The Radcliffe consists of two telescopes on a single German equatorial mount, designed and built in the days when Imperial units were standard. The larger, 24-inch (60-cm) telescope was originally used to take images on 12x12-inch glass photographic plates, for astrometry including parallax measurements. For practical reasons (including economy!) 6x6-inch plates were later used for student training, but large-format CCD detectors have been employed almost exclusively for imaging since 1994. The co-aligned 18-inch (45-cm) telescope was originally intended for 'hand-and-eye' guiding, to correct tracking errors during long photographic exposures. This is no longer important because of improved telescope control, and because of the generally shorter integrations associated with highly efficient digital detectors, but the 18-inch continues to be used for visual and video-camera observing.
The matched focal lengths of the telescopes
are each nearly seven metres, and the dome which houses the Radcliffe is over
10 metres in diameter. The total weight of the tube of the telescope and
the arm required to counterbalance its weight is about five tonnes, and
the framework a further six.
|Optics:||Twin Grubb Refractor|
|Aperture:||18" (45cm), 24" (60cm) [f/15, f/11.5]|
|Focal Length:||276" (7.0m)|
|Plate Scale:||29.5 arcsec/mm|
Apogee Alta U9000 camera
(Kodak KAF-09000 3056x3056 CCD, 12x12-micron pixels)
'comet' filters, H2O+ (620.5nm) + continuum (625.0nm)
|Detector 18":||visual & video imaging|
|CCD Field of view:||18 x 18 arcmin|
|Controls:||Manual (motorised) slew with digital readouts.|
|Drive:||Electric stepper motor|
The telescope drive was originally gravity driven and regulated by
Grubb's pendulum-controlled electro-mechanical regulating
system. Later, the gravity drive was replaced by a three-phase
electric motor. The current system provides digital control, so
tracking and positioning can now be controlled by computer, alongside
other systems like the CCD imaging.
The resulting simplifications in operations have opened up use of the telescope to more students, and allow more ambitious observing projects to be attempted. The telescope can now be pointed with an accuracy of approximately ten arcseconds (rms), so that even faint, isolated targets can be reliably acquired.
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