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Lord's Bridge railway station

1862 establishments in EnglandDisused railway stations in CambridgeshireFormer London and North Western Railway stationsPages with no open date in Infobox stationRailway stations in Great Britain closed in 1968
Railway stations in Great Britain opened in 1862Use British English from January 2018
Lords Bridge station Mar2009
Lords Bridge station Mar2009

Lord's Bridge was a railway station on the Varsity Line which ran between Oxford and Cambridge. Situated in the north of the parish of Harlton on the western outskirts of Cambridge, it was the penultimate station before the line's eastern terminus at Cambridge. The station opened in 1862 and closed more than a century later in 1968. The site is now part of the Mullard Radio Astronomy Observatory, which includes several rail-mounted radio-telescopes.

Excerpt from the Wikipedia article Lord's Bridge railway station (License: CC BY-SA 3.0, Authors, Images).

Lord's Bridge railway station
Cambridge Road, South Cambridgeshire

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Wikipedia: Lord's Bridge railway stationContinue reading on Wikipedia

Geographical coordinates (GPS)

Latitude Longitude
N 52.1706 ° E 0.0389 °
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Address

Mullard Radio Astronomy Observatory

Cambridge Road
CB23 1EX South Cambridgeshire
England, United Kingdom
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Lords Bridge station Mar2009
Lords Bridge station Mar2009
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Ryle Telescope
Ryle Telescope

The Ryle Telescope (named after Martin Ryle, and formerly known as the 5-km Array) was a linear east-west radio telescope array at the Mullard Radio Astronomy Observatory. In 2004, three of the telescopes were moved to create a compact two-dimensional array of telescopes at the east end of the interferometer. The eight antennas have now become the Arcminute Microkelvin Imager Large Array. The Ryle Telescope was an eight-element interferometer operating at 15 GHz (2cm wavelength). The elements were equatorially mounted 13-m Cassegrain antennas, on an (almost) east-west baseline. Four aerials were mounted on a 1.2 km rail track, and the others were fixed at 1.2 km intervals. Baselines between 18 m and 4.8 km were therefore available, in a variety of configurations. For high-resolution imaging, the mobile aerials were arranged along the track, to give uniform baseline coverage to 4.8 km; for low-brightness astronomy (e.g. the Sunyaev-Zel'dovich effect) the mobile aerials were arranged in a 'compact array', with a maximum baseline of about 100 m. All antenna pairs were correlated, so some long baseline data were always available, even in the 'compact array' configuration. As the telescope was an east-west instrument, most imaging observations involved 12-hour observations in order to fill the synthesised aperture (calibration observations are routinely interleaved). Another consequence of the geometry was that it is not practical to image sources near the equator, or in the south. The two-dimensional Large Array overcomes this problem with its new north-south baselines. Although the telescope was not designed as a common user instrument, the operators were happy to accept proposals for observing time on the instrument from outside observers, provided that they did not overlap substantially with existing observing programmes, on a 'best efforts' basis. Monitoring variable sources was possible using short observations which could often be inserted between longer 'standard' observations. The telescope had three main scientific programs: study of the Sunyaev-Zel'dovich effect in galaxy clusters, particularly in determining the Hubble constant; surveying for radio sources that would contaminate degree-scale observations of the cosmic microwave background made with the Very Small Array, and flux monitoring of galactic variable sources.