TPF-I SWG Report - Exoplanet Exploration Program - NASA

More documents

Recommendations

Info

C HAPTER 1 angled Three Telescope Nuller with a dedicated beam combiner spacecraft to alleviate the complexity of the beam relay, and sufficient asymmetry to improve the imaging properties. The focus at NASA was on improving the imaging properties of the array, which is important for separating the contributions from multiple planets, determining the orbit, and discriminating against lumps in the exozodiacal emission. This led to a rearrangement of the collectors in the Linear DCB to produce the X-Array – a configuration in which the nulling baselines lie along the short side of the rectangle and the imaging baselines (which determine the angular resolution) along the long dimension. The beams are relayed in a single hop from each collector to a central combiner. The decoupling of the nulling and imaging baselines makes the X-Array more flexible than other configurations. This flexibility was subsequently exploited to eliminate ‘instability noise’ with the ‘Stretched X-Array’ design. Instability noise—an analog of speckle noise in the coronagraph—arises from fluctuations in the path lengths, pointing, dispersion, etc. of the instrument, and drives the requirement on the null depth down to 10 -6 . The long imaging baselines of the Stretched X-Array give the planet signals a unique spectral signature that can be effectively separated from the instability noise, and they also greatly improve the angular resolution of the instrument. The configurations above are defined by the relative location of the collectors. Until recently, the combiner spacecraft was always located in the same plane as the collectors, normal to the direction to the target star. ESA then proposed the ‘Emma’ architecture, in which the combiner is moved out towards the star by about 1 km, and the collectors are reduced to a single spherical mirror. Most of the nulling configurations already described can be implemented in either the classic planar format or the out-ofplane Emma format. The Emma design offers significant advantages which are presently being studied independently by ESA and NASA. Preliminary results of these studies were first reported very recently, only in the later half of 2006, and are therefore not within the scope of this document. The appeal of the Emma design is primarily in its simplification of the telescope optics, eliminating the need for any deployables, and also in the design of the sunshields, which become folded into a hard shell—thereby reducing the risk of catastrophic failure. However, the simplification of the telescope optics increases the complexity of the beam combiner, and it currently is not known to what extent this will reduce the overall cost and risk of the mission. What is clear is that there exists obvious agreement in design principles between researchers at NASA and ESA, and the architectures for both TPF-I and Darwin appear to be converging in 2007. 6
I NTRODUCTION 1.4 References Angel, R., and Woolf, N., “An imaging interferometer to study extrasolar planets,” Astrophys. J. 475, 373–379 (1997). Beichman, C. A., Fridlund, M., Traub, W. A., Stapelfeldt, K. R., Quirrenbach, A., and Seager, S., Protostars and Planets V, edited by Reipurth, B., Jewitt, D., and Keil, K., University of Arizona Press, Tucson, AZ, pp. 915 (2007). Beichman, C. A., Woolf, N. J., and Lindensmith, C. A., TPF: A NASA Origins Program to Search for Habitable Planets, JPL Publication 99-3, Jet Propulsion Laboratory, Pasadena, CA (1999). http://planetquest.jpl.nasa.gov/TPF/tpf_book/index.cfm Beichman, C. A., Coulter, D. R., Lindensmith, C. A., and Lawson, P. R., editors, Summary Report on Architecture Studies for the Terrestrial Planet Finder, JPL Publication 02-011, Jet Propulsion Laboratory, Pasadena, CA (2002). http://planetquest.jpl.nasa.gov/TPF/arc_index.cfm Fridlund, C. V. M., d'Arcio, L., den Hartog, R., Karlsson, A. 2006, “Status and recent progress of the Darwin mission in the Cosmic Vision program,” Advances in Stellar Interferometry, edited by Monnier, J. D, Schöller, M., Danchi, W. C., Proc. SPIE 6268, 62680Q (2006). Harrington, J., Hansen, B. M., Luszcz, S. H., Seager, S., Deming, D., Menou, K., Cho, J. Y.-K., and Richardson, L .J., “Phase dependent infrared brightness of the extrasolar planet υ Andromedae b,” Science 314, 623–626 (2006). Kuchner, M. J., General Astrophysics and Comparative Planetology with the Terrestrial Planet Finder Missions, JPL Publication 05-01, Jet Propulsion Laboratory, Pasadena, CA (2005). http://planetquest.jpl.nasa.gov/documents/GenAst28b.pdf Lawson, P. R., Unwin, S. C., and Beichman, C. A., editors, Precursor Science for the Terrestrial Planet Finder, JPL Publication 04-014, Jet Propulsion Laboratory, Pasadena, CA (2004) http://planetquest.jpl.nasa.gov/documents/RdMp273.pdf Traub, W. A.; Ridgway, S. T., Beichman, C. A., Johnston, K. J., Kasting, J., Shao, M. IAU Colloquium #200, edited by Aime, C. and Vakili, F.: Cambridge University Press, Cambridge, UK, 399 pp. (2006). Woolf, N. J., and Angel, J. R. P., “Astronomical searches for Earth-like planets and signs of life,” Ann. Rev. Astron. Astrophys. 36, 507–538 (1998). A Road Map for the Exploration of Neighboring Planetary Systems (ExNPS) JPL Publication 96-22, Jet Propulsion Laboratory, Pasadena, CA (1996). http://origins.jpl.nasa.gov/library/exnps/index.html 7
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: I NTRODUCTION Standard Interferomet
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 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?