TPF-I SWG Report - Exoplanet Exploration Program - NASA

More documents

Recommendations

Info

C HAPTER 7 7.1.2 Priority 2: Frequency of Terrestrial Planets Improved knowledge of extrasolar planetary systems will allow us to predict with greater certainty the scientific return from TPF-I. This question has highest priority once each mission enters Phase A, and therefore should have a high priority in the preceding years. • A comprehensive theoretical investigation into many aspects of the formation and evolution of planets and planetary systems must provide the framework within which to understand necessarily incomplete observational results. The combination of the existing and near-term radial velocity and transit programs—with theoretical insights into the orbital stability of planets, planetary migration, and the relationship between gas giants and rocky planets—will further enrich our understanding of extrasolar planetary systems. • Our current understanding of the frequency of Earth-like planets is based on observations of highermass planets discovered through radial velocity surveys, transit surveys, and on inferences from gravitational microlensing results. These highly successful programs should be further supported and encouraged as new detections of lower-mass and longer-period planets continue to refine our estimate of the frequency of Earths. • Radial velocity surveys would be better supported through the development of new specialized highresolution échelle spectrometers to offset the current demand for these instruments. Investments in new equipment for radial velocity surveys, directed also at under-used 2–3-m class telescopes, would represent an excellent strategy in the development of workhorse instruments for exoplanet detection. • The space-based missions CoRoT (CNES/ESA, launched in 2006) and Kepler (NASA, launch in 2009) hold great promise for identifying transiting planets down to an Earth radius around stars located 100–1000 pc away. With these missions we will determine the statistical incidence of terrestrial planets and, with suitable follow-up, new insights into the physical state of these distant planets. Ground-based transit surveys should also be encouraged. Of special interest is the development of a worldwide network of dedicated wide-field transit or microlensing search telescopes that would allow follow-up studies of bright targets. 7.1.3 Priority 3: Target Stars The quality of science that will be derived from TPF-I will be partly determined by the stars included in the final target list. A preliminary list of stars will greatly assist in judging the technical feasibility of the mission concepts. This preliminary target list may include a larger number of stars than are retained in the final list. • The TPF-I project needs to determine which stellar parameters are most relevant to the search for life. These parameters, once known, will need to be monitored over time for the stars included in the target list. Spectroscopic observations over a broad range of wavelengths will be needed with coordinated access to appropriate space observatories run by NASA and ESA. The TPF-I and Darwin projects should work with NASA and ESA to ensure a coordinated observing program to observe target stars. 160
F UTURE D EVELOPMENTS • To complement the studies of nearby stars and potential targets, adequate support is needed for the development and maintenance of comprehensive databases and archives relevant to planet searches. A database, or central clearing-house, with active solicitations to provide missing information (colors, radial velocities, photometric variability, metallicities, binarity, interferometric measurements of diameters, etc.) should be established in Pre-Phase A. 7.1.4 Priority 4: Signs of Life The technical requirements for the architectures of both coronagraphs and interferometers are dependent upon the wavelength range, or spectral bandpass, that is necessary to detect evidence of life. In particular, the shortest operating wavelength determines the required surface smoothness of optics and the mechanical stability of the observatory. The need for better starlight suppression would push the designs to use longer wavelengths, but amongst mid-IR biomarkers the relatively short-wavelength water-vapor band at 6.3 μm may prove the most sensitive and easiest to interpret—forcing a tightening of requirements of a mid-IR interferometer design. The necessary spectral bands of visible and mid-IR biomarkers must be known if the design team is to provide instruments tailored to TPF-I’s needs. To explore the plausible range of terrestrial planets that we may find, it is important to create selfconsistent theoretical models of planetary characteristics and evolution. These models will help to refine Figure 7-1. Summary schedule identifying the mission phases and science gates for the Terrestrial Planet Finder Missions. 161
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 173: F UTURE D EVELOPMENTS 7 Preparatory
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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?