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''[[:en:List of cosmic microwave background experiments]]'''
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[[Image:BigBangNoise.jpg|thumb|right|300px|A comparison of the sensitivity of WMAP with COBE and Penzias and Wilson's telescope. Simulated data.]]
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There have been a variety of [[experiment]]s to measure the [[Cosmic microwave background radiation|Cosmic microwave background (CMB) radiation]] anisotropies and polarization since its first observation in 1964 by [[Arno Allan Penzias|Penzias]] and [[Robert Woodrow Wilson|Wilson]]. These include a mix of ground-, balloon- and space-based receivers. The most notable of these are [[COBE]], which first detected the temperature anisotropies of the CMB, and showed that it had a black body spectrum; [[DASI]], which first detected the polarization signal from the CMB; [[Cosmic Background Imager|CBI]] that made high-resolution observations and obtained the first E-mode polarization spectrum and [[WMAP]], which has provided the best full-sky CMB maps to date. Planned future experiments include the [[Planck (spacecraft)|Planck spacecraft]], which aims to produce high-resolution all-sky maps of both the temperature anisotropies and polarization signals, and various ground-based experiments primarily intended to investigate small-scale anisotropies and trying to detect the polarization caused by [[gravitational wave]]s in the early [[universe]].
 
The design of cosmic microwave background experiments is a very challenging task. The greatest problems are the receivers, the telescope optics and the atmosphere. Many improved microwave amplifier technologies have been designed for microwave background applications. Some technologies used are [[HEMT]], [[Monolithic Microwave Integrated Circuit|MMIC]], [[Superconductor-Insulator-Superconductor|SIS]] and [[bolometer]]s. Experiments generally use elaborate [[cryogenics|cryogenic]] systems to keep the amplifiers cool. Often, experiments are [[interferometer]]s which only measure the spatial fluctuations in signals on the sky, and are insensitive to the average 2.7&nbsp;K background.
 
Another problem is the [[1/f noise|1/''f'' noise]] intrinsic to all detectors. Usually the experimental scan strategy is designed to minimize the effect of such noise. To minimize [[side lobe]]s, microwave optics usually utilize elaborate [[Lens (optics)|lenses]] and [[feed horn]]s. Finally, the atmosphere is an issue because water absorbs microwave radiation (a fact utilized in the operation of [[microwave oven]]s), it is rather difficult to observe the microwave background with ground-based instruments. CMB research therefore makes increasing use of air and space-borne experiments. Ground-based observations are usually made from dry, high altitude locations such as the [[Andes|Chilean Andes]] and the [[South Pole]].
 
The list below consists of a partial list of past, current and planned CMB experiments. The name, start and end years of each experiment are given, followed by the basis of the experiment—whether space, balloon or ground based—and the ___location where appropriate. The frequency and amplifier technologies used are given, as is the main targets of the experiments.
 
