TPF-I SWG Report - Exoplanet Exploration Program - NASA

More documents

Recommendations

Info

C HAPTER 2 0.7 to 1.5 AU scaled by the square root of stellar luminosity. The minimum terrestrial planet must be detectable at the outer edge of the HZ. • Orbital Phase Space: The distribution of orbital elements of terrestrial type planets is presently unknown, but observations suggest that giant-planet orbits are distributed roughly equally in semi-major axis, and in eccentricity up to those of the Solar System planets and larger. Therefore, TPF-I must be designed to search for planets drawn from uniform probability distributions in semi-major axis over the range 0.7 to 1.5 AU and in eccentricity over the range 0 to 0.35, with the orbit pole uniformly distributed over the celestial sphere with random orbit phase. Giant Planets The occurrence and properties of giant planets may determine the environments of terrestrial planets. The TPF-I field of view and sensitivity must be sufficient to detect a giant planet with the radius and geometric albedo or effective temperature of Jupiter at 5 AU (scaled by the square root of stellar luminosity) around at least 50% of its target stars. A signal-to-noise ratio of at least 5 is required. Exozodiacal Dust Emission from exozodiacal dust is both a source of noise and a legitimate target of scientific interest. TPF-I must be able to detect planets in the presence of zodiacal clouds at levels up to a maximum of 10 times the brightness of the zodiacal cloud in the Solar System. Although the average amount of exozodiacal emission in the “habitable zone” is not yet known (see Section 2.6), we adopt an expected level of zodiacal emission around target stars of 3 times the level in our own Solar System with the same fractional clumpiness as our Solar System’s cloud. From a science standpoint, determining and understanding the properties of the zodiacal cloud is essential to understanding the formation, evolution, and habitability of planetary systems. Thus, TPF-I should be able to determine the spatial and spectral distribution of zodiacal clouds with at least 0.1 times the brightness of the Solar System’s zodiacal cloud. Spectral Range The required spectral range of the TPF-I mission for characterization of extrasolar planets will emphasize the characterization of Earth-like planets and is therefore set to 6.5 to 18 µm in the infrared. The minimum range is 6.5 to 15 µm. Spectrum The TPF-I mission will use the spectrum of a planet to characterize its surface and atmosphere. The spectrum of the present Earth, scaled for semi-major axis and star luminosity, is used as a reference and suggests a minimum spectral resolution is 25 with a goal of 50. TPF-I must measure water (H 2 O) and ozone (O 3 ) with 20% accuracy in the equivalent width of the spectral feature. Additionally it is highly desirable that TPF-I also be able to measure carbon dioxide CO 2 ) as well as methane (CH 4 ) (if the latter is present in high quantities predicted in some models of pre-biotic, or anoxic planets, e.g. Kasting et al. 2003). 10
E X O P L A N E T S CIENCE Table 2-1. TPF-I Science Requirements Parameter TPF-I Requirement Star Types F, G, K, selected, nearby M, and others Habitable Zone 0.7–1.5 AU scaled as L 1/2 Number of Stars to Search 150 Completeness for Each Core Star 90% Minimum Number of Visits per Target 3 Minimum Planet Size 0.5–1.0 Earth Area Geometric Albedo Earth’s Spectral Range and Resolution 6.5–18 μm; R = 25 [50] Characterization Completeness Spectra of 50% of Detected or 10 Planets Maximum Giant Planets Jupiter Flux, 5 AU, 50% of Stars Maximum Tolerable Exozodiacal Emission 10 times Solar System Zodiacal Cloud Number of Stars to be Searched To satisfy its scientific goals, TPF-I should detect and characterize a statistically significant sample of terrestrial planets orbiting F, G, and K stars. Although at this time, the fractional occurrence of terrestrial exoplanets in the Habitable Zone is not known, a sample of 150 stars within 30 pc (including a small number of nearby M stars) should suffice based on our present understanding. Extended Number of Stars It is desired to search as many stars as possible, beyond the required core sample. We anticipate that any mission capable of satisfying these objectives will also be capable of searching many more stars if the overall requirements on completeness are relaxed. It is desired that TPF-I be capable of searching an extended group of stars defined as those systems of any type in which all or part of the continuously habitable zone (see below) can be searched. Search Completeness Search completeness is defined as that fraction of planets in the orbital phase space that could be found within instrumental and mission constraints. We require each of the 150 stars to be searched at the 90% completeness level. For other targets in addition to the 150 stars, the available habitable zone will be searched as to limits in planet's orbital characteristics. Characterization completeness While it will be difficult to obtain spectra of the fainter or less well positioned planets, we require that TPF-I be capable of measuring spectra of at least 10 (~50%) of the detected planets. 11
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 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:
D ESIGN AND A R C H I T E C T U R E
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 147 and 148:
Page 149 and 150:
Page 151 and 152:
Page 153 and 154:
Page 155 and 156:
Page 157 and 158:
Page 159 and 160:
Page 161 and 162:
Page 163 and 164:
Page 165 and 166:
Page 167 and 168:
Page 169 and 170:
Page 171 and 172:
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
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?