TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 3 3.3 Conclusions Darwin/TPF-I will open a gateway to future space-based interferometry to deliver ever increasing angular resolution throughout the electromagnetic spectrum. The baseline design will provide order-of-magnitude improvements in angular resolution over any other instrument. Combined with sensitivity to objects as faint as magnitude 20, Darwin/TPF-I capabilities have the potential for revolutionary advances in all areas of astrophysics and planetary science. This mission will transform our understanding of galaxy formation and evolution, stellar and planetary system origins, the cycles of matter and energy in the cosmos; and it will enable the detailed mapping of surfaces and weather patterns in Solar System objects. The utility of this instrument for general astrophysics and planetary science will only be limited by the lack of available observing time. Acknowledgements: We thank Marc Kuchner for providing selected material from the NASA / JPL Publication 05-01, General Astrophysics and Comparative Planetology with the Terrestrial Planet Finder Missions. 3.4 References Adams, F. C., Proszkow, E. M., Fatuzzo, M., and Myers, P. C., “Early evolution of stellar groups and clusters: Environmental effects on forming planetary systems,” Astrophys. J. 641, 504–525 (2006). Barger, A. J., Cowie, L. L., Sanders, D. B., et al., “Submillimetre-wavelength detection of dusty starforming galaxies at high redshift,” Nature 394, 248–251 (1998). Boden, A. F., Shao, M., and van Buren, D., “Astrometric observations of MACHO gravitational microlensing,” Astrophys. J. 502, 538–549 (1998). Dalal, N., and Lane, B. F., “Bringing closure to microlensing mass measurements,” Astrophys. J. 589, 199–209 (2003). De Breuck, C., van Breugel, W., Röttgering, H., et al., “Spectroscopy of ultra-steep-spectrum radio sources,” Astron. J. 121, 1241–1265 (2001). Dray, L. M., Tout, C. A., Karakas, A. I., and Lattanzio, J. C., “Chemical enrichment by Wolf-Rayet and asymptotic giant branch stars,” Mon. Not. R. Astron. Soc. 338, 973–989 (2003). Dwek, E., “The evolution and elemental abundances in the gas and dust phases of the Galaxy,” Astrophys. J. 501, 643–665 (1998). Edmunds, M. G., “An elementary model for the dust cycle in galaxies,” Mon. Not. R. Astron. Soc. 328, 223–236 (2001). Franx, M., Labbé, I., Rudnick, G., et al., “A significant population of red, near-infrared high-redshift galaxies,” Astrophys. J. 587, L79–L82 (2003). 54
G ENERAL A STROPHYSICS Gavilán, M., Buell, J. F., and Mollá, M., “Low and intermediate mass star yields: The evolution of carbon abundances,” Astron. Astrophys. 432, 861–877 (2005). Ghez, A. M., Salim, S., Hornstein, S. D., et al., “Stellar orbits around the Galactic central black hole,” Astrophys. J. 620, 744–757 (2005). Granato, G., Danese, L., and Franceschini, A., “Thick tori around active galactic nuclei: The case for extended tori and consequences for their x-ray and infrared emission,” Astrophys. J. 486, 147– 159 (1997). Hollenbach, D. J., Yorke, H. W., and Johnstone, D., “Disk dispersal around young stars,” in Protostars and Planets IV, editors, Mannings, V., Boss, A. P., and Russell, S. S., University of Arizona Press: Tucson, AZ, 401 (2000). Hughes, D. H., Serjeant, S., Dunlop, J., et al., “High-redshift star formation in the Hubble Deep Field revealed by a submillimeter-wavelength survey,” Nature 394, 241–247 (1998). Johnstone, D., Hollenbach, D., and Bally, J., “Photoevaporation of disks and clumps by nearby massive stars: Application to disk destruction in the Orion nebula,” Astrophys. J. 499, 758–776 (1998). Kroupa, P., “The initial mass function of stars: Evidence for uniformity in variable systems,” Science 295, 82–91 (2002). Labbé, I., Franx, M., Rudnick, G., et al., “Ultradeep near-infrared ISAAC observations of the Hubble Deep Field South: Observations, reduction, multicolor catalog, and photometric redshifts,” Astron. J. 125, 1107–1123 (2003). Labbé, I., Huang, J., Franx, M., et al., “IRAC mid-infrared imaging of the Hubble Deep Field-South: Star formation histories and stellar masses of red galaxies at z>2,” Astrophys. J. 624, L81–L84 (2005). Lada, C. J., and Lada, E. A., “Embedded clusters in molecular clouds,” Ann. Rev. Astron. Astrop. 41, 57– 115 (2003). Maeder, A., “Stellar yields as a function of initial metallicity and mass limit for black hole formation,” Astron. Astrophys. 264, 105–120 (1992). MacLow, M.-M., and Klessen, R. S., “Control of star formation by supersonic turbulence,” Reviews of Modern Physics 76, 125–194 (2004). Moorwood, A. F., “ISAAC: a 1–5 μm imager/spectrometer for the VLT,” Optical Telescopes of Today and Tomorrow, Proc. SPIE 2871, Ardeberg; A. L. editor, 1146–1151 (1997). Mullally, F., Kilic, M., Reach, W. T., et. al., “A Spitzer white dwarf infrared survey,” Astrophys. J. Supp. Ser. astro-ph/0611588 (2006). 55
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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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Page 19 and 20: I NTRODUCTION Standard Interferomet
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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 48 and 49: C HAPTER 2 Beichman, C. A., Fridlun
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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 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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Page 114 and 115: C HAPTER 5 Heavy launch vehicle. Th
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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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