http://www.rssboard.org/rss-specification 720 http://ecuip-xtf.lib.uchicago.edu/xtf/search?docsPerPage%3D100;f6-associated-Lesson%3DX-Ray%20Science Results for your query: docsPerPage=100;f6-associated-Lesson=X-Ray Science Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/8005694/8005694.dc.xml Renamed the Einstein Observatory after launch, the image on the left shows HEAO-2 during pre-flight testing. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/8005694/8005694.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/99828main_axaf2/99828main_axaf2.dc.xml Renamed the Chandra X-ray Observatory after launch, this image shows AXAF during pre-launch testing. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/99828main_axaf2/99828main_axaf2.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Air-Shower-Schematic-GC/Air-Shower-Schematic-GC.dc.xml A schematic diagram of particles in an extensive air shower (EAS), approaching an array of detectors at the speed of light. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Air-Shower-Schematic-GC/Air-Shower-Schematic-GC.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/Auger-Animation.dc.xml This animation models how an extensive air shower (EAS) is detected by the Pierre Auger Cosmic Ray Observatory Engineering Array. The cosmic ray particles spread out to form a shower front. The shower front is illustrated using green dots to represent electrons and positrons, and red dots to represent muons. Yellow indicates that particles have been detected coincidentally by one of the water tank detectors. Slight differences in the detection times at the various tank positions allow scientists to determine the cosmic ray arrival direction. See the sketch of the cosmic ray creating an air shower and heading towards the detector on the previous page. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/Auger-Animation.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/sas3_layout/sas3_layout.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is a diagram of the instruments onboard the SAS-3. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/sas3_layout/sas3_layout.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/FNAL-Auger-Detector/FNAL-Auger-Detector.dc.xml The Pierre Auger Observatory has 1,600 water tanks arrayed throughout a 1,200-square mile area in western Argentina. Each of the 3,000-gallon tanks is a particle detector for capturing cosmic rays. The Auger Observatory uses both water tanks and optical detectors to measure the cosmic ray air showers. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/FNAL-Auger-Detector/FNAL-Auger-Detector.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/FNAL-Linsley-Volcano-Ranch/FNAL-Linsley-Volcano-Ranch.dc.xml (Left) John Linsley at Volcano Ranch. On February 22, 1962, Linsley observed an air shower created by a primary particle with an energy greater than 1020 eV, the highest energy cosmic ray observed up to that point. If a particle of this energy was created within the galaxy, it could not be contained in the galaxy. Linsley’s observations at Volcano Ranch suggested that not all cosmic rays are confined within the galaxy, as had been previously supposed. (Right) The plan of Volcano Ranch array in 1962, as it looked when Linsley made his observation. The circles represent 3.3 m2 scintillation detectors. Numbers near circles are shower densities (particles/m2) registered in the event. Point 'A' is the estimated location of the shower core. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/FNAL-Linsley-Volcano-Ranch/FNAL-Linsley-Volcano-Ranch.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/George-Clark-Harvard/George-Clark-Harvard.dc.xml George Clark’s graduation picture from Harvard University. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/George-Clark-Harvard/George-Clark-Harvard.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/MIT-Clark-Kraushaar-1956/MIT-Clark-Kraushaar-1956.dc.xml Professors William Kraushaar and George Clark close the air-tight cover on the balloon gondola that carried the second of their two (unsuccessful) balloon experiments in search for high-energy cosmic gamma rays. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/MIT-Clark-Kraushaar-1956/MIT-Clark-Kraushaar-1956.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/MIT-Rossi-BBR-45/MIT-Rossi-BBR-45.dc.xml Professor Bruno Rossi supervises as a student assembles equipment for a cosmic ray balloon experiment in 1948. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/MIT-Rossi-BBR-45/MIT-Rossi-BBR-45.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Explorer-11-Flight/NASA-Explorer-11-Flight.dc.xml Explorer 11, the first gamma-ray detection satellite flown, was launched on April 27, 1961. The satellite could not be actively pointed, so it was put into a tumble in order to get a "rough" scan of the entire celestial sphere.. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Explorer-11-Flight/NASA-Explorer-11-Flight.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Fermi-Map/NASA-Fermi-Map.dc.xml This all-sky image made in 2011 was constructed using two years of observations by NASA's Fermi Gamma-ray Space Telescope. It shows how the sky appears at energies greater than 1 billion electron volts (1 GeV). Brighter colors indicate brighter gamma-ray sources. A diffuse glow fills the sky and is brightest along the plane of our galaxy (middle). Discrete gamma-ray sources include pulsars and supernova remnants within our galaxy, as well as distant galaxies powered by supermassive black holes. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Fermi-Map/NASA-Fermi-Map.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-OSO-3-GC/NASA-OSO-3-GC.dc.xml Scale drawing of the OSO 3 detector. Inset is a picture of the satellite. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-OSO-3-GC/NASA-OSO-3-GC.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/SAS3-Rapid-Burster-GC/SAS3-Rapid-Burster-GC.dc.xml This image displays the light curve of the Rapid Burster discovered by Walter Lewin in data from SAS-3. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/SAS3-Rapid-Burster-GC/SAS3-Rapid-Burster-GC.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/SSP-1945-winners/SSP-1945-winners.dc.xml Winners of the 1945 Westinghouse Science Talent Search assemble with Vice-President Harry S. Truman. George Clark was among the top ten finalists who were selected as winners. He stands 6th from the left in the back row. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/SSP-1945-winners/SSP-1945-winners.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/chandra_labeled/chandra_labeled.dc.xml Renamed the Chandra X-ray Observatory after launch, this image shows the instruments onboard the observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/chandra_labeled/chandra_labeled.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_detector/explorer-11_detector.dc.xml Draushaar and Clark’s detector for Explorer 11 was designed to detect gamma rays above 50 MeV. The image on the left shows the detector. It measured 20 inches high, 10 inches in diameter, and weighed about 30 pounds. The image on the right is a diagram of the detector, which consisted of a sandwich crystal scintillator and a Lucite Cherenkov counter, surrounded by a plastic anticoincidence scintillator. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_detector/explorer-11_detector.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_grbd/explorer-11_grbd.dc.xml Kraushaar and Clark’s detector for Explorer 11 was designed to detect gamma rays above 50 MeV. The image on the left shows the detector. It measured 20 inches high, 10 inches in diameter, and weighed about 30 pounds. The image on the right is a diagram of the detector, which consisted of a sandwich crystal scintillator and a Lucite Cherenkov counter, surrounded by a plastic anticoincidence scintillator. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_grbd/explorer-11_grbd.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/heao2_diagram/heao2_diagram.dc.xml Renamed the Einstein Observatory after launch, the image on the left shows HEAO-2 during pre-flight testing. This image shows the placement of the instruments onboard the observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/heao2_diagram/heao2_diagram.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3/sas3.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is an artist’s conception of the satellite in orbit.. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3/sas3.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3_layout/sas3_layout.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is a diagram of the instruments onboard the SAS-3. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3_layout/sas3_layout.dc.xml Thu, 01 Jan 1970 12:00:00 GMT