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The European Extremely Large Telescope (E-ELT)
The European Extremely Large Telescope (E-ELT)

... be phased and, to this purpose, we have been working within the FP6 ELT Design Study programme, and within the Project Office, to develop both a phasing methodology and the requisite sensors. The ac­tive phasing experiment will test different phasing sensors on a small segmented mirror. It is to be ...
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... • The Giant Void (Supervoid), is an extremely large void (part of the universe containing very few galaxies) within the vicinity of this constellation. It may possibly be the largest void ever discovered, slightly larger than the Eridanus Supervoid and 1,200 times the volume of expected typical void ...
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summary - guideposts
summary - guideposts

... How do planets form? Modern astronomy reveals that the matter in our solar system was formed in the big bang, and the atoms heavier than helium were cooked up in a few generations of stars. The sun and planets evidently formed from a cloud of gas in the interstellar medium. In general, planets that ...
Do It Yourself Telescopes
Do It Yourself Telescopes

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Miss Nevoral - Ms. Nevoral`s site

... Section 10.1 – Explaining the Early Universe (pages 346 – 355) 1. Define astronomers: People who study space and objects in space. 2. Explain why scientific theories are not considered the final truth/fact about something. Theories are developed with existing information. The main ideas about a theo ...
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The Universe and Galaxies - West Jefferson Local Schools

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Uranus - WordPress.com

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... 130 B.C. - Greek astronomer Hipparchus develops the first accurate star map and star catalogue, and a reliable method to predict solar eclipses 46 B.C. - Julius Caesar, after consulting the astronomer Sosigenes of Alexandria, introduces the Julian Calendar, a regular year of 365 days divided into 12 ...
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Stellar Evolution - University of California, Santa Cruz

... • Upper mass limit is around 100 solar masses set by inability for a star to hang on to its outer layers because high radiation pressure (high luminosity). ...
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... motion towards or away from Earth. Thus, the Wobble method provides for a wider range of planetary systems. If both methods can be used on a exo-system, the size and mass of the planets can be determined. Given these two methods, it’s not entirely surprising that many of the earliest exo-planets dis ...
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... • Upper mass limit is around 100 solar masses set by inability for a star to hang on to its outer layers because high radiation pressure (high luminosity). ...
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... electromagnetic waves called radio waves. The radio waves travel through space and through Earth's atmosphere. They're then converted back into sound waves by electronic equipment and audio speakers. Radio waves and visible light from the Sun are just two types of electromagnetic radiation. Other ty ...
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... The star Rigel, which belongs to Orion, is blue-white because of its high temperature and 57000 times brighter than our sun. In spite of the distant of 540 light years from the Earth, it shines as the seventh brightest star in our night sky. The astronomers believe, that Rigel is the most luminous s ...
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... • Certain light-sensitive chemicals (usually silver oxide) are placed on glass plates or on plastic film. • The chemicals are altered when exposed to light, the degree to which depends on the intensity of the light. • A chemical “development” process “freezes” the chemicals in their altered states, ...
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... monitoring an area of 3 square degrees along the bar in the LMC, and also an area of 1 square degree in the central part of the SMC. In the last 10 years, we observed these areas about 80-90 and 100-110 times for LMC and SMC, respectively. As a result, we obtained time series data with more than 3,0 ...
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THE BIG BANG THEORY
THE BIG BANG THEORY

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... Our target list is composed of objects being surveyed both for SETI and for other astrophysical interests. Dave Latham and colleagues have recently begun characterizing 11,000 F, G, and K dwarfs (2000 completed thus far) for possible observations by next generation targeted SETI searches. Specificall ...
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Spitzer Space Telescope



The Spitzer Space Telescope (SST), formerly the Space Infrared Telescope Facility (SIRTF), is an infrared space observatory launched in 2003. It is the fourth and final of the NASA Great Observatories program.The planned mission period was to be 2.5 years with a pre-launch expectation that the mission could extend to five or slightly more years until the onboard liquid helium supply was exhausted. This occurred on 15 May 2009. Without liquid helium to cool the telescope to the very low temperatures needed to operate, most of the instruments are no longer usable. However, the two shortest-wavelength modules of the IRAC camera are still operable with the same sensitivity as before the cryogen was exhausted, and will continue to be used in the Spitzer Warm Mission. All Spitzer data, from both the primary and warm phases, are archived at the Infrared Science Archive (IRSA).In keeping with NASA tradition, the telescope was renamed after its successful demonstration of operation, on 18 December 2003. Unlike most telescopes that are named after famous deceased astronomers by a board of scientists, the new name for SIRTF was obtained from a contest open to the general public.The contest led to the telescope being named in honor of astronomer Lyman Spitzer, who had promoted the concept of space telescopes in the 1940s. Spitzer wrote a 1946 report for RAND Corporation describing the advantages of an extraterrestrial observatory and how it could be realized with available or upcoming technology. He has been cited for his pioneering contributions to rocketry and astronomy, as well as ""his vision and leadership in articulating the advantages and benefits to be realized from the Space Telescope Program.""The US$800 million Spitzer was launched from Cape Canaveral Air Force Station, on a Delta II 7920H ELV rocket, Monday, 25 August 2003 at 13:35:39 UTC-5 (EDT).It follows a heliocentric instead of geocentric orbit, trailing and drifting away from Earth's orbit at approximately 0.1 astronomical unit per year (a so-called ""earth-trailing"" orbit). The primary mirror is 85 centimeters (33 in) in diameter, f/12, made of beryllium and is cooled to 5.5 K (−449.77 °F). The satellite contains three instruments that allow it to perform astronomical imaging and photometry from 3 to 180 micrometers, spectroscopy from 5 to 40 micrometers, and spectrophotometry from 5 to 100 micrometers.
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