TPF-I SWG Report - Exoplanet Exploration Program - NASA

More documents

Recommendations

Info

C HAPTER 6 Pedretti, E., et al., “First images on the sky from a hypertelescope,” Astron. Astrophys. Sup. Ser.147, 285–290 (2000). Quirrenbach, A. et al. “The PRIMA astrometric planet search project,” New Frontiers in Stellar Interferometry, Proc SPIE 5491, edited by W. A. Traub, 424–432 (2004). Rinehart, S. A. et al., “The wide-field imaging interferometry testbed: recent results,” Advances in Stellar Interferometry, Proc. SPIE 6268, edited by J.D. Monnier, M. Schöller, and W. C. Danchi, 626836 (2006). 158
F UTURE D EVELOPMENTS 7 Preparatory Science for TPF-I The development of precursor science for TPF-I is shown schematically in Fig. 7-1, which highlights the major project phases and gate reviews. In green, we indicate the most significant programmatic decisions the mission must face. In the sections below, we describe in more detail how scientific questions feed directly into the decisions that TPF-I faces during its development. 7.1 Pre-Phase A In Pre-Phase A, the focus of TPF-I science will be to contribute to the Mission Concept Review that will allow TPF-I to enter Phase A of its project life cycle. Key questions will include the level of exozodiacal emission and its influence on the designs of interferometer architectures, an assessment (mostly complete) of the spectral markers for TPF-I, and an initial selection of appropriate target stars. 7.1.1 Priority 1: Exozodiacal Dust For the interferometer, a driving requirement is the need to suppress or reject starlight so that planet light can be detected. Moreover, atmospheric spectroscopy must be possible within the bands of biomarkers that have been identified. A starlight rejection of ~ 10 5 –10 6 :1 is needed for a mid-IR interferometer. Previous architecture studies have shown that the brightness of dust in the habitable zone of the target star adversely affects the integration time necessary to detect planets. Thus, in addition to a critical assessment of the technology needed for each architecture, it is important to characterize and understand the brightness of the average exozodiacal emission surrounding potential target stars prior to the Mission Concept Review. • A survey of a representative sample of target stars for dust on all orbital scales, from < 1 AU out to 100 AU, is important for both the mission concept review and selection of preliminary targets. Although selected stars may be studied through individual peer-reviewed proposals, a program coordinated between NASA and ESA is needed that will make the best use of missions such as Spitzer and Herschel. • The TPF-I and Darwin Projects should also work to coordinate and make best use of upcoming ground-based facilities, such as the nulling instruments at KI and LBTI. • Our understanding of levels of exozodiacal dust and the relation of those levels to the search for planets would be further bolstered by strong support for a wide-ranging program of theory and modeling. 159
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
Page 36 and 37:
C HAPTER 2 Figure 2-6. The mid-infr
Page 38 and 39:
C HAPTER 2 Lines of constant stella
Page 40 and 41:
C HAPTER 2 presence of zodiacal clo
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
Page 75 and 76:
Page 77 and 78:
Page 79 and 80:
Page 81 and 82:
Page 83 and 84:
Page 85 and 86:
Page 87 and 88:
Page 89 and 90:
Page 91 and 92:
Page 93 and 94:
Page 95 and 96:
Page 97 and 98:
Page 99 and 100:
Page 101 and 102:
Page 103 and 104:
Page 105 and 106:
Page 107 and 108:
Page 109 and 110:
Page 111:
Page 114 and 115:
C HAPTER 5 Heavy launch vehicle. Th
Page 116 and 117:
C HAPTER 5 5.3.2 Combiner Spacecraf
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
Page 122 and 123: C HAPTER 5 Figure 5-9. First sectio
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 138 and 139: C HAPTER 5 5.8.4 Angular Resolution
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 171: T E C H N O L O G Y R OADMAP FOR TP
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
Page 187: F L I G H T S YSTEM C ONFIGURATION
Page 190 and 191: A PPENDIX C 2. Identical FACS fligh
Page 192 and 193: A PPENDIX C 2. Recall that the coef
Page 194 and 195: A PPENDIX C Once the formation has
Page 196 and 197: A PPENDIX C Figure C-3. Example of
Page 198 and 199: A PPENDIX C Figure C-4. FAST Flight
Page 200 and 201: A PPENDIX C The “true” time of
Page 202 and 203: A PPENDIX C References Cohen, S., a
Page 204 and 205: A PPENDIX D DC DCB DM DM DOCS DOD D
Page 206 and 207: A PPENDIX D NaCl NAR NASA NASTRAN N
Page 208 and 209: A PPENDIX E Appendix E TPF-I Review
Page 210 and 211: A PPENDIX F Alice Quillen, Universi
Page 212: A PPENDIX F Figure 3-1 - Original f
show all

TPF-I SWG Report - Exoplanet Exploration Program - NASA

Create successful ePaper yourself

Delete template?

Save as template?