http://www.rssboard.org/rss-specification 720 http://ecuip-xtf.lib.uchicago.edu/xtf/search?docsPerPage%3D100;f12-subject%3DInstrument Results for your query: docsPerPage=100;f12-subject=Instrument Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_config/GRIS_config.dc.xml Diagram illustrating the placement of the detectors and shields. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_config/GRIS_config.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Geiger_counter_patent/Geiger_counter_patent.dc.xml Friedman holds U.S. Patent No. 2,475,603, for an adaptation of the tube used in a Geiger-Mueller counter. His tube design increased the counter's sensitivity to weak radiation sources by lowering the background noise of the counter itself. Figure 1 (upper left) is a cut-away view of Friedman's counter tube mounted within a container, called a shield. Figure 2 (lower left) is a front-end view of the tube. Figure 3 (upper right) is a cross-section of the tube showing the arrangement of parts and the structure used for mounting the tube within the shield. Figure 4 (lower right) is a cross-section diagram showing the tube anode and cathode, and a plot of the electric field within the tube. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Geiger_counter_patent/Geiger_counter_patent.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/aristotle-solar-system/aristotle-solar-system.dc.xml Illustration of Oronce Fine, Astronomy personified and an armillary sphere. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/aristotle-solar-system/aristotle-solar-system.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/harvard-acis-chandra/harvard-acis-chandra.dc.xml The Advanced CCD Imaging Spectrometer is an instrument on the Chandra X-Ray Observatory that consists of an array of charged coupled devices. ACIS is especially useful because it can make X-ray images, and at the same time, measure the energy of each incoming X-ray, so that scientists can make pictures of objects using only X-rays produced by a single chemical element. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/harvard-acis-chandra/harvard-acis-chandra.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_Ge_detectors/GRIS_Ge_detectors.dc.xml GRIS consists of seven of the world's largest, high-purity, n-type germanium (Ge) detectors. The detectors are cooled to liquid nitrogen temperatures (in order to achieve high resolution) and are surrounded by a thick anti-coincidence shield which allows the rejection of background events from true astrophysical events. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_Ge_detectors/GRIS_Ge_detectors.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/NASA-Microshutter/NASA-Microshutter.dc.xml The James Webb Space Telescope's (JWST) Near-infrared Spectrograph will use microshutters that act like tiny doorways to block unwanted light from nearby objects in space, while allowing light from very distant stars and galaxies to shine through. The microshutters are assembled as an array about the size of a postage stamp. Each array contains over 62,000 shutters. Individually, each microshutter measures 100 by 200 microns, or about the width of a human hair. The telescope will contain four of these microshutter arrays. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Microshutter/NASA-Microshutter.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Microshutter-NIRSPEC/NASA-Microshutter.dc.xml Many of the objects that JWST will study, such as the first galaxies to form after the Big Bang, are so faint, that its giant mirror must stare at them for hundreds of hours in order to collect enough light to form a spectrum. In order to study thousands of galaxies during its 5 year mission, the NIRSpec is designed to observe 100 objects simultaneously. The NIRSpec will be the first spectrograph in space that has this multi-object capability. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Microshutter-NIRSPEC/NASA-Microshutter.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Nested-Paraboloid/Nested-Paraboloid.dc.xml This cutaway illustrates the grazing-incidence design and functioning of the High Resolution Mirror Assembly (HRMA) on the Chandra X-ray Observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Nested-Paraboloid/Nested-Paraboloid.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