There no world-class optical telescopes in the UK. The reason for this is cost. The world's largest telescopes cost hundreds of millions of pounds. Construction has started on the 32-m diameter E-ELT, with an estimated cost of €1 billion. It makes sense to build these telescopes in the best locations on Earth. None of these are in continental Europe. So what makes a site suitable for a billion Euro telescope?
L09: Professional Observatories locations and technology
Radio telescopes can see through cloud. Optical telescopes can't! This is one of the primary reasons there are no major research telescopes in the UK. Figure 54 (left) shows monthly average cloud cover. Desert regions including Antarctica, Australia, parts of Africa and the west coast of the Americas provide some of the best cloud-free skies.
Light from street lights and industry can greatly increase the sky background. The increased background light causes increased noise in astronomical images, making it harder to detect faint sources. Therefore, the largest telescopes are placed in regions of low light pollution. Figure 55 shows the artificial night sky brightness around the world. It can be seen that some of the regions which show low cloud cover in figure 54, such as the sparsely populated western coasts of South America and Africa, are also largely free of light pollution. Figure 55 also clearly shows why no major telescopes are now built in mainland Europe.
Selecting a site with good seeing is one of the most important criteria. Lower seeing improves the spatial resolution of images. Since the light from the stars is also spread out over fewer pixels, good seeing also improves the signal-to-noise ratio. Seeing is caused by turbulence in the atmosphere and this has two causes: heat from the ground rising through the atmosphere and strong winds higher in the atmosphere (e.g the jet stream).
The atmosphere over the sea tends to be much less turbulent than the atmosphere over land, as the sea exhibits an essentially smooth, constant-temperature surface compared to the land. Some of the best astronomical sites are therefore located on small islands in the middle of oceans, such as Hawaii and the Canaries, as these small land masses cause little additional turbulence. For the same reason, coastal regions that receive winds predominantly from the direction of the ocean, such as the western coasts of the Americas and Africa, also exhibit excellent seeing.
The higher the site of an astronomical observatory, the thinner the atmosphere above the telescope. This reduces atmospheric extinction, and can also help reduce the seeing if the observatory lies above a turbulent layer in the atmosphere. High-altitude telescopes are also often above the local inversion layer in the atmosphere, meaning that local cloud formation occurs below the telescope, significantly increasing the number of usable nights at the observatory compared to a telescope sited below the inversion level.
Additional factors, such as the difficulty of supplying utilities like water and power, accessibility, humidity and wind speed all play a lesser role in locating professional observatories. For a detailed discussion of many of these factors, see Vik Dhillon's old notes.
Political stability is also a factor in the location of large telescopes. This has been a particular issue in recent years, with protests from Native Hawaiians causing severe issues for the Thirty Meter Telescope project's plans to build their telescope on Mauna Kea.
The world's largest telescopes
Figure 56 shows the sites of the worlds largest telescopes. For the reasons discussed above these are clustered around a few major sites, namely Chile, Hawaii and the Canary Islands. The gallery below shows photos of these observatories. These sites have low cloud cover, low light pollution, good seeing and low humidity. They are all at high altitude and are politically stable.
The Keck and Subaru telescopes at the summit of Mauna Kea, Hawaii.
The Roque de los Muchachos Observatory (ORM) on La Palma in the Canary Islands.
The Very Large Telescopes (VLT) at the Paranal Observatory in the Atacama Desert, Chile.
Space Based Observatories
The factors which degrade astronomical images, such as seeing, sky background, transparency variations and extinction are all atmospheric-induced phenomena. These effects can all be removed at a stroke by siting optical telescopes in space. The best known example of this is the 2.4 m Hubble Space Telescope (HST), which has helped to revolutionise astronomy since 1990 with its diffraction-limited imaging capability. Because space-based telescopes don't suffer from atmospheric extinction, HST also allows astronomical observations in the UV - impossible from the ground! The main drawback with siting telescopes in space is the cost: the HST cost many billions of dollars to build and operate, approximately ten times the sum required for the largest ground-based telescopes.
