Maunakea Spectroscopic Explorer (MSE) is the first of the future generation of massively multiplexed spectroscopic 11.25m mirror facility on a recycled site. MSE is designed to enable transformative science, being completely dedicated to large-scale multi-object spectroscopic surveys, each studying thousands to millions of astrophysical objects. MSE’s transformational potential lies in answering numerous scientific questions and finding new puzzles. Its success will depend in part on its ability to detect large populations of faint sources, from those responsible for reionization to merging galaxies at cosmic dawn and the stellar populations of nearby dwarf galaxies. This capability is set, in part, by our ability to remove the sky from the target spectra. Here we describe the initial steps in a threeyear long effort to develop a model of the Maunakea skies comparable to the model developed by ESO of the southern ESO sites. The model will be used to derive best-practices (e.g. the number of required fibers given specific observing conditions, and required sensitivity) and sky subtraction algorithms to achieve << 1% sky subtraction accuracy
We describe the camera articulation prototype (CAP) for the Giant Magellan Telescope Multi-object Astronomical and Cosmological Spectrograph (GMACS), which is a wide field, multi-object, moderate-resolution, optical spectrograph of the Giant Magellan Telescope (GMT). The GMACS will have the Camera and Grating Articulation System (CGAS) which has two independent cameras and grating modules. The grating angles and the camera angles can be changed to adjust the dispersed light bands on the detector. The electronics components of this system include motors with encoder, pneumatic brakes, and limit switches. We demonstrate how to control the camera angles using a prototype that is designed for the camera articulation controller as a miniature model of the GMACS. The prototype was built with commercially-available extruded aluminum struts and 3D-printed parts and includes two motors with encoders. The prototype was produced quickly and inexpensively, but replicates all functions of the camera articulation mechanism in GMACS. We have developed the control package for the prototype that will be one of the GMACS Device Control System (DCS). The software is designed by the Agile development process and SysML, and developed using Visual C++ on Windows OS. This software has five major control functions: power, homing, resolution mode changing, limit detection, and emergency process. The limit detection is implemented by setting up the limit angle range in the software, because the limit switches are not included in the prototype. We present the demonstration result and discuss the details of the communication route about data flow between high-end user software and hardware components.
We describe and present initial testing of TCal, a mobile spectrophotometric calibration system that will be used to characterize the throughput as a function of wavelength for imaging systems at observatories around the world. TCal measurements will enhance the science return from follow-up observations of imaging surveys such as LSST (Large Synoptic Survey Telescope) and DES (Dark Energy Survey) by placing all tested imaging systems on a common photometric baseline. TCal uses a ~ 1 nm bandpass tunable light source to measure the instrumental response function of imaging systems from 300 nm to 1100 nm, including the telescope, optics, filters, windows, and detector. The system is comprised of a monochromator-based light source illuminating a dome flat field screen monitored by a calibrated CCD, which allows determination of the telescope throughput as a function of wavelength. This calibration will be performed at 1-8m telescopes that expect to devote time towards survey follow-up. Performing the calibration on these telescopes will reduce systematic errors due to small differences in bandpass, making follow-up efforts more precise and accurate.
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