Chapter 6 6 Instrument <strong>Technology</strong> and Advanced Concepts 6.1 Instrument <strong>Technology</strong> An announcement of opportunity for Instrument Concept Studies was released early in 2005 for the purpose of soliciting the best ideas from academia and industry. The instruments defined in these studies along with the technical requirements that their accommodation would place on the observatory system will be considered by the Science and <strong>Technology</strong> Definition Team for inclusion in their final report. These studies are expected to expose technology needs for classes of instruments, and those identified for the most promising candidates will be addressed when the <strong>TPF</strong>-C <strong>Technology</strong> Development <strong>Plan</strong> is updated next. This section serves as a placeholder for those activities. 6.1.1 Detectors The PIs of the selected Instrument Concept Studies will be asked to determine detector requirements and assess the needs against the state-of-the-art for fabrication and characterization. If a technology need is identified, a development plan will be added in the next version of this document. 6.2 Advanced Concepts Currently there are two advanced concepts under development. The visible nulling architecture and the phase-induced amplitude apodization represent alternatives to the baseline coronagraphic approach to achieving the necessary starlight suppression. These efforts are carried as options to reduce risk to the Project through a development ending with proof-of-concept demonstrations. 6.2.1 Visible Nulling “Coronagraph” Testbed Objective The object of this technology development is to demonstrate the principle of nulling interferometry as applied to exo-planet imaging at visible wavelengths. The visible nulling testbed integrates all component and subsystem technologies developed for starlight suppression 94
Instrument <strong>Technology</strong> and Advanced Concepts and is intended ultimately to demonstrate 10 -10 light suppression to 3λ/D or better. The testbed demonstrates proof-of-concept control of the amplitude, phase, spectral band pass, and polarization of the light to achieve target performance levels. Approach The visible nulling testbed achieves high contrast imaging via interferometry. 35,36,37 Using the telescope pupil, we synthesize a “nulling interferometer-based coronagraph” by dividing the light into two or more copies, applying π phase changes to selected copies, and recombining them with a lateral shear proportional to the required baseline. The pupil overlap region is then projected into the far-field, i.e., sent to an image plane, so that the resulting image is the superposition of the star and planet system with an interference fringe pattern. The star is in the dark portion of the fringe and is deeply attenuated, whereas the planet falls within the light or unattenuated location of the fringe. Previous nulling experiments used a rotational shearing interferometer and a single mode optical fiber. 38,39 For <strong>TPF</strong> applications, rotational shearing is not acceptable because of the multiple baselines induced. Consequently, a linear shear is introduced via a modified Mach-Zehnder interferometer. 40 A coherent array of single mode fibers filters starlight over a wide field of view. 41 Its principal function is loosely analogous to the filtering of scattered starlight in the Lyot plane of a ‘conventional’ coronagraph. Starlight that leaks past the diffraction suppression of the nulling interferometer is spatially filtered by each optical fiber in the array while the planet light is allowed to propagate without attenuation. The residual leaked starlight is also incoherent with planet light, thus the filtered planet light will focus into an image (a single pixel in the field) while the leaked starlight will be evenly distributed over the field of view. Thus to achieve the 10 -10 contrast between star and planet, it is sufficient for the nuller to operate at 10 -7 with the residual light spread over 1000 sub-apertures in the single mode fiber array (SMFA). 42 This fiber array may also be a valuable component in a conventional coronagraphic imaging system. 35 Angel, R. (1990), “Use of a 16-m Telescope to Detect Earthlike <strong>Plan</strong>ets,” Proceedings of the Workshop on The Next Generation Space Telescope, P. Bely and C. Burrows, eds., Space Telescope Science Institute, pp. 81–94. 36 Angel, J.R.P, and Woolf, N.J. (1997),”An Imaging Nulling Interferometer to Study Extrasolar <strong>Plan</strong>ets,”Astrophysical Journal, v475, pp. 373-379. 37 Shao, M., (1991), “Hubble Extra Solar <strong>Plan</strong>et Interferometer,” SPIE v1494. 38 Serabyn, E., Wallace, J.K., Hardy, G.J., Schwindthin, E.G.H., and Nguyen (1999), “Deep Nulling of Visible LASER Light,” Appl. Opt., v38, p7128. 39 Wallace, K., Hardy, G, and Serabyn, E. (2000), “Deep and stable interferometric nulling of broadband light with implications for observing planets around nearby stars,” Nature, v406. 40 Serabyn, E. and Colavita, M.M. (2001), “Fully Symmetric Nulling Beam Combiners,” Applied Optics, v40, pp. 1668–1671. 41 Shao, M., Serabyn, E., Levine, B.M., Mennesson, B.P., and Velusamy, T. (2002), “Visible nulling coronagraph for detecting planets around nearby stars,” SPIE v4860. 42 Levine, B.M., Shao, M., Liu, D.T., Wallace, J.K., and Lane, B.F. (2003), “<strong>Plan</strong>et Detection in Visible Light with a Single Aperture Telescope and Nulling Coronagraph,” SPIE v5170. 95
- Page 1 and 2:
JPL Publication 05-8 Technology Pla
- Page 3:
TECHNOLOGY PLAN TERRESTRIAL PLANET
- Page 6 and 7:
Recent Highlights Technical progres
- Page 8 and 9:
Figure i-4. Deformable mirror deliv
- Page 10 and 11:
Table of Contents Approvals........
