Gemini telescopes instrumentation program

Douglas A. Simons; David J. Robertson; C. Matt Mountain

doi:10.1117/12.211268

6 June 1995 Gemini telescopes instrumentation program

Douglas A. Simons, David J. Robertson, C. Matt Mountain

Proceedings Volume 2475, Infrared Detectors and Instrumentation for Astronomy; (1995) https://doi.org/10.1117/12.211268
Event: SPIE's 1995 Symposium on OE/Aerospace Sensing and Dual Use Photonics, 1995, Orlando, FL, United States

Abstract

The Gemini Telescopes are being built to exploit the unique infrared sites of Mauna Kea in Hawaii and Cerro Pachon in Chile. Both telescopes are being designed to deliver 0.1 arcsec images at the focal plane at 2.2 micrometers which will include all tracking and enclosure affects. Beyond 2 micrometers , using fast tip/tilt secondaries these 8 m telescopes will be essentially diffraction limited. In addition the use of protected silver coatings for both the primary and secondary mirrors and efficient in-situ mirror cleaning means the Mauna Kea telescope should be capable of delivering focal plane emissivities of approximately 2%. The baseline design for the Mauna Kea telescope also includes an adaptive optics system capable of feeding a 1 - 2 arcminute corrected field to near infrared instruments mounted at the f/16 Cassegrain focus. Fully exploiting the superb characteristics of the Gemini Telescopes will require a new generation of instruments which will challenge both instrument designers and infrared array technologies. The baseline complement of infrared instruments includes a 1 - 5 micrometers imager, a 1 - 5 micrometers spectrometer, and a mid-infrared (8 - 25 micrometers ) imager. Several optical instruments will also be built under the baseline instrumentation plan.

Citation Download Citation

Douglas A. Simons, David J. Robertson, and C. Matt Mountain "Gemini telescopes instrumentation program", Proc. SPIE 2475, Infrared Detectors and Instrumentation for Astronomy, (6 June 1995); https://doi.org/10.1117/12.211268

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