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The fifth Sloan Digital Sky Survey Local Volume Mapper (LVM) is a wide-field integral field unit survey that uses an array of four 160 mm fixed telescopes with siderostats to minimize the number of moving parts. An individual telescope observes the science or calibration field independently and is synchronized with the science exposure. We developed the LVM Acquisition and Guiding Package (LVMAGP)optimized telescope control software program for LVM observations, which can simultaneously control four focusers, three K-mirrors, one fiber selector, four mounts (siderostats), and seven guide cameras. This software is built on a hierarchical architecture and the SDSS framework and provides three key sequences: autofocus, field acquisition, and autoguide. We designed and fabricated a proto-model siderostat to test the telescope pointing model and LVMAGP software. The mirrors of the proto-model were designed as an isogrid open-back type, which reduced the weight by 46% and enabled reaching thermal equilibrium quickly. In addition, deflection due to bolting torque, self-gravity, and thermal deformation was simulated, and the maximum scatter of the pointing model induced by the tilt of optomechanics was predicted to be 4′.4, which can be compensated for by the field acquisition sequence. We performed a real sky test of LVMAGP with the proto-model siderostat and obtained field acquisition and autoguide accuracies of 0″.38 and 1″.5, respectively. It met all requirements except for the autoguide specification, which will be resolved by more precise alignment among the hardware components at Las Campanas Observatory.
The fifth Sloan Digital Sky Survey Local Volume Mapper (LVM) is a wide-field integral field unit survey that uses an array of four 160 mm fixed telescopes with siderostats to minimize the number of moving parts. An individual telescope observes the science or calibration field independently and is synchronized with the science exposure. We developed the LVM Acquisition and Guiding Package (LVMAGP)optimized telescope control software program for LVM observations, which can simultaneously control four focusers, three K-mirrors, one fiber selector, four mounts (siderostats), and seven guide cameras. This software is built on a hierarchical architecture and the SDSS framework and provides three key sequences: autofocus, field acquisition, and autoguide. We designed and fabricated a proto-model siderostat to test the telescope pointing model and LVMAGP software. The mirrors of the proto-model were designed as an isogrid open-back type, which reduced the weight by 46% and enabled reaching thermal equilibrium quickly. In addition, deflection due to bolting torque, self-gravity, and thermal deformation was simulated, and the maximum scatter of the pointing model induced by the tilt of optomechanics was predicted to be 4′.4, which can be compensated for by the field acquisition sequence. We performed a real sky test of LVMAGP with the proto-model siderostat and obtained field acquisition and autoguide accuracies of 0″.38 and 1″.5, respectively. It met all requirements except for the autoguide specification, which will be resolved by more precise alignment among the hardware components at Las Campanas Observatory.
The Magdalena Ridge Observatory Interferometer is a 10-element 1.4 meter aperture optical and near-infrared interferometer being built at 3,200 meters altitude on Magdalena Ridge, west of Socorro, NM. The interferometer layout is an equilateral "Y" configuration to complement our key science mission, which is centered around imaging faint and complex astrophysical targets. This paper serves as an overview and update on the status of the observatory and our progress towards first light and first fringes in the next few years. MAGDALENA RIDGE OBSERVATORYThe Magdalena Ridge Observatory is a Federally Funded facility being built and managed by New Mexico Institute of Mining and Technology (NMT) which also serves as host for the observatory offices on the NMT campus in Socorro, NM. The observatory consists of two major facilities: a fast-tracking 2.4 m telescope and an optical interferometer. The 2.4 m telescope obtained first light on Oct. 31, 2006 and is currently moving into full operations. It is a superb instrument for the study of fast-moving objects and targets of opportunity, owing to its very high slew and tracking rates; its operations are currently funded 30% by NASA for NearEarth Object follow-on studies 1 . The optical interferometer is being designed and built in collaboration with our partners at the University of Cambridge, Cavendish Lab. In this last development phase the interferometer is moving towards a first fringes date in late 2010. Phase A of the interferometer build will include 6 telescopes and infrared fringe-tracking and scientific imaging capabilities. Phase B will add 4 more telescopes and associated beam trains, visible operations, and will have an additional location in the beam combining laboratory for guest instruments. (See Figure 1 for views of the two facilities.) The greater observatory facilities include over 8 miles of maintained road, on-site water, power, ethernet, housing facilities and a location on the Ridge for a third scientific facility yet to be determined.
It is vitally important to improve effects of error compensation for horizontal photoelectric theodolite and reduce production costs by executing rational control of verticality error of shafting. This paper analyzes the mechanism how the verticality error of shafting influences measurement precision of photoelectric theodolite considering the architectural characteristics of the frame of horizontal theodolite. Matlab software has been used to simulate pointing accuracy. Verticality error of shafting of horizontal theodolite has been detected. Measured verticality error of shafting is 37 and detection error is 10. Results of analysis and detection to be applied for error compensation can improve pointing accuracy of the theodolite.
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