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Table of contents
1 Active optics for large-scale instrumental projects
1.1 Image quality in telescopes
1.1.1 Image quality: definition
1.1.2 Optical aberrations theory
1.1.3 Telescope quality: ground versus space
1.2 Instrumental needs for modern astrophysics
1.2.1 Searching for exoplanets and for life
1.2.2 Cosmology
1.2.3 Galaxy physics and star formation
1.2.4 Earth observation
1.2.5 Conclusion: instrumental needs
1.3 Active optics: an overview
1.3.1 Active optics: a link between optical aberrations and elasticity theories
1.3.2 Active optics design with Finite Element Analysis
1.3.3 Access to optimal performance thanks to active optics
1.4 Active Optics for large telescopes
1.4.1 The Very Large Telescope: the most advanced Visible/Infra-Red telescope
1.4.2 Toward large segmented active telescopes: ELT and JWST
1.5 Conclusion
2 Correcting active mirror for space telescope : MADRAS project
2.1 Large space observatories context
2.1.1 Space telescope evolution and needs
2.1.2 MADRAS project
2.2 MADRAS mirror design
2.2.1 Multimode Deformable Mirror: principle
2.2.2 Final design
2.3 FEA performance
2.3.1 Influence Functions and Eigen Modes
2.3.2 Mode correction
2.3.3 Global WFE correction
2.3.4 Conclusion on the Finite Element Analysis
2.4 Hardware specification and integration
2.4.1 Actuators
2.4.2 Estimating geometric sensitivities with FEA
2.4.3 Complete mirror system
2.4.4 System integration
2.5 Complete mirror system validation with interferometry
2.5.1 Test set-up
2.5.2 Influence Function
2.5.3 Performance of the complete mirror system
2.6 Conclusion
3 MADRAS mirror performance in closed loop
3.1 Test bed overview
3.1.1 Objectives
3.1.2 Design
3.1.3 Data analysis
3.2 Test bed characterization
3.2.1 WFE generation
3.2.2 Aberrations of the bench
3.3 Active correcting loop calibration
3.3.1 Interaction Matrix and Control Matrix
3.3.2 Loop Noise
3.3.3 Flattening
3.4 Mode correction
3.4.1 Operation
3.4.2 Specified modes
3.4.3 Stability in open loop
3.5 Representative WFE correction
3.5.1 Linearity
3.5.2 Mode combination
3.5.3 Global performance
3.6 Conclusion
4 Giant telescopes: segments manufacturing with stress polishing
4.1 The E-ELT and its large segmented primary mirror
4.1.1 A 5 mirror telescope
4.1.2 A 39 m diameter primary mirror
4.1.3 Segment prototype with stress mirror polishing
4.2 Warping harness design
4.2.1 System description and modeling
4.2.2 Design optimization and FEA performance
4.2.3 Error sources characterization
4.2.4 Overall system performance and specifications
4.3 Experimental testing
4.3.1 Prototype
4.3.2 Testing means
4.4 Conclusion
5 Optimized active systems: 1 actuator – 1 mode
5.1 Adapting the influence functions to the correction requirements
5.1.1 System simplification: context
5.1.2 System simplification: design
5.1.3 System simplification: optimization method
5.2 “Variable Off-Axis paraboLA” system (VOALA)
5.2.1 Application domain
5.2.2 Focus and Coma generation
5.2.3 Astigmatism generation
5.2.4 Modes combination and alternative design
5.3 “Correcting Optimized Mirror with a Single Actuator” system (COMSA)
5.3.1 Application domain
5.3.2 Contour adaptation
5.3.3 Thickness distribution
5.3.4 Actuation point location
5.4 Examples of application
5.4.1 Field compensation in an interferometer
5.4.2 Off-Axis Parabola generation
5.4.3 Zoom system
5.5 Conclusion