{| class="wikitable sortable"
|-
! style="width: 10%;" class="unsortable" | Image
! style="width: 30%;" | Name
! style="width: 5%;" | Start
! style="width: 5%;" | End
! style="width: 5%;" | Basis
! style="width: 10%;" | Location
! style="width: 5%;" | Frequency (GHz)
! style="width: 10%;" | Amplifier technology
! style="width: 12%;" class="unsortable" | Targets
! style="width: 3%;" class="unsortable" | Ref(s)
|-
|
| [[Advanced Cosmic Microwave Explorer]] (ACME)<br />Also HACME: [[HEMT]]+ACME
| style="text-align: center;" | 1988
| style="text-align: center;" | 1996
| Ground
|
| 26–35; 38–45
| HEMT
| Temperature anisotropies
| <ref name="nasa_lambda">{{cite web | url=http://lambda.gsfc.nasa.gov/links/experimental_sites.cfm | title=LAMBDA&nbsp;— CMB Experiment Sites | date=18 April 2008 | accessdate=2008-10-19}}</ref>
|-
|
| [[Antarctic Plateau Anisotropy Chasing Experiment]] (APACHE)
| style="text-align: center;" | 1995
| style="text-align: center;" | 1996
| Ground
| [[Antarctic]]
| 100, 150, 250
| Bolometer
| Temperature anisotropies
| <ref name="nasa_lambda" />
|-
|
| [[Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission]] (ARCADE)
| style="text-align: center;" | 2001
| style="text-align: center;" | —
| Balloon
|
| 3, 5, 7, 10, 30, 90
| HEMT
| CMB Spectrum
| <ref name="nasa_lambda" />
|-
| [[Image:Archeops gondola at launch.jpg|100px|Archeops]]
| [[Archeops]]
| style="text-align: center;" | 1999
| style="text-align: center;" | 2002
| Balloon
|
| 143, 217, 353, 545
| Bolometer
| Measured large and intermediate scale with improved precision at the larger scales.
| <ref name="nasa_lambda" />
|-
|
| [[Arcminute Cosmology Bolometer Array Receiver]] (ACBAR)
| style="text-align: center;" | 2001
| style="text-align: center;" | —
| Ground
|
| 150, 219, 274
| Bolometer
| Temperature anisotropies
| <ref name="nasa_lambda" />
|-
| [[Image:Mrao ami lba ryle.jpg|100px|AMI]]
| [[Arcminute Microkelvin Imager]] (AMI)
| style="text-align: center;" | 2005<!--check this-->
| style="text-align: center;" | —
| Ground
| [[UK]]: [[Mullard Radio Astronomy Observatory]]
| 12-18
| Interferometer
| [[SZ effect]], Temperature anisotropies
| <ref name="nasa_lambda" />
|-
|
| [[ARGO]]
| style="text-align: center;" | 1988, 1990, 1993
| style="text-align: center;" | 1993
| Balloon
|
| 150-600
| Bolometer
|
| <ref name="nasa_lambda" />
|-
| [[Image:AMiBA 1.jpg|100px|AMiBA]]
| [[Array for Microwave Background Anisotropy]] (AMiBA)
| style="text-align: center;" | 2002
| style="text-align: center;" | —
| Ground
| Hawaii: [[Mauna Loa]]
| 86-102
| MMIC
| SZ effect; Polarization
| <ref name="nasa_lambda" /><ref name="Ho08">{{cite journal | first=Paul | last=Ho | coauthors=et al. | year=2008 | title=The Yuan-Tseh Lee Array for Microwave Background Anisotropy | id={{arxiv|0810.1871}} }}</ref><ref name="Wu08">{{cite journal | first=Jiun-Huei Proty | last=Wu | coauthors=et al. | title = AMiBA Observations, Data Analysis and Results for Sunyaev-Zel'dovich Effects | year=2008 | id={{arxiv|0810.1015}} }}</ref>
|-
| [[Image:Atacama cosmology telescope night.jpg|100px|ACT]]
| [[Atacama Cosmology Telescope]] (ACT)
| style="text-align: center;" | 2007<!--check this-->
| style="text-align: center;" | —
| Ground
| [[Chile]]: [[Atacama Desert]]
| 145, 225, 265
| Bolometer
| Temperature anisotropies
| <ref name="nasa_lambda" />
|-
| [[Image:Phot-24a-06.jpg|100px|APEX]]
| [[Atacama Pathfinder Experiment]] (APEX)
| style="text-align: center;" | 2005<!--check this-->
| style="text-align: center;" | —
| Ground
|
| 150, 217
| Bolometer
| Temperature anisotropies; SZ effect
| <ref name="nasa_lambda" />
|-
| [[Image:ATCA Radio Telescope Narrabri 2005 12 21.jpg|100px|ATCA]]
| [[Australia Telescope Compact Array]] (ATCA)
| style="text-align: center;" | 1991
| style="text-align: center;" | 1997
| Ground
|
| 8.7
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Background Emission Anisotropy Scanning Telescope]] (BEAST)
| style="text-align: center;" | 2000
| style="text-align: center;" | —
| Balloon, Ground
|
| 25-35; 38-45
| HEMT
| A ground single dish CMB observatory at the University of California's [[White Mountain Peak]] Research station.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Background Imaging of Cosmic Extragalactic Polarization]] (BICEP)
| style="text-align: center;" | 2006
| style="text-align: center;" | 2008
| Ground
| [[South Pole]]<!--check this-->
| 100, 150
| Bolometer
| Will measure large scale polarization with improved precision.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Balloon-borne Anisotropy Measurement]] (BAM)
| style="text-align: center;" | 1995
| style="text-align: center;" | 1998
| Balloon
| UBC Balloon Expt<!--check this-->
| 110-250
| Spectrometer
