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en:List of cosmic microwave background experiments

A comparison of the sensitivity of WMAP with COBE and Penzias and Wilson's telescope. Simulated data.

There have been a variety of experiments to measure the Cosmic microwave background (CMB) radiation anisotropies and polarization since its first observation in 1964 by Penzias and 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; 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, 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 waves 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, MMIC, SIS and bolometers. Experiments generally use elaborate cryogenic systems to keep the amplifiers cool. Often, experiments are interferometers which only measure the spatial fluctuations in signals on the sky, and are insensitive to the average 2.7 K background.

Another problem is the 1/f noise intrinsic to all detectors. Usually the experimental scan strategy is designed to minimize the effect of such noise. To minimize side lobes, microwave optics usually utilize elaborate lenses and feed horns. Finally, the atmosphere is an issue because water absorbs microwave radiation (a fact utilized in the operation of microwave ovens), 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 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.

Tabella

Immagine	Nome	Inizio	Fine	Tipo esperimento	Localizzazione	Frequenza (GHz)	Tipo di amplificazione	Obiettivi	Note
	Advanced Cosmic Microwave Explorer (ACME) HACME: HEMT+ACME	1988	1996	Terra		26–35; 38–45	HEMT	Anisotropie temperatura CMB	[1]
	Antarctic Plateau Anisotropy Chasing Experiment (APACHE)	1995	1996	Terra	Antartide	100, 150, 250	Bolometro	Anisotropie temperatura CMB	[1]
	Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE)	2001	—	Pallone		3, 5, 7, 10, 30, 90	HEMT	Spettro CMB	[1]
	Archeops	1999	2002	Pallone		143, 217, 353, 545	Bolometro	Misura delle anisotropie di temperatura della CMB	[1]
	Arcminute Cosmology Bolometer Array Receiver (ACBAR)	2001	—	Terra		150, 219, 274	Bolometro	Misura delle anisotropie di temperatura della CMB	[1]
	Arcminute Microkelvin Imager (AMI)	2005	—	Terra	Regno Unito: Mullard Radio Astronomy Observatory	12-18	Interferometro	Effetto Sunyaev-Zel'dovich, Misura delle anisotropie di temperatura della CMB	[1]
	ARGO	1988, 1990, 1993	1993	Pallone		150-600	Bolometro		[1]
	Array for Microwave Background Anisotropy (AMiBA)	2002	—	Terra	Hawaii: Mauna Loa	86-102	MMIC	Effetto Sunyaev-Zel'dovich; polarizzazione	[1][2][3]
	Atacama Cosmology Telescope (ACT)	2007	—	Terra	Cile: Deserto di Atacama	145, 225, 265	Bolometro	Misura delle anisotropie di temperatura della CMB	[1]
	Atacama Pathfinder Experiment (APEX)	2005	—	Terra		150, 217	Bolometro	Misura delle anisotropie di temperatura della CMB; effetto Sunyaev-Zel'dovich	[1]
	Australia Telescope Compact Array (ATCA)	1991	1997	Terra		8.7	HEMT		[1]
	Background Emission Anisotropy Scanning Telescope (BEAST)	2000	—	Pallone, terra		25-35; 38-45	HEMT	Osservatorio presso la stazione di ricerca dell'Univeristà della California, stazione di ricerca White Mountain Peak	[1]
	Background Imaging of Cosmic Extragalactic Polarization (BICEP)	2006	2008	Terra	Polo Sud	100, 150	Bolometro	Misurarazione polarizzazione su larga scala con maggiore precisione	[1]
	Balloon-borne Anisotropy Measurement (BAM)	1995	1998	Pallone	Pallone UBC	110-250	Spettrometro		[1]
	Balloon-borne Radiometers for Sky Polarisation Observations (BaR-SPoRT)	Future	—	Pallone		32, 90	Polarizzatore / OMT		[1]
	Berkeley-Illinois-Maryland Association (BIMA)	1986	2004	Terra		70-116; 210-270	SIS		[1]
	Esperimento BOOMERanG	1997	2003	Pallone	Antartide	90-420	Bolometro	Misura delle anisotropie di temperatura della CMB con precisione migliorata	[1]
	B-mode RAdiation INterferometer (BRAIN)	-	—	Terra	Dome C, Antartide
	Clover	-	—	Terra		97, 150, 230	Bolometro	Misura delle fluttuazioni su piccola scala a precisione migliorata, e la polarizzazione B-mode	[1]
	Cosmic Anisotropy Polarization Mapper (CAPMAP)	2002	—	Terra		40, 90	MMIC/HEMT		[1]
