Download The Design and Construction of Large Optical Telescopes by Pierre Bely PDF

By Pierre Bely

This e-book assembles for the 1st time in one textual content the complete variety of astronomical and engineering ideas utilized in the layout and building of huge telescopes. It goals to hide all facets of the sphere, from the basics of astronomical statement to optics, keep watch over platforms, and structural, mechanical, and thermal engineering, in addition to such really expert themes as web site choice and software administration. The e-book is the results of the collaboration of many prime astronomers, engineers, and undertaking managers. Their contributions were edited to supply a constant technique and remedy: for instance, floor- and space-based telescopes are handled from a typical point of view.
Topics coated comprise:
- layout equipment and undertaking administration
- Telescope Optics
- Stray gentle regulate
- constitution and Mechanisms
- Pointing and keep watch over
- energetic and Adaptive Optics
- Thermal keep an eye on
- Integration and Verification
- Observatory Enclosure and Siting

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Extra resources for The Design and Construction of Large Optical Telescopes (Astronomy and Astrophysics Library)

Example text

5 log φ2 . 4(m1 −m2 ) . 1 illustrates the correspondence between magnitude differences and brightness ratios. 1. 75 2. 1. 51 2. 5 10. 5 100 10 10 000 By convention, at all wavelengths, magnitude 0 has been attributed to the bright star Vega (a blue main-sequence star of spectral type A0). Objects brighter than Vega (Sun, bright planets) have negative magnitudes. Accurate photometry is accomplished with photoelectric and solid-state devices and filters which accept only certain wavelength bands. 1).

Astronomical Observations tion, mirror edges and spider, from a slightly different angle on the two sides of the chop. This results in a residual background variation which limits the accuracy of the background subtraction. To remove this residual background difference, which is stable over time scales of minutes, one must repoint the telescope as a whole. This is the socalled “beam-switching” or “nodding” technique. This operation needs to be done often enough, usually on the order of 60 seconds, to eliminate telescope thermal variations.

In the visible, extinction is only about 10–15%, but the atmosphere becomes opaque below 300 nm due to the ozone layer, which is at an altitude of about 20 to 30 km. 35 µm, there are some absorption bands caused by water vapor and oxygen, but the atmosphere is never completely opaque. 3 µm, there begin to occur absorption bands where the atmosphere is completely opaque, especially at low-altitude sites. The transparent wavelength regions (windows), which cor- 10 1. Astronomical Observations Transmission (%) 100 80 L I J N H K M 60 40 20 0 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 Wavelength ( m) Fig.

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