| Used differential Fourier Transform Spectrometer to measure degree scale anisotropy<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Balloon-borne Radiometers for Sky Polarisation Observations]] (BaR-SPoRT)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Balloon
|
| 32, 90
| Polarizer / OMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Berkeley-Illinois-Maryland Association]] ([[BIMA]])
| style="text-align: center;" | 1986
| style="text-align: center;" | 2004
| Ground
|
| 70-116; 210-270
| SIS
|
| <ref name="nasa_lambda" />
|-
| [[Image:Boomerang Telescope.jpeg|100px|BOOMERanG]]
| [[BOOMERanG experiment]]
| style="text-align: center;" | 1997
| style="text-align: center;" | 2003<!--check this-->
| Balloon
| Long-duration balloon above Antarctica<!--check this-->
| 90-420
| Bolometer
| Measured intermediate scale fluctuations with improved precision.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[BRAIN|B-mode RAdiation INterferometer]] (BRAIN)
| style="text-align: center;" | Never
| style="text-align: center;" | —
| Ground
| Dome-C, Antarctica
|
|
|
| <!--check this-->
|-
|
| [[Clover (telescope)|Clover]]
| style="text-align: center;" | Never
| style="text-align: center;" | —
| Ground
|
| 97, 150, 230
| Bolometer
| Will measure the small scale fluctuations with improved precision, and the B-mode polarization.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Cosmic Anisotropy Polarization Mapper]] (CAPMAP)
| style="text-align: center;" | 2002
| style="text-align: center;" | —
| Ground
|
| 40, 90
| MMIC/HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Cosmic Anisotropy Telescope]] (CAT)
| style="text-align: center;" | 1994
| style="text-align: center;" | 1997
| Ground
| [[Mullard Radio Astronomy Observatory]]
| 13-17
| Interferometer / HEMT
| Measured the very small scale fluctuations in small regions of the sky.
| <ref name="nasa_lambda" />
|-
| [[Image:Cosmic Background Imager.jpeg|100px|CBI]]
| [[Cosmic Background Imager]] (CBI)
| style="text-align: center;" | 2002
| style="text-align: center;" | 2008<!--check this-->
| Ground
| [[Llano de Chajnantor Observatory]], Chile
| 26-36
| HEMT
| Measured the very small scale fluctuations with improved precision in small regions of the sky and polarization of CMB.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[COSMOSOMAS]]
| style="text-align: center;" | 1998
| style="text-align: center;" | —
| Ground
| [[Teide Observatory]], Tenerife, Spain
| 10-18
| HEMT
| Circular scanning experiments for CMB and foregrounds in Tenerife.
| <ref name="nasa_lambda" />
|-
| [[Image:Cobe vision1.jpg|100px|COBE]]
| [[Cosmic Background Explorer]] (COBE)
| style="text-align: center;" | 1989
| style="text-align: center;" | 1993
| Space
| [[Earth orbit]]
|
|
| Temperature anisotropies
| <ref name="nasa_lambda" />
|-
|
| [[Cosmological Gene]]
| style="text-align: center;" | 1999
| style="text-align: center;" | —
| Ground
|
| 0.6 to 32
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Degree Angular Scale Interferometer]] (DASI)
| style="text-align: center;" | 1999
| style="text-align: center;" | 2003
| Ground
|
| 26-36
| HEMT
| A temperature and polarization telescope at the South Pole.
| <ref name="nasa_lambda" />
|-
|
| [[The E and B Experiment]] (EBEX)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Balloon
| Antarctica
| 150-450
| Bolometer
| Detection of the inflationary gravitational-wave background (IGB) signal is a primary goal of the EBEX experiment
| <ref name="nasa_lambda" />
|-
|
| [[Far Infra-Red Survey]] (FIRS)
| style="text-align: center;" | 1989
| style="text-align: center;" | 1989
| Balloon
|
| 170-680
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[KU-band Polarization IDentifier]] (KUPID)
| style="text-align: center;" | 2003
| style="text-align: center;" | —
| Ground
|
| 12-18
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Medium Scale Anisotropy Measurement]] (MSAM)
| style="text-align: center;" | 1992
| style="text-align: center;" | 1997
| Balloon
|
| 150-650
| Bolometer
|
| <ref name="nasa_lambda" />
|-
| [[Image:MAXIMA Balloon.jpg|100px|MAXIMA]]
| [[Millimeter Anisotropy eXperiment IMaging Array]] (MAXIMA)
| style="text-align: center;" | 1995, 1998, 1999
| style="text-align: center;" | 1999
| Balloon
| Near Palestine, Texas<!--check this-->
| 150-420
| Bolometer
| Measured intermediate scale fluctuations with improved precision.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Millimeter Interferometer]] (MINT)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Ground
|
| 150
| SIS
|
| <ref name="nasa_lambda" />
|-
|
| [[Millimeter-Wave Bolometric Interferometer]] (MBI-B)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Ground
|
| 90
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[Mobile Anisotropy Telescope]] (MAT)
| style="text-align: center;" | 1997, 1998
| style="text-align: center;" | 1998
| Ground