Another drawback with space is the risk involved in the launch, and the great difficulty of fixing problems, servicing the telescope and upgrading the instrumentation once the telescope has been deployed. For the HST, servicing missions, which cost nearly $1 billion each, were of limited number and were very risky for the astronauts involved. More recent telescopes, such as the JWST, have been located much further from Earth and the Sun to keep them cool for as long as possible; servicingmissions for these telescopes are impossible, so they had better work!
We have already seen that telescopes use mounts to track the motion of stars in the sky. In practice, it isn't possible to do this accurately enough for professional work, or even for amateur astrophotography. This is due to mechanical imperfections in the drive systems of the mount, flexure of the mount, and misalignment of equatorial mounts with regard to the celestial pole.
The result is that stars drift slowly across the field of view, which would cause smearing in long exposures. To get round this, it is necessary to guide telescopes. This is done using an autoguider, a system which monitors the position of a star somewhere in the field of view, and nudges the telescope to keep the guide star locked onto the same pixel on the autoguider's detector.
There are two main types of autoguiders in use. Guidescopes use a separate, smaller telescope to image a wider field of view. The wide field of view means that guide scopes are likely to find a bright star to guide on, but because they are mechanically separate from the main telescope, they can flex relative to the main scope. This means that, even though the guide star is held fixed, the main telescope's view of the sky can drift slowly. Off-axis guiders use a mirror on a moveable stage to pick off some light from the main telescope, and focus it on a separate autoguiding camera. This exhibits less flexure than the guidescope method, and is the one most often used for large telescopes. Both designs are shown below in figure 58.
The huge mirrors in the world's largest telescopes pose a difficult engineering problem - they can be too heavy. For example the 4.2 m mirror of the William Herschel Telescope (WHT) on La Palma, for example, has a thickness of 56 cm and a weight of 16.5 tonnes (see figure 59). Larger mirrors of the same thickness would be too heavy to move. But a thinner, lighter mirror will bend and change shape as the telescope moves, due to the effects of gravity. This distortion of the primary mirror would ruin the focusing properties of the telescope, producing poor quality images. Despite this, the 8-m mirror of the Very Large Telescope (VLT) in Chile is only 18cm thick and weighs only 24 tonnes. If it were the same thickness as the WHT mirror it would weigh around 100 tonnes!
The distortion of modern, thin mirrors is overcome by active optics, where the thin (and hence flexible) mirror is mounted on a set of actuators, which are devices that transform an electrical signal into linear motion. The system works as follows (see figure 60): whilst the telescope is observing a science target, the light from a bright reference star somewhere in the field of view around the science target is picked off and the quality of its image is measured. This measurement is usually performed by a wavefront sensor, which we shall discuss in more detail in the next lecture. The actuators are used to push and pull different parts of the primary mirror so that its shape changes in such a way as to improve the quality of the reference star image. Only about one measurement and correction cycle per minute is required, as the orientation of the telescope whilst tracking a target does not change significantly on timescales shorter than this. Note that, as well as correcting the shape of the primary mirror, many active optics systems also correct for the change in the position of the secondary mirror (see figure 60). This corrects for changes in the shape of the telescope itself, which can occur due to flexure under gravity or expansion and contraction caused by changes in temperature.
Figure 60: schematic showing the components of a typical active optics system. Note the actuators (shown as green springs) controlling the primary mirror shape and the vertical and horizontal position of the secondary mirror.
An increasingly common alternative to the single-piece mirrors shown in figure 59 are segmented mirrors. This approach has been adopted, for example, on the twin 10 m Keck telescopes. The segments are typically hexagonal in shape and usually have an asymmetric profile so that when all of the segments are combined they form, for example, a hyperbolic shape. Active optics systems are essential for segmented-mirror telescopes, as the position of each segment needs to be carefully controlled so that the overall shape of the primary mirror is retained as it is tilted to different sky positions. Each segment is therefore mounted on its own set of actuators.
Segmented mirrors are the only feasible way of constructing telescopes with apertures significantly in excess of 8 m, as single-piece mirrors would become extremely expensive and ultimately impossible to manufacture, transport, install and maintain. The European Extremely Large Telescope (E-ELT) will have a 39 m mirror, composed of 798 elements, each 1.4 m wide and 5 cm thick.