	Cosmic Anisotropy Telescope (CAT)	1994	1997	Terra	Mullard Radio Astronomy Observatory	13-17	Interferometro / HEMT	Misura delle fluttuazioni a scala piccolissima in regioni piccole dell'universo	[1]
	Telescopio CBI (CBI)	2002	2008	Terra	Llano de Chajnantor Observatory, Cile	26-36	HEMT	Misura delle fluttuazioni a scala piccolissima in regioni piccole dell'universo con precisione maggiore, e la polarizzazione della CMB	[1]
	COSMOSOMAS	1998	—	Terra	Osservatorio del Teide, Tenerife, Spagna	10-18	HEMT	Esperimenti a scansione circolare per la CMB	[1]
	Cosmic Background Explorer (COBE)	1989	1993	Space	Orbita geocentrica			Misura delle anisotropie di temperatura della CMB	[1]
	Cosmological Gene	1999	—	Terra		da 0.6 a 32	HEMT		[1]
	Degree Angular Scale Interferometer (DASI)	1999	2003	Terra		26-36	HEMT	Temperatura e polarizzazione al Polo Sud	[1]
	E and B Experiment (EBEX)	In futuro	—	Pallone	Antartide	150-450	Bolometro	Immagine larga e ad altà fedeltà delle anisotropie di polarizzazione della CMB e rilevazione delle onde gravitazionali inflazionarie di fondo	[1]
	Far Infra-Red Survey (FIRS)	1989	1989	Pallone		170-680	Bolometro		[1]
	KU-band Polarization IDentifier (KUPID)	2003	—	Terra		12-18	HEMT		[1]
	Medium Scale Anisotropy Measurement (MSAM)	1992	1997	Pallone		150-650	Bolometro		[1]
	Millimeter Anisotropy eXperiment IMaging Array (MAXIMA)	1995, 1998, 1999	1999	Pallone	Palestine, Texas	150-420	Bolometro	Misura delle fluttuazioni su scala media con precisione migliorata	[1]
	Millimeter Interferometer (MINT)	In futuro	—	Terra		150	SIS		[1]
	Millimeter-Wave Bolometric Interferometer (MBI-B)	In futuro	—	Terra		90	Bolometro		[1]
	Mobile Anisotropy Telescope (MAT)	1997, 1998	1998	Terra		30-140	HEMT / SIS		[1]
Planck	Planck	2009	—	Space	Lagrange 2	30-857	HEMT / Bolometro	Polarization; Misura delle anisotropie di temperatura della CMB; Foregrounds	[1]
	Polarization Observations of Large Angular Regions (POLAR)	2000	2000	Terra		26-46	HEMT		[1]
	Polarization of Background Microwave Radiation (POLARBeaR)	Future	—	Terra		90-240	Bolometro		[1]
	Polatron	Never	—	Terra		100	Bolometro		[1]
	Princeton I, Q, and U Experiment (PIQUE)	2002	2002	Pallone		90	Bolometro		[1]
	Python	1992	1997	Terra		30-90	HEMT / Bolometro		[1]
	QMAP	1996	1996	Terra		30-140	HEMT / SIS		[1]
	QUaD	2005	2007	Terra	South Pole	100, 150	Bolometro	Measured intermediate scale polarization with improved precision.	[1]
	Qubic	Future	—	Terra		97, 150, 230	Bolometro	Will measure the B-mode polarization on intermediate scale.
	Q/U Imaging ExperimenT (QUIET)	2008	—	Terra	Llano de Chajnantor Observatory, Chile	40, 90	HEMT		[1]
	RELIKT-1	1983	1984	Space	Earth orbit			Misura delle anisotropie di temperatura della CMB	[1]
	Saskatoon experiment	1993	1995	Terra	Saskatchewan	26-46	HEMT		[1]
	Sky Polarization Observatory (SPOrt)	Future	—	Space	International Space Station			Polarization	[1]
South Pole Telescope	South Pole Telescope	2006		Terra	South Pole			Will measure the small scale fluctuations and polarization.	[1]
	SPIDER	2011		Pallone		90, 150, 220	Bolometro	Will measure very large scale polarization.
	Sunyaev-Zeldovich Array (SZA)	Future	—	Terra		26-36; 85-115	Interferometer	Effetto Sunyaev-Zel'dovich	[1]
	Sunyaev-Zeldovich Infrared Experiment (SuZIE)	1996	—	Terra		150, 220, 350	Bolometro	Effetto Sunyaev-Zel'dovich	[1]
	Tenerife Experiment	1984	2000	Terra	Tenerife	10, 15, 33	HEMT		[1]
	TopHat	2002	—	Pallone		150-720	Bolometro		[1]
	Very Small Array	2002	2008	Terra		26-36	Interferometer / HEMT	Measured intermediate and small scale fluctuations with improved precision in small regions of the sky.	[1]
	Wilkinson Microwave Anisotropy Probe (WMAP)	2001	—	Space	Lagrange 2	23-94	HEMT	Misura delle anisotropie di temperatura della CMB; Polarization	[1]

References

1. LAMBDA — CMB Experiment Sites, su lambda.gsfc.nasa.gov, 18 aprile 2008. URL consultato il 13 giugno 2010.
2. ^ Paul Ho, et al., The Yuan-Tseh Lee Array for Microwave Background Anisotropy, 2008, arΧiv:0810.1871.
3. ^ Jiun-Huei Proty Wu, et al., AMiBA Observations, Data Analysis and Results for Sunyaev-Zel'dovich Effects, 2008, arΧiv:0810.1015.