|
| 30-140
| HEMT / SIS
|
| <ref name="nasa_lambda" />
|-
| [[Image:Planck satellite.jpg|100px|Planck]]
| [[Planck (spacecraft)|Planck]]
| style="text-align: center;" | 2009
| style="text-align: center;" | —
| Space
| [[Lagrange 2]]
| 30-857
| HEMT / Bolometer
| Polarization; Temperature anisotropies; Foregrounds
| <ref name="nasa_lambda" />
|-
|
| [[Polarization Observations of Large Angular Regions]] (POLAR)
| style="text-align: center;" | 2000
| style="text-align: center;" | 2000
| Ground
|
| 26-46
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Polarization of Background Microwave Radiation]] (POLARBeaR)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Ground
|
| 90-240
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[Polatron]]
| style="text-align: center;" | Never
| style="text-align: center;" | —
| Ground
|
| 100
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[Princeton I, Q, and U Experiment]] (PIQUE)
| style="text-align: center;" | 2002
| style="text-align: center;" | 2002
| Balloon
|
| 90
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| Python
| style="text-align: center;" | 1992
| style="text-align: center;" | 1997
| Ground
|
| 30-90
| HEMT / Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[QMAP]]
| style="text-align: center;" | 1996
| style="text-align: center;" | 1996
| Ground
|
| 30-140
| HEMT / SIS
|
| <ref name="nasa_lambda" />
|-
| [[Image:050128quad-from-crane.jpg|100px|QUaD]]
| [[QUaD]]
| style="text-align: center;" | 2005
| style="text-align: center;" | 2007
| Ground
| [[South Pole]]
| 100, 150
| Bolometer
| Measured intermediate scale polarization with improved precision.<!--check this-->
| <ref name="nasa_lambda" />
|-
|
| [[Qubic experiment|Qubic]]
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Ground
|
| 97, 150, 230
| Bolometer
| Will measure the B-mode polarization on intermediate scale.
|
|-
|<!-- Image with inadequate rationale removed: [[Image:QUIET telescope illustration.jpg|100px|QUIET]] -->
| [[QUIET|Q/U Imaging ExperimenT]] (QUIET)
| style="text-align: center;" | 2008
| style="text-align: center;" | —
| Ground
| [[Llano de Chajnantor Observatory]], Chile<!--check this-->
| 40, 90
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[RELIKT-1]]
| style="text-align: center;" | 1983
| style="text-align: center;" | 1984
| Space
| [[Earth orbit]]
|
|
| Temperature anisotropies
| <ref name="nasa_lambda" />
|-
|
| [[Saskatoon experiment]]
| style="text-align: center;" | 1993
| style="text-align: center;" | 1995
| Ground
| [[Saskatchewan]]
| 26-46
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[Sky Polarization Observatory]] (SPOrt)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Space
| [[International Space Station]]
|
|
| Polarization
| <ref name="nasa_lambda" />
|-
| [[Image:South Pole Telescope (2008).JPG|100px|South Pole Telescope]]
| [[South Pole Telescope]]
| style="text-align: center;" | 2006<!--check this-->
| style="text-align: center;" |
| Ground
| [[South Pole]]
|
|
| Will measure the small scale fluctuations and polarization.
| <ref name="nasa_lambda" />
|-
|
| [[Spider CMB|SPIDER]]
| style="text-align: center;" | 2011
| style="text-align: center;" |
| Balloon
|
| 90, 150, 220
| Bolometer
| Will measure very large scale polarization.
| <!--check this-->
|-
| [[Image:Sza.gif|100px|SZA]]
| [[Sunyaev-Zeldovich Array]] (SZA)
| style="text-align: center;" | Future
| style="text-align: center;" | —
| Ground
|
| 26-36; 85-115
| Interferometer
| SZ effect
| <ref name="nasa_lambda" />
|-
|
| [[Sunyaev-Zeldovich Infrared Experiment]] (SuZIE)
| style="text-align: center;" | 1996
| style="text-align: center;" | —
| Ground
|
| 150, 220, 350
| Bolometer
| SZ effect
| <ref name="nasa_lambda" />
|-
|
| [[Tenerife Experiment]]
| style="text-align: center;" | 1984
| style="text-align: center;" | 2000
| Ground
| [[Tenerife]]
| 10, 15, 33
| HEMT
|
| <ref name="nasa_lambda" />
|-
|
| [[TopHat (Balloon)|TopHat]]
| style="text-align: center;" | 2002
| style="text-align: center;" | —
| Balloon
|
| 150-720
| Bolometer
|
| <ref name="nasa_lambda" />
|-
|
| [[Very Small Array]]
| style="text-align: center;" | 2002
| style="text-align: center;" | 2008
| Ground
|
| 26-36
| Interferometer / HEMT
| Measured intermediate and small scale fluctuations with improved precision in small regions of the sky.
| <ref name="nasa_lambda" />
|-
| [[Image:WMAP collage.jpg|100px|WMAP]]
| [[Wilkinson Microwave Anisotropy Probe]] (WMAP)
| style="text-align: center;" | 2001
| style="text-align: center;" | —
| Space
| [[Lagrange 2]]
| 23-94
| HEMT
| Temperature anisotropies; Polarization
| <ref name="nasa_lambda" />
|}
 
== References ==
{{Reflist}}
 
{{CMB experiments}}
 
{{DEFAULTSORT:List Of Cosmic Microwave Background Experiments}}
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