Telescopes. A Warm Up Exercise. A Warm Up Exercise. A Warm Up Exercise. A Warm Up Exercise. Key Ideas:
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1 Telescopes A Warm Up Exercise If we measure the wavelengths of emission lines and absorption lines from the same gas, we find that (ignoring any Doppler shifts) a) Some emission lines shift to the red and some to the blue b) The pattern of wavelengths is completely different c) The emission lines are shifted to shorter wavelengths d) The wavelengths are the same e) The emission lines are shifted to longer wavelengths A Warm Up Exercise If we measure the wavelengths of emission lines and absorption lines from the same gas, we find that (ignoring any Doppler shifts) a) Some emission lines shift to the red and some to the blue b) The pattern of wavelengths is completely different c) The emission lines are shifted to shorter wavelengths d) The wavelengths are the same e) The emission lines are shifted to longer wavelengths A Warm Up Exercise A Doppler shift in the spectral lines of a star is enough to tell us a) How fast the distance to the star is changing b) The distance to the star c) How fast the star is moving d) How fast the observer is moving e) The temperature of the star A Warm Up Exercise A Doppler shift in the spectral lines of a star is enough to tell us a) How fast the distance to the star is changing b) The distance to the star c) How fast the star is moving d) How fast the observer is moving e) The temperature of the star Key Ideas: Light Gathering Power Types of Telescopes: Refracting (lenses) Reflecting (mirrors) Observatory Sites Other Types of Telescopes: Radio Telescopes Space Telescopes 1
2 The Quest for More Light The basic function of a telescope is: gather light from a distant object concentrate (focus) the light into an image make a higher resolution image Simplest telescope is the human eye: Lens focuses the light from an object into an image on the retina at the back of the eye. Has a small collecting area (<1 cm 2 for a fully dilated pupil) The Diffraction Limit Because light acts like a wave, you have to worry about how the waves add up when you produce an image using a lens or a mirror These effects from Diffraction limit the ultimate resolution of a telescope This is what the image of a perfect point source should look like from a perfect telescope the width of the central peak is what is meant by the diffraction limit Collecting Area Retina The surrounding rings are a consequence of the wave nature of light (although you will also get the same answer using photons) Lens How small an angle can you resolve? Theoretical diffraction limit for a telescope of diameter D The atmosphere blurs the images stars twinkle 0.1(1m/D) arcsec Bigger telescopes should have better resolution Your eyes are an example of a small telescope D 1.5cm 0.015m So they have a resolution of 60arcsec 1arcmin 0.02degrees radians A star twinkling your image will be the average of all these Adaptive optics a computer controlled mirror is removing the twinkles to try to get back to the diffraction limit. 2
3 Light Gathering Power The measure of a telescope is its Light Gathering Power: The total collecting area of the telescope. The greater the area, the more light can be collected. We usually state the diameter of the telescope: Light Gathering Power increases as the square of the diameter of the primary collecting optic. Refracting Telescopes Uses large lenses to gather light: Original form of the telescope (Lipperhey s spy glass & Galileo s telescopes) Large Objective Lens to gather and focus light. Objective is usually a compound lens to help correct color distortions. Employs smaller secondary lenses to form images for an eye, camera, or spectrometer. Most common telescope until the 1900s. Simple Refracting Telescope Objective Lens Focus Secondary Lens (Eyepiece) Refracting Telescopes (cont d) The size of a refracting telescope is limited by the largest lens that you can make: Larger lenses are heavier, and tend to sag under their own weight, ruining the images. Long tubes are hard to keep mechanically stiff and flex under the weight of the lens. Largest: 40-inch Yerkes Refractor: In Williams Bay, Wisconsin (U Chicago) Lens is mounted on a 69-foot steel tube. Tube is 69-feet long Dome is 75-feet in diameter Focal Station at the Back (Astronomer for scale) 3
