TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 2 Lines of constant stellar type 30.00 Diameter of circle proportional to intrinsic diameter of star 25.00 F0 Distance / pc 20.00 15.00 G0 F9 10.00 G9 K0 5.00 K9 M0 0.00 0 50 100 150 200 Projected IHZ / mas Figure 2-7. Candidate targets for TPF-I. Each of the 1014 candidate stars is represented by a circle with a diameter proportional to the diameter of the star (intrinsic, not angular diameter). Curves show loci of a given spectral type. Beyond the distance criterion, at this early phase it is desirable to keep the number of culling criteria as small as possible. The scientific target stars can be summarized quite simply: bright, nearby, solar-like, main-sequence stars for which a binary companion is not too close. This statement translates in straightforward fashion to the detailed technical requirements listed in Table 2-3. The final column in this table gives the number of potential target stars remaining after the set of culls down to a given line has been applied. Even after all applicable science culls have been applied, over 1000 suitable targets remain. These 1014 stars are plotted in Fig. 2-7 on a space of stellar distance vs. projected inner habitable zones size, from which it can be seen, e.g., that for a sizable candidate population of stars to be observable, an inner working angle of 50 milliarcsecond (mas) or smaller is needed. The final candidate list of 1014 stars was used to predict the performance of different TPF-I architectures. 2.5.2 Engineering Criteria Next one also needs to include instrumental or engineering constraints which can eliminate certain classes of stars. With the current baseline design of TPF-I, these fall into two categories. First, sunshade constraints limit observations to stars within 45° of the ecliptic. Second, control of stray light implies that any bright companion stars must be more than 10 arcsec away from the target star of interest. As Table 2-2 shows, this eliminates about 40% of the scientifically interesting stars. 24
E X O P L A N E T S CIENCE Table 2-3. Science and Engineering Criteria for Selection of TPF-I Candidate Targets Parameter Constraint Remaining Stars Science Culls Distance (Hipparcos catalog) < 30 pc 2350 Apparent magnitude < 9 1299 Bolometric luminosity < 8 1284 Luminosity class IV, V 1247 B-V index > 0.3 1184 Variability < 0.1 1143 Companions further than 50 AU 1014 Engineering Culls After science culls 1014 Field of regard |Ecliptic latitude| < 45 deg 650 Multiplicity Separation > 10" 620 2.6 Exozodiacal Dust 2.6.1 Zodiacal Dust as a Constituent of Planetary Systems The presence of dust around a mature, main-sequence star is a reminder that the star was born by accretion in a dense protostellar disk of gas and dust and that any planets possessed by the star were born out of that same material. The dust around a mature star is not itself primordial, since radiative forces will remove small dust grains in a few thousands to a few millions of years. However, the parent bodies of the observed small dust grains—large numbers of either asteroids or comets—are the remnants of primordial material, and the debris within them provides hints to the origin of planetary systems. Additionally, this solid material is important in the evolution of life, since the cold outer reaches of a planetary system are rich in water and volatiles needed for the creation of habitable environments in the inner reaches of the system. Thus, we want to study the exozodiacal clouds of nearby stars for their intrinsic scientific importance using a variety of observational facilities, including TPF-I/Darwin and TPF-C. Yet the brightness of the exozodiacal cloud is also a potential problem for the detection of terrestrial planets due to increased photon noise and confusion between planets and structures in the zodiacal cloud. Thus, the incidence, distribution and composition of material in the habitable zones of nearby stars are important for the design of TPF-I or TPF-C and for the feasibility of studying individual targets. After a brief discussion about the impact of photon noise from exozodiacal emission on both visible-light and mid-IR instruments, we summarize recent observational results, discuss theoretical expectations for the level of exozodiacal emission, and describe future observational programs relevant to determining the level of exozodiacal emission around typical TPF targets. We will show that TPF-I can operate in the 25
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
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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
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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
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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
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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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C HAPTER 5 Figure 5-15. TPF-I Fligh
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C HAPTER 5 secondary mirror along t
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C HAPTER 5 a) c) b) d) IWA = 43 mas
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C HAPTER 5 planets found. Figure 5-
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C HAPTER 5 30 25 5 M earth 3 M eart
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C HAPTER 5 5.8.4 Angular Resolution
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C HAPTER 5 Table 5-3. Angular Resol
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C HAPTER 5 The optimization works b
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T E C H N O L O G Y R OADMAP FOR TP
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F UTURE D EVELOPMENTS 7 Preparatory
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F UTURE D EVELOPMENTS • To comple
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F UTURE D EVELOPMENTS Table 7-1. Pr
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D ISCUSSION AND C ONCLUSION 8 Discu
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Appendices 167
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T E C H N O L O G Y A DVISORY C O M
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F L I G H T S YSTEM C ONFIGURATION
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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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