|
|
The Northumberland Equatorial Telescope, University Observatory, 18388452 views`The Northumberland' is the only remaining large instrument from the early days of the University Observatory, and is preserved because of its great historical interest. It was for some years one of the world's largest refracting telescopes with an accurate clock-driven equatorial mounting to follow a star in its diurnal motion across the sky.
The Duke of Northumberland, later Chancellor of the University, indicated his wish to present a large telescope to the recently founded Observatory in 1833, and was enthusiastically encouraged by the Director, G.B. Airy.
The lens was an achromatic doublet of 11.6 inches clear aperture and focal length 19ft 6in, made by Cauchoix of Paris. Airy recognised that the mounting needed to be of great rigidity and adopted the `English' form (of which the telescope is indeed one of the prototypes). The polar axis is composed of two massive triangular prisms of ingenious design, in which the components are kept in permanent tension and compression to attain the desired resistance to torsion and flexure.
The main structure was built by the engineers Ransomes of Ipswich, and the fine mechanical work by the London instrument makers Troughton and Simms. The polar axis frame and the telescope tube are of Norwegian fir. The observing chair which gives access to the eyepiece in all positions is the original. The polar axis points upwards to the North celestial pole, at an altitude equal to the latitude of the Observatory (+52degrees 13minutes). A small electric motor, now replacing the original mechanical clock, turns the polar axis once in a sidereal day. Once directed to a star the telescope tube remains in a fixed orientation in space, while the Earth turns beneath it.
A program of automation was started at the end of 2001 to provide high-precision coordinate capability.
The original Cauchoix lens is not (by present day optical standards) very good and it is now in store. The optics on the telescope are modern: a 12 inch aperture visual achromatic doublet designed by Dr R.V. Willstrop of the Institute and constructed by the local firm A.E. Optics Ltd. was installed to mark the 150th anniversary of the telescope.
The steel dome covering the telescope was made by Cooke, Troughton and Simms Ltd. of London & York in 1932 to replace the original wood structure which had become increasingly dilapidated after 96 years.
The telescope was last used in a regular Observatory research programme, for the micrometrical measurement of double stars, in the 1930s. It continues, however, to be actively used for visual observations by members of the University Astronomical Society (founded 1942) who have an Observing Guide on the CUAS website, and for Public Observing on clear Wednesday evenings in the winter months, and so continues a useful life of now over 150 years.
Description source: Institute of Astronomy
|
|
Cara Dillon2678 views
|
|
Cloudy afternoon2645 viewsA view of King's College Chapel from the other side of the river Cam.
|
|
King's College Bridge2596 viewsKing's College Bridge over the river Cam taken from Bodley's court.
|
|
Trinity Hall Bridge2573 viewsConstructed 1639 - 1640
|
|
Eddi Reader2434 views
|
|
Trinity Hall Entrance2408 viewsTrinity Hall Entrance
|
|
Trinity College Great Court2308 viewsThe beauty and size of Trinity's courts attract visitors from all over the world.
|
|
Gonville and Caius College2242 viewsGonville and Caius College
|
|
The Schmidt Camera ?2210 viewsThis instrument was built in 1952 by Grubb-Parsons of Newcastle-upon-Tyne and replaced an older telescope in the existing dome, which had been made by T. Cooke & Sons Ltd. of London & York at the time of the move of the Solar Physics Observatory from South Kensington to Cambridge.
It is a `Classical Schmidt' - the simplest and most efficient form of the ingenious wide-field camera invented in 1930 by Bernhard Schmidt of Hamburg Observatory. Light from the sky falls upon a 61 cm (24-inch) mirror with a spherical reflecting surface, at the bottom of the tube. It is reflected to a focus in the centre of the tube and half-way up it, 163 cm (64 inches) from the primary mirror. At the focus a photographic plate P 15 cm (6 inches) in diameter, which must be bent to fit a curved surface, records the star images in an area of sky 5 degrees in diameter. (The full Moon is half a degree in diameter.)
Without any further optical element the star images would be of poor quality owing to ``spherical aberration'': light falling near the edge of the mirror would come to a focus too close to it, and light falling near the centre of the mirror would be focused a little too far away. Schmidt's invention was to place at the centre of curvature of the primary mirror, near the top of the tube, a weak meniscus lens (in this case 43 cm (17 inches) in diameter) with one aspheric optical surface: this makes the light which passes through it near the edge diverge slightly, lengthening the focus of the outer parts of the mirror, and makes the light passing through near the centre converge, shortening the focus of the centre of the mirror. This optical combination of lens and mirror forms a fast, efficient camera giving sharp star images of uniform quality over the full 5 degrees field. It is an ideal sky-surveying instrument; by contrast the 36-inch (91.4 cm) telescope, with its paraboloidal mirror of 4.1 metres (162 inches) focal length (f/4.5), has a field of view only 7.2 arc minutes in diameter with images smaller than 2 arc seconds.
The auxiliary 15 cm (6 inch) telescope is for guiding. The exposure time is usually of the order of 10 minutes, and during this time the image can wander about on the photographic plate mainly because of irregularities in the refraction in the earth's atmosphere. These are corrected by maintaining a star image at the intersection of the cross-wires in the guiding telescope.
The Palomar and U.K. 48-inch (1.22 metres) Schmidt cameras which were used to make the all-sky surveys (now kept in the Cambridge Astronomical Survey Unit) have apertures nearly three times as large as our telescope, but focal lengths (and tubes) only twice as long. Only one Schmidt camera (the 53-inch (1.35 metres) at Tautenburg, Germany) has ever been built larger than these two. The reason is that, if a Schmidt camera is simply scaled up, its image size is also scaled up, and as Bernhard Schmidt himself predicted, the 48-inch Schmidts are close to the practical limit. The main image defect arises because the thin lens can correct the ``spherical aberration'' of the mirror exactly in only one colour of light, (usually blueish green), red light is under-corrected, and blue or ultra-violet light is over-corrected. To minimise the length of the tube, and so the size and cost of the dome, the 48-inch Schmidts have been made with an aperture of f/2.5 (ours is f/3.7) and the ``spherical aberration'' of the mirror is then 3.2 times as large as in our camera. Three of the largest Schmidt cameras have been fitted with ``achromatic'' lenses which reduce the residual colour errors, but astronomers now use very fine-grain emulsions, and wish to observe a wide range of colours of light, so these large Schmidts are still at the practical limit of size.
Fortunately, a new design of wide-field telescope, using three mirrors and no lenses, has been developed; a prototype can be seen nearby.
Description source: Institute of Astronomy
|
|
Emmanuel College Chapel2144 viewsEmmanuel College Chapel
|
|
Cara Dillon2093 views
|
|
| 125 files on 11 page(s) |
1 |
 |
|
|
|
|
|
|
|
|