- Page 12 and 13:
7.5.2 Precision Hexapod............
- Page 14 and 15:
Chapter 1 Figure 1-1. Artist's impr
- Page 16 and 17:
Chapter 1 interferometry, continues
- Page 18 and 19:
Chapter 1 Back end coronagraph opti
- Page 20 and 21:
Chapter 1 Surrounding the whole tel
- Page 22 and 23:
Chapter 1 Pol. BS fold/steering Mic
- Page 24 and 25:
Chapter 1 1.6.5 Sunshield The teles
- Page 26 and 27:
Chapter 1 expected architecture dow
- Page 28 and 29:
Chapter 1 Table 1-3. TPF-C Technolo
- Page 30 and 31:
Chapter 1 3B: Demonstrate, using th
- Page 32 and 33:
Chapter 2 2 Error Budgets 2.1 Contr
- Page 34 and 35:
Chapter 2 Error Budget Validation G
- Page 36 and 37:
Chapter 2 Further, it is shown that
- Page 38 and 39:
Chapter 2 Table 2-1. Requirement on
- Page 40 and 41:
Chapter 3 3 Optics and Starlight Su
- Page 42 and 43:
Chapter 3 are in progress with cont
- Page 44 and 45:
Chapter 3 Figure 3-5. Coronagraph s
- Page 46 and 47:
Chapter 3 (though not light-weight
- Page 48 and 49:
Chapter 3 Table 3-3. ITT Metrology
- Page 50 and 51:
Chapter 3 observations. The time it
- Page 52 and 53:
Chapter 3 vacuum-compatible, low-po
- Page 54 and 55:
Chapter 3 blank size. Westerhoff et
- Page 56 and 57: Chapter 3 configurations, performan
- Page 58 and 59: Chapter 3 Figure 3-10: Plots showin
- Page 60 and 61: Chapter 3 The wavefront quality of
- Page 62 and 63: Chapter 3 Figure 3-13. Optical layo
- Page 64 and 65: Chapter 3 algorithms have limitatio
- Page 66 and 67: Chapter 3 simulated star source is
- Page 68 and 69: Chapter 4 Figure 4-1. Overview of t
- Page 70 and 71: Chapter 4 enclosures, and stable la
- Page 72 and 73: Chapter 4 facilities from which dat
- Page 74 and 75: Chapter 4 Figure 4-5. Microslip Tri
- Page 76 and 77: Chapter 4 Figure 4-7. Calibration o
- Page 78 and 79: Chapter 4 Figure 4-8. Comparison of
- Page 80 and 81: Chapter 4 4.2 Subsystem and System
- Page 82 and 83: Chapter 4 Figure 4-11. Schematic of
- Page 84 and 85: Chapter 4 Figure 4-12. Fine guiding
- Page 86 and 87: Chapter 4 (5) The Fine Steering Mir
- Page 88 and 89: Chapter 4 Third, precise thermal co
- Page 90 and 91: Chapter 4 giving confidence that fl
- Page 92 and 93: Chapter 4 surface polish is nonethe
- Page 94 and 95: Chapter 5 TPF-C is planning a suite
- Page 96 and 97: Chapter 5 engineering judgment (i.e
- Page 98 and 99: Chapter 5 categories, in reality ea
- Page 100 and 101: Chapter 5 Table 5-3. Validation of
- Page 102 and 103: Chapter 5 5.6.1 Modeling Methodolog
- Page 104 and 105: Chapter 5 strength of computer simu
- Page 108 and 109: Chapter 6 Figure 6-1. Detailed conc
- Page 110 and 111: Chapter 6 The first method is self-
- Page 112 and 113: Chapter 6 super computers and is us
- Page 114 and 115: Chapter 7 7 Plan for Technology Dev
- Page 116 and 117: Chapter 7 Figure 7-1. TPF-C Technol
- Page 118 and 119: Chapter 7 Improvements to the DM ov
- Page 120 and 121: Chapter 7 7.3 Error Budgets 7.3.1 D
- Page 122 and 123: Chapter 7 7.4 Optics and Starlight
- Page 124 and 125: Chapter 7 7.4.2 Apodizing Masks and
- Page 126 and 127: Chapter 7 7.4.4 Wavefront Sensing a
- Page 128 and 129: Chapter 7 7.4.6 Transmissive Optics
- Page 130 and 131: Chapter 7 7.4.8 Scatterometer Scope
- Page 132 and 133: Chapter 7 7.5 Structural, Thermal,
- Page 134 and 135: Chapter 7 7.5.3 Precision Structura
- Page 136 and 137: Chapter 7 model of TPF-C and should
- Page 138 and 139: Chapter 7 7.5.6 Secondary Mirror To
- Page 140 and 141: Chapter 7 7.5.8 Sub-scale EM Sunshi
- Page 142 and 143: Chapter 7 7.6 Integrated Modeling a
- Page 144 and 145: Chapter 7 7.7.3 Advanced Concepts:
- Page 146 and 147: Chapter 8 134
- Page 148 and 149: Appendices Appendix B: TPF-C Detail
- Page 150 and 151: Appendices Appendix D: TPF-C Techno
- Page 152 and 153: Appendices Appendix F: Acronym List
- Page 154: Appendices RWA SAO SBIR SIM SM SMFA