TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 7 Up until launch, preparatory science activities will aid in preparations for each mission: undertaking complementary observations of the target stars, establishing databases of standardized measurements, and refining techniques for the detection of biomarkers. There will be a wide variety of activities focused on improving the scientific productivity of the missions. 164
D ISCUSSION AND C ONCLUSION 8 Discussion and Conclusions The goal of NASA’s Navigator program is to find terrestrial planets and to search for life. We must find potentially habitable planets, (e.g., 0.5 to 10 Earth mass) located in or near the habitable zone of their parent stars, characterize their physical properties in terms of our growing knowledge of conditions that might be hospitable for the formation and stable evolution of life, and determine their atmospheric constituents or surface composition by looking for specific biomarkers (O 2 , O 3 , chlorophyll) or, more generally, the disequilibrium processes that might be attributable to the presence of life. As outlined in Chapters 1 and 2, this program is an ambitious one requiring the determination of masses via astrometry (with SIM PlanetQuest) and the detection of optical photons (with TPF-C) and mid-IR photons (with TPF-I/Darwin). In addition, TPF-I will address the cradle-to-grave evolution of stellar systems, specifically; the early evolution of star and planet formation, stellar and planetary death and cosmic recycling, the formation and evolution of Black holes, and galaxy formation and evolution. The main areas of focus for TPF-I in the past 3 years have been on architecture selection with emphasis on reducing sources of systematic noise and on technology development in the areas of starlight nulling and formation flying. In a 5-year mission, the X-array architecture using four 3.5-m telescopes has the capability to: a) Survey at least 150 F, G, K, and nearby M stars with at least three visits each; b) Make spectroscopic observations of the planets detected around at least 10 stars looking for O 3 , CO 2 , H 2 O, and possibly other species that are trace constituents in the Earth’s atmosphere but which might be abundant in alien atmospheres such as CH 4 and N 2 O; c) Carry out a program for general astrophysics probing the 3-μm to 20-μm wavelength region with unprecedented μJy sensitivity and milli-arcsecond angular resolution. We have also examined in a cursory way the scientific capabilities of a reduced TPF-I mission consisting of four 3.2-m telescopes on a 36-m boom. While this configuration would be severely limited compared to the full TPF-I/Darwin mission, because of its limited angular resolution, it would be able to measure the mid-IR emission of nearby terrestrial planets found with other missions (SIM and/or TPF-C) in a number of broad-band colors and to look for the broadest spectral lines in a few of the brightest planets. If terrestrial planets prove to be common, nearby, and bright, a reduced version of TPF-I might be worth considering as a first probe of the infrared properties of planets. As outlined in this report a cadre of capable scientists and engineers around the country (and in Europe) are making steady progress on the precursor science and enabling technologies. Stable nulls deeper than10 -4 have been achieved with a spectral bandwidth of 32%. Deeper nulls of 10 -6 have been achieved in narrow laser bandpasses. Simulated planetary signals two million times fainter than a simulated star have been extracted using the Planetary Detection Testbed. The formation-flying testbeds are developing 165
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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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C HAPTER 5 Heavy launch vehicle. Th
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C HAPTER 5 5.3.2 Combiner Spacecraf
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C HAPTER 5 5.3.5 Beam Transfer betw
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C HAPTER 5 Figure 5-8. Control sche
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C HAPTER 5 Figure 5-9. First sectio
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C HAPTER 5 Figure 5-9 shows the fir
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C HAPTER 5 5.4.4 Shear Metrology Sh
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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-
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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 and 174: F UTURE D EVELOPMENTS 7 Preparatory
Page 175 and 176: F UTURE D EVELOPMENTS • To comple
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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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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
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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
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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
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TPF-I SWG Report - Exoplanet Exploration Program - NASA

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