http://www.rssboard.org/rss-specification 720 http://ecuip-xtf.lib.uchicago.edu/xtf/search?f4-type%3DArtwork;f5-associated-Lesson%3DX-Ray%20Science Results for your query: f4-type=Artwork;f5-associated-Lesson=X-Ray Science 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/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/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/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