Step 4-Angular Resolution and Light-Gathering Power Let's consider the choices that need to be made between the advantag

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Step 4 Angular Resolution And Light Gathering Power Let S Consider The Choices That Need To Be Made Between The Advantag 1 (30.97 KiB) Viewed 92 times

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Step 4-Angular Resolution and Light-Gathering Power Let's consider the choices that need to be made between the advantages of getting the highest angular resolution and light-gathering power versus the disadvantages of the added cost, mainte- nance, repair, and other practical matters that will occur. • The angular resolution of a telescope is directly proportional to ("proportional to" is given the math symbol o) the wavelength being observed and inversely proportional to the diameter of the aperture of the telescope: angular resolution wavelength/diameter We want the angular resolution to be small (to detect very small details). This means we want to make the telescope as large as possible.

to a 2-meter-diameter 42 ACTIVITY 8 Deciding The light-gathering power is proportional to the area of the aperture. Because the objective lens of a refracting telescope or the main mirror of a reflecting telescope is round, the light-gathering power is proportional to the radius squared. For example, if a telescope can be built with a diameter telescope (radius of 1 meter) is proportional to = 100. The 20-meter telescope has 100 times of 20 meters (radius of 10 meters), the light-gathering power compared more light gathering power than the 2-meter telescope. That is a considerable increase. 8. When building a telescope, the goal is to achieve the smallest angular resolution and highest light-gathering power possible. There may be disadvantages to the telescopes required to meet those goals, such as cost or complexity . Discuss the pros and cons of the following types of telescopes and their locations. Consider both the wavelength region and the diameter when talking about getting the smallest angular resolution. A space telescope built to get the smallest angular resolution for radio wavelengths between 100 and 1,000 meters. b. An extremely large telescope with its main mirror 39 meters in diameter, built on a 3,046-m peak in Chile, to observe visual and near-infrared wavelengths. Sllo 38