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{{About|the astronomy experiment||Quiet (disambiguation){{!}}Quiet}}
{{Infobox Telescope
|name        = QUIET
|image        = [[Image:QUIET telescope illustration.jpg|150px]]
|caption      = An illustration of the completed QUIET telescope on the CBI platform.
|organization = International collaboration
|location    = [[Llano de Chajnantor Observatory]]
|coords      =
|altitude    = 5,080 m
|weather      =
|wavelength  = 40 and 90 GHz
|built        =
|first_light  =
|website      = [http://quiet.uchicago.edu/ quiet.uchicago.edu]
|style        = 4 telescopes
|diameter    = Three 2 m, one 7 m
|angular_resolution = Few arcminutes to several degrees
|area        =
|focal_length =
|mounting    =
|dome        =
}}


'''QUIET''' is an [[astronomy]] [[experiment]] to study the polarization of the [[cosmic microwave background radiation]].<ref name="quiet_homepage" /> QUIET stands for '''Q/U Imaging ExperimenT'''. The Q/U in the name refers to the ability of the telescope to measure the Q and U [[Stokes parameters]] simultaneously.  QUIET is located at an elevation of 5,080 [[metre]]s (16,700 feet) at [[Llano de Chajnantor Observatory]] in the [[Chile]]an [[Andes]].<ref name="quiet_site" /> It began observing in late 2008 and finished observing in December 2010.<ref>{{cite arXiv | eprint=1012.3191 | version=v2 | title=First Season QUIET Observations: Measurements of CMB Polarization Power Spectra at 43 GHz in the Multipole Range 25 <= ell <= 475 | author1=QUIET Collaboration | author2=Bischoff | author3=Brizius | author4=Buder | author5=Chinone | author6=Cleary | author7=Dumoulin | author8=Kusaka | author9=Monsalve | class=astro-ph.CO | year=2010}}</ref>


QUIET is the result of an international collaboration that has its origins in the [[Cosmic Anisotropy Polarization Mapper|CAPMAP]], [[Cosmic Background Imager]] (CBI) and [[QUaD]] collaborations. The collaboration consists 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 Institute for Radio Astronomy|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). Other members of the collaboration are from the [[University of California, Berkeley]], the [[Goddard Space Flight Center]] and the [[Harvard-Smithsonian Center for Astrophysics]].<ref name="quiet_homepage">{{Cite web| url=http://quiet.uchicago.edu/ | title=QUIET (Q/U Imaging ExperimenT) | publisher=QUIET collaboration | date=17 February 2008 | accessdate=2008-05-24}}</ref>
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==Instrument==
QUIET will have arrays of detectors at two frequencies: 40&nbsp;[[GHz]] ([[Q band]]) and 90&nbsp;GHz ([[W band]]). It will use four telescopes, three of which will be purpose-built 2&nbsp;m ones with the other being the 7&nbsp;m Crawford Hill telescope currently used for [[CAPMAP]]. As a result, it will have [[angular resolution]]s between a few arcminutes and several degrees. The detectors are mass-produced [[Coherence (physics)|coherent]] [[correlation]] [[polarimeter]]s.<ref name="quiet_homepage" /><ref name="quiet_science" />
 
The instrument is being constructed in three phases. The first phase consisted of a 7-element 90&nbsp;GHz array to demonstrate the technology. The second phase aims to mount a 91-element 90&nbsp;GHz array (with 18&nbsp;GHz [[Bandwidth (signal processing)|bandwidth]]) and a 19-element 40&nbsp;GHz array (with 8&nbsp;GHz bandwidth) on 1.4&nbsp;m [[Cassegrain reflector|cassegrain]] telescopes, mounted on what is currently the [[Cosmic Background Imager|CBI]] platform. It is expected that these will start observing in 2008. The third phase aims to construct four further arrays by around 2010. Two of these will be at 40&nbsp;GHz, with 91 elements each, and the other two will be at 90&nbsp;GHz, with 397 elements each. These will then be mounted on three 2&nbsp;m dishes on the CBI platform and the 7&nbsp;m telescope.<ref name="2008Samtleben">Samtleben (2008)</ref><ref name="quiet_instrumentation">{{Cite web| url=http://quiet.uchicago.edu/instrumentation/index.html | title=QUIET: Instrumentation | publisher=QUIET collaboration | date=27 January 2008 | accessdate=2008-05-24}}</ref>
 
The instrument is located at a height of 5,080&nbsp;m at Llano de Chajnantor Observatory in the [[Chile]]an [[Andes]]. The site is owned by the Chilean government, and is leased to the [[Atacama Large Millimeter Array]]. 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.<ref name="quiet_site">{{Cite web| url=http://quiet.uchicago.edu/site/index.html | title=QUIET: Site | publisher=QUIET collaboration | date=27 January 2008 | accessdate=2008-05-24}}</ref>
 
==Science==
[[Image:Quiet Telescope.JPG|thumb|alt=A photograph of the QUIET telescope|The QUIET [[telescope]] with its ground screen raised]]
QUIET will measure the polarization of the [[cosmic microwave background radiation]] (CMB). This polarization is commonly split into two components: E-modes, which represent the gradient component, and B-modes, which give the curl component. It is thought that B-modes are formed both from primordial fluctuations due to [[cosmic inflation]], and from [[gravitational lens]]ing of the CMB. As of 2008, only E-modes have been detected. 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.<ref name="quiet_science">{{Cite web| url=http://quiet.uchicago.edu/science/index.html | title=QUIET: Science | publisher=QUIET collaboration | date=27 January 2008 | accessdate=2008-05-24}}</ref>
 
B-modes are thought to be much fainter than E-modes, as they are formed by higher order effects. 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. For QUIET this value is r=0.009, which corresponds to the [[energy scale]] of [[cosmic inflation]] being around <math>10^{16}</math>&nbsp;[[GeV]].<ref name="quiet_science" />
 
QUIET's measurements of the CMB's [[power spectrum]] will be between the [[multipole]]s of about 40 and 2,500, and will be made in a section of the sky known to have low foreground contamination.<ref name="quiet_science" />
 
==Status==
As of March 2011, the QUIET team described the status<blockquote>
Observations were made from October 2008 through May 2009 using a 19-element 40 GHz instrument coupled to a 1.4 meter telescope located at the Llano de Chajnantor Observatory in Chile. Observations with a 91-element 90 GHz instrument on the same telescope finished in December 2010. The QUIET instrument has been dismantled from the old CBI mount.
</blockquote>
 
==References==
{{Reflist|1}}
 
===Journal article===
<div class="references-small">
* {{Cite journal| last=Samtleben | first=Dorothea | coauthors=QUIET collaboration | year=2008 | title=Measuring the Cosmic Microwave Background Radiation (CMBR) polarization with QUIET | arxiv=0802.2657 |bibcode = 2008arXiv0802.2657S }}
</div>
 
{{CMB experiments}}
{{Astronomical observatories in Chile}}
 
{{Coord missing|Chile}}
{{Use dmy dates|date=September 2010}}
 
{{DEFAULTSORT:Quiet}}
[[Category:Cosmic microwave background experiments]]
[[Category:Astronomical observatories in Chile]]
[[Category:Buildings and structures in Antofagasta Region]]
[[Category:Science and technology in Chile]]

Latest revision as of 12:40, 20 December 2014


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