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Plans for a 1.8 m Adaptive Optics Telescope and a 1.1 m Wide Field Telescope at PARI J. D. Cline, M. W. Castelaz (Pisgah Astronomical Research Institute) AAS 200th meeting, Albuquerque, NM, June 2002 Wednesday, June 5, 2002, 10:00am-7:00pm . Session 64.08
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1.8 m Adaptive Optics Telescope
1.1 m Wide Field Telescope at PARI
J. D. Cline, M. W. Castelaz(Pisgah Astronomical Research Institute)
AAS 200th meeting, Albuquerque, NM, June 2002Wednesday, June 5, 2002, 10:00am-7:00pm. Session 64.08
Two 26-m radio telescopes with 1.42, 4.8, 6.7, and 12.2 GHz receivers are shown here. The telescopes slew, set, guide, and track. They can be operated together (300 m near E-W baseline) or separately.
26 m West
26 m East
The 12.2-m antenna is available for consortium sponsorship and use at frequencies up to 60 GHz.
12.2-m prime focus feed
Aerial Image of the Optical Ridge. At an altitude of 910 m, the ridge runs East-West with steep sloping sides to the North and South. The highest point on the horizon is 5 degrees, with an average of 2 degrees. The 1.8 m and 1.1 m locations are shown (red), along with existing telescopes (blue).
Lat: 35d 11.828m N, Long: 82d 52.346m WAltitude: 934
One of the actuators is shown. The back of the mirror is coupled to the actuator through a glass block for thermal insulation.
Telescope definition is an open issue and depends on input from the astronomical community. Suggestions for use and design beyond those listed below are welcome. Please feel free to contact us (e-mail [email protected]) or leave a note here for us to contact you..
Telescope Uses and Designs under consideration:
The telescope will be field corrected prime focus camera with a 1.73 degree diameter field of view.
The Primary Mirror
We have set the condition that image quality in the focal plane will not be limited by telescope optics, rather by seeing and mechanical effects. To meet this condition, a 3-element field corrector, will be used to focus a 15 cm diameter focal plane. The table below summarizes the properties of the corrector. All lenses are made of BK7 glass. Lens 1 is nearest to the primary mirror at a distance of 391.35 cm, and Lens 3 is 7.16 cm from the focal plane.
The prime focus is formed by three lenses comprising a corrector. Shown here is the third of the lenses, along with the shutter, and two guide cameras. Light in the center 10 cm square field (1.15o) is the science field. Two guide cameras are located 180o apart in the fields formed by the 15 cm diameter field and chords along the science field. A third chord area will hold several fiber optics for a future spectrograph.
Spot diagrams based on the prime focus corrector for the 1.1 m telescope. The boxes are 24 microns, or 1 arcsec on a side. a) The spot diagram on the optical axis, b) the spot diagram 7.65 cm from the optical axis.
The open structure optical tube telescope mount we plan to use is the DFM Engineering equatorial mount, shown above. The DFM 1.27 m polar axle and support telescope mount will be customized for the 1.1-m mirror.
Weather Station: probes for temperature, humidity, pressure, wind, rain.
All-Sky Camera: Live video of the sky through a fisheye lens.
The information from the Bright Star Telescope and the other seeing/transparency instruments build a database of atmospheric conditions accessible to other telescopes of the PARI Observatories and observers using the telescopes remotely.
Pisgah Astronomical Research Institute
1 PARI Drive
Rosman, NC 28772
Office: 828-862-5554FAX: 828-862-5877Internet: www.pari.edu