Basic optical design features:
- Ritchey-Chrétien Cassegrain optics
- f/10 focus at Cassegrain
- Primary mirror:
- 2.0m diameter
- focal ratio f/3
- 0.45m central bore
- Secondary mirror:
- 0.62m diameter
- moves axially for focus
- Acquisition and Guidance (A&G) box at Cassegrain focus gives
- one straight-through port
- four science fold ports - accessed by deployable science fold mirror at 45° to optical axis, rotatable round optical axis to access all four side ports
- Prime focus image scale: 29.1 µm/arcsec
- Cassegrain image scale: 97 µm/arcsec
- Through port clear aperture:
- 40 arcmin field of view
- field curvature radius -1773mm
- correctable to plane surface with wide-field corrector lens (not fitted)
The autoguider allows closed loop tracking of the telescope and corrects tracking errors by monitoring a guide star. Our autoguider is based around an Andor Technology DV435 frame transfer camera, which has the following specification:
- 1024x1024 active pixels
- 0.22 arcsec/pixel
- 13µm x 13µm pixel size
- Peak Q.E. 95%
- Operating temperature -40°C
- Pixel readout rate 1MHz
It runs under a custom control system, which does dark subtraction, flat-fielding and object detection on frames taken. The system operates over a fixed set of exposure lengths from 50ms to 10s. The guide window is nominally 100x100 pixels, and guide centroids are sent to the Telescope Control System which applies the correction accordingly. You do not need to pick your own guide star. As we have only one autoguider, only translational tracking errors are corrected, rotational errors are not.
Basic telescope mechanical design features:
- Alt/az mount
- Steel tube conventional open truss serrurier design
- Friction-free hydrostatic bearings
- Slew rate 2°/sec on all axes
- Altitude range: 25°–88°
- Zenith avoidance zone = 2° radius (determined by maximum allowed velocity & acceleration of alt/az servos)
- Active primary mirror support — 1.35 tonne mirror dynamically held by axial & lateral pneumatic actuators
- Motion control in alt/az by embedded x86 industrial PCs on & off-mount
- Control data distributed system-wide in real time over switched network
- Services PLC controller for real-time monitoring of telescope, interlocks and hydraulics
The observatory consists of three buildings:
- the enclosure which houses the telescope
- the pump room which contains the hydraulic and pneumatic systems for the telescope and enclosure
- the computer/IT room which houses all computing systems for the observatory
The enclosure is a novel clamshell design, consisting of two shutters, each comprising three separate portals. To open the shutters, two hydraulic rams at either end of the enclosure retract, allowing the top portals to move down and the other two sets of portals follow dynamically. When the enclosure is fully open, the telescope has an unencumbered view of the sky to an optical horizon of 25° altitude, its mechanical horizon being 20°. Fully opening the enclosure takes approximately three minutes.
The entire observatory structure was designed by TTL and built by Cammell-Laird in Birkenhead, the famous shipbuilding company in Merseyside, UK. The hydraulic ram system was designed and built by Hydraulsyd (now PMC Hydraulics) of Sweden.
The Liverpool Telescope's WGS84 coordinates - depending on the format in which you want to enter these data - are:
|28° 45' 44.8"||17° 52' 45.2"||342° 07' 14.8"|
|28° 45.747'||17° 52.753'||342° 07.247'|
|Altitude: 2363 metres / 7753 feet / 1.47 miles|
Contrary to what the name might suggest, the Liverpool Telescope is not in Liverpool at all, but on the island of La Palma, the westernmost of the Canary Islands.
The Canaries are a group of volcanic islands 200-300 km off the northwest coast of Africa. La Palma (arrowed at right) is probably the least developed of the islands in terms of tourism. This, however, is arguably a good thing, given that most of the island boasts breathtaking scenery.
The most distinctive feature of the island is the enormous Caldera de Taburiente, the eroded remains of a volcano that collapsed two million years ago, leaving behind the largest caldera in the world. One point on its rim is the highest point on the island (2426m), called the Roque de Los Muchachos ("Rock of the Little Children") because of the small rock formations there.
The Roque is one of the best observing sites in the world, and for this reason many European observatories have been built there, under the umbrella organisation of the Observatorio del Roque de Los Muchachos ("ORM").