Parsons improved the techniques of casting, grinding and polishing large telescope mirrors from speculum metal, and constructed steam-powered grinding machines for parabolic mirrors. His mirror of 1839 was cast in smaller pieces, fitted together before grinding and polishing; its 1840 successor was cast in a single piece. In 1842, Parsons cast his first mirror, but it took another five casts, before he had two ground and polished mirrors. Speculum mirrors tarnished rapidly; with two mirrors, one could be used in the telescope while the other was being re-polished. The telescope tube and supporting structure were completed in 1845. The mirror was 5 in thick and weighed almost 3 tons. This required a mirror cell to support and to prevent the mirror deforming under its own weight. The length of the tube and mirror box is about ; including the mirror it weighed about 12 tons. The tube is supported at the mirror end by a "universal joint", a hinge with two axes, which allows the tube to be inclined through a large range of altitude and also to be turned through a limited range of azimuth. The azimuth range is limited to about one hour by the supporting walls that flank the tube on its eastern and western sides. The walls are apart, high, and long. A chain and counterweight keeps the telescope in balance, another chain with a winch controls the altitude. A rack and pinion beam underneath the tube controls the azimuth. This beam is connected to the eastern supporting wall, where it can move on a circular iron arc to allow the telescope to change altitude. The tube is of the Newtonian design with the eyepiece on its western side. At low altitude, the observer accesses the eyepiece from a wooden gallery that spans the distancebetween the walls and can slide up and down guides to follow the telescope in altitude. A cage on the gallery moves sideways to reach the eyepiece at different azimuth. At high elevation, curved galleries on top of the western wall are used, which can be moved across the wall to follow the telescope in azimuth.
Operation
The purpose of the telescope was to re-visit the nebulae in the catalogues of Charles Messier and John Herschel. These catalogues list star clusters as well as nebulae, and the question was whether the latter were merely unresolved star clusters or genuinely nebulous regions of space. It resolved into stars unclear areas which might be the first galaxies to be identified as such. Parsons discovered that several nebulae had a spiral structure, suggesting "dynamical laws". The most notable spiral nebula observed by Parsons was Messier 51, which he resolved into stars. After William Parsons died in 1867, the 4th Earl continued to operate the six-foot telescope. From 1874 to 1878, J. L. E. Dreyer worked with the telescope and began the compilation of his New General Catalogue of Nebulae and Clusters of Stars. Although the 4th Earl built a smaller 3 ft equatorial in 1876, the six-foot telescope remained in use until about 1890. After his death in 1908, the telescope was partly dismantled, and in 1914, one of the mirrors with its mirror box was transferred to the Science Museum in London. The walls remained. The tube, second mirror box, and universal joint survived.
Reconstruction
Following a TV programme, lecture, and book by Patrick Moore, there was renewed interest in the six-foot telescope in the 1970s. Gradually, the telescope became a visitor attraction. But it was not until the 1990s that plans to actually rebuild the telescope came to fruition. In 1994 the retired structural engineer and amateur astronomerMichael Tubridy was called in to research and re-design the Rosse six-foot telescope. The original plans were lost, and so it took detective work to review the remains of the telescope, incidental comments in observing logs, and contemporary photographs taken by Mary Rosse, wife of the 3rd Earl. Reconstruction work lasted from early 1996 to early 1997. It had been planned to include a working mirror, but due to budget constraints this had to be left for a separate project. The new mirror was installed in 1999. Unlike the speculum original, and unlike modern aluminium- or silver-coated glass mirrors, this is made of aluminium, as a compromise between authenticity and utility in astronomical observation.
Modern companion radio telescope
In 2017, LOFAR radio-telescope station IE613, one of some 50 similar stations in Europe, was constructed in the grounds of the castle. This is the westernmost station in the LOFAR network. LOFAR makes observations in the 10 MHz to 240 MHz frequency range with two types of antennas: Low Band Antenna and High Band Antenna, optimized for 10-80 MHz and 120-240 MHz respectively. The Birr Castle station consists of 96 LBA's and 96 HBA's and a total of 96 digital Receiver Units. The Birr Castle station on its own is the Irish Low Frequency Array I-Lofar telescope. In 2018, I-LOFAR observed for the first time a billion-year-old red-dwarf, flare star called CN Leo, almost 75 trillion kilometres away.