4 Reflecting Telescopes Invented by Isaac Newton. Uses a curved (concave) mirror to focus the light. Primary Mirror gathers and focuses light Use secondary mirrors to direct the light to cameras and spectrometers. All modern large telescopes are reflecting telescopes. Prime Focus Secondary Mirror Primary Mirror Cassegrain Focus Reflecting Telescopes (cont d) Advantages: Mirrors can be supported from behind, and thus can be made very large. Largest single mirror is 8.4-meters (27.6 ft) in diameter (Large Binocular Telescope). Largest reflecting telescopes are the Keck 10-meter telescopes on Mauna Kea, Spanish 10.4m GTC on the Canary Islands Use 36 smaller hexagonal segments to build up the collecting area, under computer control. Newton s Reflecting Telescope 8-meter VLT Telescope (European Southern Observatory) 8.4-meter LBT Mirror 1 10-meter Segmented Mirror of Keck I 4
5 The Largest Telescopes 10-meter Keck I & II 10.5-meter Grand Telescope Canarias (Spain) 10-meter Keck I and II (Caltech, UC, NASA) 8.3-meter SUBARU (Japan) 8.1-meter GEMINI (US, UK, Canada, Chile, Brazil, Argentina, & Australia). One in Hawaii, one on Cerro Pachon, Chile 8-meter Very Large Telescopes (European) 4 telescopes on Cerro Paranal, Chile Twin 8.4-meter Large Binocular Telescope Mt. Graham, Arizona 8-meter VLT (UT1 and UT2) LBT: Mirror 1 and a Computer Model The Large Binocular Telescope LBT Enclosure on Mt. Graham 5
6 Basically the same size as this except you can spin it around in circles. Some Assembly Required Radio Telescopes Use antennas to detect cosmic radio waves: Radio-wavelength lines of Hydrogen and Molecules (CO) from cold interstellar gas Radio emitted by hot electrons, or electrons accelerated by strong magnetic fields. Interferometry: Trick of ganging together many smaller telescopes to achieve the higher resolution of a large single dish (aperture synthesis). Very Large Array Socorro New Mexico meter Radio Telescopes, on movable tracks designed for radio observations at cm to m wavelengths 304-meter (1000 foot) Radio Dish Arecibo, Puerto Rico 6
7 Space Telescopes Newest addition, Atacama desert Chile 66 dishes designed to work at wavelengths of mm rather than cm driest desert in world average rain/snow-fall a few mm/year Only radio waves, visible light, and some infrared light penetrate the atmosphere. Need to go into space to observe all others: Infrared Telescopes Ultraviolet Telescopes X-Ray and Gamma-Ray Telescopes They are very expensive ($100M to $Billions) to build and operate. The Electromagnetic Spectrum NASA s Space Observatories Blocked Blocked Blocked Hubble Space Telescope UV, Visible, IR imaging & spectroscopy Chandra X-Ray Observatory X-Ray imaging & spectroscopy Spitzer Space Telescope (SST) Thermal infrared imaging & spectroscopy Hubble Space Telescope SIRTF: Space Infrared Telescope Facility Chandra X-Ray Observatory 7
8 Smaller, Dedicated Satellites to determine the nature of our universe -- WMAP Or Search for Planets -Kepler The next ground based telescope? Giant Magellan Telescope 5 mounts 4 telescopes per mount 14cm lens, 2k 2k thinned CCDs degree field-of-view 7.8" pixel scale V-band and g-band filters limiting magnitude V~17 (g~18) 6,000 images per night 40,000 square degrees per night Telescopes Data 4.5 8
9 LCOGT 1 meters Magellan 2 x 6.5 meter LBT 2 x 8.4 meter Du Pont 2.5 meter MDM 2.4 meter Liverpool Telescope 2 meter Swift satellite many others (SALT, UH 2.2m, FLWO 1.5m, NOT 2.5m, Faulkes, HST, Chandra, VLA ) Follow-up Facilities 9
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