KEYWORDS: Mirrors, Manufacturing, Surface roughness, Telescopes, Etching, Surface finishing, Short wave infrared radiation, Received signal strength, Temperature metrology, Optical simulations
The Fred Young Submillimeter Telescope (FYST) is a 6-meter diameter telescope with a surface accuracy of 10.7 microns, operating at submillimeter to millimeter wavelengths (100 GHz – 1.5 THz). It will be located at 5600 meters elevation on Cerro Chajnantor in the Atacama desert of northern Chile overlooking the ALMA site. Its novel optical “crossed-Dragone” design will deliver a high-throughput, wide field-of-view telescope capable of mapping the sky very rapidly and efficiently. This paper discusses the mirror panel production and its contribution to the overall half wave front error of the telescope. The first half details the panel manufacturing precision. The effect of panel production quality on the beam shape and beam quality is presented. The second half of the paper looks at the local surface roughness of a mirror panel. Surface roughness data for a machined panel with an etched surface are presented. Some non-ideal surface features for an etched panel are discussed.
The Fred Young Submillimeter Telescope (FYST) is a 6-meter diameter telescope with a surface accuracy of 10 microns, operating at submillimeter to millimeter wavelengths. It will be located at 5600 meters elevation on Cerro Chajnantor in the Atacama desert of northern Chile overlooking the ALMA site. Its novel optical “crossed-Dragone” design will deliver a high-throughput, wide field-of-view telescope capable of mapping the sky very rapidly and efficiently. The telescope can host up to three instruments, with the heterodyne array “CHAI” and the direct-detection camera “Prime-Cam” as first-generation instruments. The often harsh environmental conditions at the telescope site require that FYST be operated remotely, either from the base station near San Pedro de Atacama or from the scientist’s home institutions in the US, Canada and Germany. Automated observations will therefore be the dominant observation mode. FYST’s Observatory Control System (OCS) gives instrument teams the responsibility to control observations. We believe that this model is a good fit for FYST because the observatory will operate exclusively in campaign mode. Furthermore, instrument teams have significant investments in software they want to preserve. The OCS adopts a micro-service design using off-theshelf components as far as possible to minimize development effort. We will present the OCS design and the selection of off-the-shelf components used.
The Fred Young Submillimeter Telescope (FYST) is a 6-meter diameter telescope currently being built by the CCAT-prime project that will observe at millimeter and submillimeter wavelengths. It will deliver a total wavefront error of less than 22 microns at the focal plane. The optics follow a modified crossed-Dragone configuration, yielding a 7.8° field of view across a ~2 meter diameter focal plane. The telescope will be located at 5600 meters on Cerro Chajnantor in the Atacama Desert. The demands of first-generation and future instruments significantly drove the design of the telescope. The telescope layout consists of multiple instrument bays, which provide the capacity to house a total of 11 tons of focal plane instrumentation across 23 square meters of floor space. The Yoke Traverse is divided into telescope servo, instrument electronics, and process spaces, and can support an additional 8 tons of instrument equipment. We discuss the final design and fabrication status of FYST.
This paper discusses the usage of LoRa wireless transmission protocol in support of CCAT-prime telescope operations in northern Chile. A LoRa based sensor network allows for low data rate sensors to be deployed with up to 1 year battery life with a broadcast range of multiple kilometers. In this paper we present the basics of a LoRa network and demonstrate its application to a vehicle tracking system as part of an observatory sensor network. We show results from a recent test campaign and demonstrate transmission ranges up to 40km. We discuss plans for future expansion and how such a system aids the remote operation of an observatory.
CCAT will be a 25m diameter sub-millimeter telescope capable of operating in the 0.2 to 2.1mm wavelength range. It will be located at an altitude of 5600m on Cerro Chajnantor in northern Chile near the ALMA site. The anticipated first generation instruments include large format (60,000) kinetic inductance detector (KID) cameras, a large format heterodyne array and a direct detection multi-object spectrometer. The paper describes the architecture of the CCAT software and the development strategy.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.