If you have ever watched the stars with a group of friends, you know that there’s plenty of starlight to go around each of you can see each of the stars. (To provide some reference point, however, keep in mind that just renovating college football stadiums typically costs hundreds of millions of dollars-with the most expensive recent renovation, at Texas A&M University’s Kyle Field, costing $450 million.) The reason astronomers keep building bigger and bigger telescopes is that celestial objects-such as planets, stars, and galaxies-send much more light to Earth than any human eye (with its tiny opening) can catch, and bigger telescopes can detect fainter objects. Now they tend to be huge devices the most expensive cost hundreds of millions to billions of dollars. Telescopes have come a long way since Galileo’s time. Even his small telescope-used over many nights-revolutionized ideas about the nature of the planets and the position of Earth. While Hans Lippershey, Zaccharias Janssen, and Jacob Metius are all credited with the invention of the telescope around 1608-applying for patents within weeks of each other-it was Galileo who, in 1610, used this simple tube with lenses (which he called a spyglass) to observe the sky and gather more light than his eyes alone could. (credit a: modification of work by Allard Schmidt) (b) Stonehenge, a prehistoric site (3000–2000 BCE), is located in England. (a) Machu Picchu is a fifteenth century Incan site located in Peru. The eye was the only device available to gather light, all of the colors in the light were observed at once, and the only permanent record of the observations was made by human beings writing down or sketching what they saw.įigure 2: Two Pre-Telescopic Observatories. Many of these ancient observatories had religious and ritual functions as well. At these ancient observatories, they could measure the positions of celestial objects, mostly to keep track of time and date. Many ancient cultures built special sites for observing the sky (Figure 2). Let’s first look at the development of the telescope. The history of the development of astronomical telescopes is about how new technologies have been applied to improve the efficiency of these three basic components: the telescopes, the wavelength-sorting device, and the detectors. (credit a: modification of work by Howard McCallon/NASA/IRAS credit b: modification of work by Howard McCallon/NASA/IRAS credit c: modification of work by Michael F. (c) Infrared radiation: here, we mainly see the glowing dust in this region. The bright, hot stars in Orion are still seen in this image, but so are many other objects located at very different distances, including other stars, star corpses, and galaxies at the edge of the observable universe. The colors are artificial, changing from yellow to white to blue with increasing energy of the X-rays. (b) X-rays: here, the view emphasizes the point-like X-ray sources nearby. (a) Visible light: this shows part of the Orion region as the human eye sees it, with dotted lines added to show the figure of the mythical hunter, Orion. The same part of the sky looks different when observed with instruments that are sensitive to different bands of the spectrum. Third, we need some type of detector, a device that senses the radiation in the wavelength regions we have chosen and permanently records the observations.įigure 1: Orion Region at Different Wavelengths. But at other times, we want to see individual spectral lines to determine what an object is made of, or to measure its speed (as explained in the Radiation and Spectra chapter). For example, we might simply want to separate blue light from red light so that we can determine the temperature of a star. Second, there is an instrument attached to the telescope that sorts the incoming radiation by wavelength. Just as you can catch more rain with a garbage can than with a coffee cup, large telescopes gather much more light than your eye can. First, there is a telescope, which serves as a “bucket” for collecting visible light (or radiation at other wavelengths, as shown in Figure 1. There are three basic components of a modern system for measuring radiation from astronomical sources.
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