Measuring Light waves
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1 Measuring Light waves We normally measure wavelengths (λ) using nanometers (nm) 1 nm = 10-9 m nm Increasing wavelengths (λ)! Visible light has wavelengths between nm! To detect other types of light, astronomers launch telescopes into space on satellites
2 ! Objects in space give off every kind of light.! However only visible light and radio waves reach Earth s surface! (some Ultra-violet light also reaches Earth) Wavelengths (λ)
3 How Do Telescopes Work? The main purpose of a telescope is to gather light. To do this we need to bend the light and focus it to a point. There are two ways to do this: lenses & mirrors
4 Focusing with Lenses focus focus The Focus is the point at which the light converges. Focal length = distance from the lens to the focus
5 Refractors Galileo s telescope used lenses to bend, or refract, and focus the light. Telescopes using lenses are called refractors. The largest refractors use 40-inch lenses. But refractors are ultimately limited in size. Lick Observatory, CA
6 Focusing with Mirrors: Reflectors To bring parallel light to a focus, we can use a mirror with a special dish-like shape *. Telescopes that use mirrors Are called reflectors. Today, all research telescopes are reflectors. Focus ( * called a paraboloid)
7 Refracting vs Reflecting Telescopes Refracting Telescope: Lens focuses light Reflecting Telescope: Mirror focuses light
8 Telescope Types Newtonian Primary Mirror Isaac Newton invented a reflecting telescope Light reflects off its curved primary mirror Then is sent to an eyepiece by a flat secondary mirror This design is still used by amateurs
9 Telescope Types Cassegrain Primary Mirror A Cassegrain telescope has a hole in the primary mirror. The light comes to a focus behind the primary mirror.
10 The primary mirror at Keck Observatory is 10 meters in diameter.
11
12 Telescopes have Three Powers 1. Light Gathering Power: The ability to collect light 2. Resolving Power: The ability to see fine details 3. Magnifying Power: The ability to make objects look bigger
13 Pizza Time!!! You and your friends are buying Pizza. Pizzas with a larger diameter cost more. Which is a better deal? A. 9 inch pizza for $10.00 B. 18 inch pizza for $25.00 C. They are the same. One 18-inch pizza = FOUR 9-inch pizzas
14 Light-gathering power Light-gathering power determines how faint a star a telescope can see. It depends on the area (A) of the primary lens or mirror: D Area = π (r) 2 A = π (D/2) 2
15 Light Gathering Power: Example The Keck telescope in Hawaii has a 10 meter primary mirror, while a telescope at McDonald observatory in Texas has a 1 meter telescope. Question: Keck can see fainter stars, but how many times fainter? Answer: The greater a telescope s Light Gathering Power, the fainter an object it can see. Light Gathering power depends on Area: A = π(d/2) 2 [D=diameter] D Keck = 10 m ; D Mc = 1 m A Keck = π ( D Keck /2) 2 ; A Mc = π (D Mc /2) 2 A keck / A mc = [π (D Keck /2) 2 ] / [π (D Mc /2) 2 ] = (D keck /D Mc ) 2 = (10/1) 2 = 100 Keck can see stars which are 100 times fainter!
16 Resolving Power: Seeing Details Resolving Power (or resolution) is a telescope s ability to see small details. It is proportional to a telescope s size (diameter D)
17 Magnification makes things look larger However it does not improve resolution (seeing fine details).
18 The Best Location for a Telescope Far away from civilization to avoid light pollution Text
19 On a mountaintop Mauna Kea, Hawai i (~14,000 feet elevation)
20 Or in Space Space Telescopes avoid the blurring effects of Earth s Atmosphere. Hubble Space Telescope
21 Space Telescopes also allow us to see light blocked by Earth s atmosphere: infrared, ultraviolet, X-rays & gamma rays. Spitzer (2003) Fermi Gamma Ray Observatory (2008)
22 Andromeda Galaxy Visible Light Infrared Light
23 A newer IR image from the WISE satellite IR camera
24 X-ray Astronomy X-rays are high energy light with very short wavelength They are emitted by very hot gas in the universe. Chandra X-ray Telescope Chandra Image of Supernova Explosion
25 The Largest Radio Telescope Since radio waves pass through Earth s atmosphere, we can build radio telescopes on the ground. The 300-m telescope in Arecibo, Puerto Rico is the largest in the world. It can hold 13 football fields!
26 Review of Chapter 3 " To understand what s in space, we must understand light. " Light is an electro-magnetic wave with three properties: " Speed: c = 300,000 km/s " Frequency (f): number of light waves per second. " Wavelength (λ): distance. from one peak to the next " We see different wavelengths as colors " These three are related: c = f x λ " Many forms of light exist, most invisible to humans: " Infrared radiation and radio waves have longer wavelengths than visible " Ultraviolet, X rays, and gamma rays have shorter wavelengths " Visible light occupies only a small portion of the elctromagnetic spectrum.
27 Chapter 3 Review " Visible light waves are small: their wavelengths are measured in nanometers (1 nm = 10-9 m) " Visible light range: λ=400 nm (violet) to λ=700 nm (red) " Light s energy depends on its frequency " Telescopes: gather light, reveal details, and magnify images " The two main types: " Reflectors produce images using mirrors, " Refractors use lenses to focus light " Light gathering ability depends on the telescope mirrors s area. " The area of a circle is: A = π r 2
28 The Power of Starlight Chapter 4 By analyzing the light from a star, we learn about its: 1. Temperature 2. Composition 3. Motion
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