>-I F L I G H T B ASELINE D ESIGN Figure 5-26. Examples of u-v coverage and dirty beam profiles for the stretched X-array in snapshort and full configuration. Snapshot: (left column) 10-μm wavelength, 5 h on 3 targets with calibrator (1.7 h per target), 180-degree array rotation over a baseline range from 20 to 60 m on the short side of the rectangle. Beam FWHM = 3.9 × 3.4 mas and highest sidelobe is 20%. Full: (right column) 6-μm wavelength, 12 h on 1 target with calibrator, 360-degree rotation over full baseline range (20 to 100 m on short side of rectangle). Beam FWHM = 1.5 × 1.2 mas and highest sidelobe is 10%. 125
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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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Page 87 and 88: 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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Page 124 and 125: C HAPTER 5 Figure 5-9 shows the fir
Page 126 and 127: C HAPTER 5 5.4.4 Shear Metrology Sh
Page 128 and 129: C HAPTER 5 Figure 5-15. TPF-I Fligh
Page 130 and 131: C HAPTER 5 secondary mirror along t
Page 132 and 133: C HAPTER 5 a) c) b) d) IWA = 43 mas
Page 134 and 135: C HAPTER 5 planets found. Figure 5-
Page 136 and 137: C HAPTER 5 30 25 5 M earth 3 M eart
Page 140 and 141: C HAPTER 5 Table 5-3. Angular Resol
Page 142 and 143: C HAPTER 5 The optimization works b
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
Page 175 and 176: F UTURE D EVELOPMENTS • To comple
Page 177 and 178: F UTURE D EVELOPMENTS Table 7-1. Pr
Page 179 and 180: D ISCUSSION AND C ONCLUSION 8 Discu
Page 181 and 182: Appendices 167
Page 183 and 184: T E C H N O L O G Y A DVISORY C O M
Page 185 and 186: 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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