We introduce a model for supporting collaborative work between people that are physically close to each other. We call this model Single Display Groupware (SDG). In this paper, we describe this model, comparing it to more traditional remote collaboration. We describe the requirements that SDG places on computer technology, and our understanding of the benefits and costs of SDG systems. Finally, we describe a prototype SDG system that we built and the results of a usability test we ran with 60 elementary school children.
A method is introduced for predicting control voltages that will generate a prescribed surface shape on a MEMS deformable mirror. The algorithm is based upon an analytical elastic model of the mirror membrane and an empirical electromechanical model of its actuators. It is computationally simple and inherently fast. Shapes at the limit of achievable mirror spatial frequencies with up to 1.5 microm amplitudes have been achieved with less than 15 nm rms error.
We report on the development of a new MEMS deformable mirror (DM) system for the hyper-contrast visible nulling coronagraph architecture designed by the Jet Propulsion Laboratory for NASA's Terrestrial Planet Finding (TPF) mission. The new DM is based largely upon existing lightweight, low power MEMS DM technology at Boston University (BU), tailored to the rigorous optical and mechanical requirements of the nulling coronagraph. It consists of 329-hexagonal segments on a 600Ι m pitch, each with tip/tilt and piston degrees of freedom. The mirror segments have 1Ι m of stroke, a tip/tilt range of 600 arc-seconds, and maintain their figure to within 2nm RMS under actuation. The polished polycrystalline silicon mirror segments have a surface roughness of 5nm RMS and an average curvature of 270mm. Designing a mirror segment that maintains its figure during actuation was a very significant challenge faced during DM development. Two design concepts were pursued in parallel to address this challenge. The first design uses a thick, epitaxial grown polysilicon mirror layer to add rigidity to the mirror segment. The second design reduces mirror surface bending by decoupling actuator diaphragm motion from the mirror surface motion. This is done using flexure cuts around the mirror post in the actuator diaphragm. Both DM architectures and their polysilicon microfabrication process are presented. Recent optical and electromechanical characterization results will also be discussed, in addition to plans for further improvement of DM figure to satisfy nulling coronagraph optical requirements.
Abstract. We report on the development of microelectromechanical (MEMS) deformable mirrors designed for ground and space-based astronomical instruments using adaptive optics. These light-weight, low power deformable mirrors will have an active aperture of up to 25.2mm consisting of thin silicon membrane mirror supported by an array of up to 4096 electrostatic actuators exhibiting no hysteresis and sub-nanometer repeatability. The continuous membrane deformable mirrors, coated with a highly reflective metal film, are capable of up to 4µm of stroke, have a surface finish of <10nm RMS with a fill factor of 99.8%. The segmented device has a range of motion of 1um of piston and 600 arc-seconds of tip/tilt simultaneously and a surface finish of 5nm RMS. Presented in this paper are device characteristics and performance results for these devices. Motivation for high-resolution wavefront correctionMost large ground based telescopes now employ AO as an essential and enabling tool for highresolution imaging. Though recent progress in AO for current and future large telescopes has been technologically exciting, its impact on astronomical science remains modest to date. AO technology is still inadequate to compensate for the larger wavefront errors and shorter atmospheric coherence lengths associated with visible wavelength observation. Its simplest implementation allows only a narrow field of compensation, and more ambitious instrument concepts are limited by the cost, size, and complexity of AO components, especially the DM. A critical assessment of AO technology was funded by the National Science Foundation several years ago, resulting in a 2008 report entitled A Roadmap for the Development of United States Astronomical Adaptive Optics. The roadmap identifies single major goal for wavefront correction: "Development of scalable, cost-effective DM technologies" and recommends a high-priority research investment to achieve this goal: "High stroke, high actuator count [deformable] mirrors to enable correction at high spatial frequencies over narrower fields of view."The coming generation of ELTs, will be the first to be designed with AO at the outset. Since the benefits of AO increase nonlinearly with telescope aperture, a phenomenon sometimes called D 4 scaling, AO will be essential for many ELT science goals [1,2]. Promising AO instruments that will require new DMs include multi-conjugate adaptive optics (MCAO), multi-object adaptive optics (MOAO), and extreme adaptive optics (ExAO) [3]. MCAO employs two or more guide stars to enable tomographic wavefront error sensing, and then two or more deformable mirrors in series to correct those errors. The result is a wider corrected field of view [4]. This technique was recently used to produce the sharpest whole-planet (Jupiter) picture ever taken from the ground [5]. MOAO is an instrument concept that also uses multiple guide stars and multiple deformable mirrors [6]. However in MOAO, many DMs would be used in parallel to apply independent corrections for the turbulence-induce...
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