The definiton of a quiet storm
For QUIET this value is r=0.009, which corresponds to the energy scale of cosmic inflation being around 10 16 GeV. The ratio of the E-mode to B-mode polarization is currently unknown, and the minimum detectable value of this can be used as a measure of the sensitivity of a CMB instrument. ī-modes are thought to be much fainter than E-modes, as they are formed by higher order effects. QUIET aims to detect and characterize the B-modes polarization for the first time, and to provide more accurate measurements of the E-mode polarization. As of 2008, only E-modes have been detected. It is thought that B-modes are formed both from primordial fluctuations due to cosmic inflation, and from gravitational lensing of the CMB. This polarization is commonly split into two components: E-modes, which represent the gradient component, and B-modes, which give the curl component. QUIET measured the polarization of the cosmic microwave background radiation (CMB). The site was selected due to the altitude, current infrastructure and accessibility, as well as the low humidity of the site, which reduces the contamination of the detected signals by the atmosphere. The site is owned by the Chilean government, and is leased to the Atacama Large Millimeter Array. The instrument is located at a height of 5,080 m at Llano de Chajnantor Observatory in the Chilean Andes. These will then be mounted on three 2 m dishes on the CBI platform and the 7 m telescope. Two of these will be at 43 GHz, with 91 elements each, and the other two will be at 95 GHz, with 397 elements each. The third phase aims to construct four further arrays by around 2010. It is expected that these will start observing in 2008. The second phase aims to mount a 91-element 95 GHz array (with 18 GHz bandwidth) and a 19-element 43 GHz array (with 8 GHz bandwidth) on 1.4 m cassegrain telescopes, mounted on what is currently the CBI platform. The first phase consisted of a 7-element 95 GHz array to demonstrate the technology. The instrument was constructed in three phases. The detectors are mass-produced coherent correlation polarimeters. As a result, it will have angular resolutions between a few arcminutes and several degrees. It used four telescopes, three of which were purpose-built 2 m ones with the other being the 7 m Crawford Hill telescope used for CAPMAP.
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QUIET had arrays of detectors at two frequencies: 43 GHz ( Q band) and 95 GHz ( W band).
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Other members of the collaboration are from the University of California, Berkeley, the Goddard Space Flight Center and the Harvard-Smithsonian Center for Astrophysics. The collaboration consisted of 7 groups in the United States (the California Institute of Technology, the University of Chicago, Columbia University, the Jet Propulsion Laboratory, the University of Miami, Princeton University and Stanford University), 4 groups in Europe (the University of Manchester, the Max-Planck-Institut für Radioastronomie Bonn, the University of Oslo and the University of Oxford) and one group in Japan ( KEK the first time a Japan group has been involved in CMB studies). QUIET iwas the result of an international collaboration that had its origins in the CAPMAP, Cosmic Background Imager (CBI) and QUaD collaborations. It began observing in late 2008 and finished observing in December 2010. QUIET was located at an elevation of 5,080 metres (16,700 feet) at Llano de Chajnantor Observatory in the Chilean Andes. The Q/U in the name refers to the ability of the telescope to measure the Q and U Stokes parameters simultaneously.
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QUIET was an astronomy experiment to study the polarization of the cosmic microwave background radiation.