List of cosmic microwave background experiments

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A comparison of the sensitivity and resolution of WMAP with COBE and Penzias and Wilson's telescope, simulated data BigBangNoise.jpg
A comparison of the sensitivity and resolution of WMAP with COBE and Penzias and Wilson's telescope, simulated data

This list is a compilation of experiments measuring the cosmic microwave background (CMB) radiation anisotropies and polarization since the first detection of the CMB by Penzias and Wilson in 1964. There have been a variety of experiments to measure the CMB anisotropies and polarization since its first observation in 1964 by Penzias and Wilson. These include a mix of ground-, balloon- and space-based receivers. [2] [3] Some notable experiments in the list 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; [4] CBI, which made high-resolution observations and obtained the first E-mode polarization spectrum; [5] WMAP; and the Planck spacecraft, which has produced the highest resolution all-sky map to-date of both the temperature anisotropies and polarization signals. [6] Current scientific goals for CMB observation include precise measurement of gravitational lensing, which can constrain the mass of the neutrino; and measurement of B-mode polarization as possible evidence for cosmic inflation.

Contents

The design of cosmic microwave background experiments [2] [3] [4] [7] [8] 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. [8] 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. [4]

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. [7] To minimize side lobes, microwave optics usually utilize elaborate lenses and feed horns. Finally, in ground-based (and, to an extent, balloon-based) instruments, water and oxygen in the atmosphere emit and absorb microwave radiation. Even at frequencies where the atmospheric transmission is high, atmospheric emission contributes photon noise that limits the sensitivity of an experiment. CMB research therefore uses of air- and space-borne experiments, as well as dry, high altitude locations such as the Chilean Andes and the South Pole. [9]

Cosmic microwave background experiments

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. [10]

ImageNameStartEndBasisLocationFrequency (GHz)Detector technologyTargetsReferences
Advanced Cosmic Microwave Explorer (ACME)
Also HACME: HEMT+ACME		19881996Ground South Pole 26–35; 38–45HEMTTemperature anisotropies [10] [11]
Antarctic Plateau Anisotropy Chasing Experiment (APACHE)19951996Ground Antarctic 100, 150, 250BolometerTemperature anisotropies [10]
ARCADE Balloon.jpg Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE)20012006Balloon3, 5, 7, 10, 30, 90HEMTCMB Spectrum [10]
Archeops gondola at launch.jpg Archeops 19992002Balloon143, 217, 353, 545BolometerMeasured large and intermediate scale with improved precision at the larger scales. [10]
Arcminute Cosmology Bolometer Array Receiver (ACBAR)20012008Ground South Pole 150, 219, 274BolometerTemperature anisotropies [10]
Mrao ami lba ryle.jpg Arcminute Microkelvin Imager (AMI)2005—Ground UK: Mullard Radio Astronomy Observatory 12-18Interferometer SZ effect, Temperature anisotropies [10]
Q U I JOint TEnerife (QUIJOTE)2012—Ground Tenerife 11, 13, 17, 19, 30, 40Polarizer / OMTPolarization on degree angular scales [10]
ARGO 1988, 1990, 19931993Balloon150-600Bolometer [10]
AMiBA 1.jpg Array for Microwave Background Anisotropy (AMiBA)2007—GroundHawaii: Mauna Loa 86-102Interferometer/MMICSZ effect; Polarization [10] [12] [13]
Atacama Bmode Search on container.JPG Atacama B-Mode Search (ABS)20122014Ground Chile: Atacama Desert 145BolometerPolarization [10] [14]
Atacama cosmology telescope night.jpg Atacama Cosmology Telescope (ACT)20082022Ground Chile: Atacama Desert 148, 218, 277BolometerSmall-scale temperature and polarization anisotropies [10]
Phot-24a-06.jpg Atacama Pathfinder Experiment (APEX)2007—Ground Chile: Atacama Desert 150, 217BolometerTemperature anisotropies; SZ effect [10]
ATCA Radio Telescope Narrabri 2005 12 21.jpg Australia Telescope Compact Array (ATCA)19911997Ground Paul Wild Observatory, New South Wales, Australia8.7HEMT [10]
Background Emission Anisotropy Scanning Telescope (BEAST)2000—Balloon, Ground25–35; 38-45HEMTA ground single dish CMB observatory at the University of California's White Mountain Peak Research station. [10]
Background Imaging of Cosmic Extragalactic Polarization (BICEP1)20062008Ground South Pole 100, 150, 220BolometerMeasured degree-scale polarization with improved precision. [10] [15]
BICEP2 20092012Ground South Pole 150BolometerDegree-scale B-mode polarization. [10] [16]
Keck Array 2010Ground South Pole 95, 150, 220BolometerDegree-scale B-mode polarization. [10]
Balloon-borne Anisotropy Measurement (BAM)19951998Balloon University of British Columbia and Brown University balloon experiment110-250SpectrometerUsed differential Fourier Transform Spectrometer to measure degree scale anisotropy [10] [17]
Balloon-borne Radiometers for Sky Polarisation Observations (BaR-SPoRT)Cancelled—Balloon32, 90Polarizer / OMT [10]
Berkeley-Illinois-Maryland Association (BIMA)19862004Ground Hat Creek Radio Observatory, California, USA70–116; 210-270SIS [10]
Boomerang Telescope.jpeg BOOMERanG experiment 19972003BalloonLong-duration balloon above Antarctica90-420BolometerIntermediate scale fluctuations [10]
B-mode RAdiation INterferometer (BRAIN)Never—GroundDome-C, Antarctica [18]
Clover Cancelled—Ground97, 150, 230BolometerCancelled experiment to measure the small scale fluctuations and to search for B-mode polarization. [10]
Cobra19821990Sounding RocketUniversity of British Columbia27-900Bolometers/ FTSFrequency spectrum of CMB [19] [20]
Cosmic Anisotropy Polarization Mapper (CAPMAP)20022008GroundCrawford Hill Telescope, New Jersey40, 90MMIC/HEMT [10]
Cosmic Anisotropy Telescope (CAT)19941997Ground Mullard Radio Astronomy Observatory 13-17Interferometer / HEMTVery small scale fluctuations in small regions of the sky. [10]
Cosmic Background Imager.jpeg Cosmic Background Imager (CBI)20002008Ground Llano de Chajnantor Observatory, Chile26-36HEMTVery small scale temperature and polarization anisotropies in a small patch of sky. [10] [21]
CLASS Experiment Site Rendering Feb 2014.png Cosmology Large Angular Scale Surveyor (CLASS)2015—Ground Llano de Chajnantor Observatory, Chile40, 90, 150, 220TES BolometerB-mode polarization signal at multipoles from 2 to 100 [10] [22]
Primordial Inflation Polarization Explorer (PIPER)Future—Balloon200, 270, 350, 800TES bolometersB-mode polarization signal [10] [23]
COSMOSOMAS 19982007Ground Teide Observatory, Tenerife, Spain10-18HEMTCircular scanning experiments for CMB and foregrounds [10] [24]
Cobe vision1.jpg Cosmic Background Explorer (COBE)19891993Space Earth orbit 31.5, 53, 90 (DMR)Temperature anisotropies; frequency power spectrum; solar system and galactic dust foregrounds. [10] [25]
Cobe vision1.jpg Cosmic Background Explorer (COBE)19891990Space Earth orbit 68-3000 200 frequencies (FIRAS)BolometersCMB Spectrum; CMB Temperature; CIB spectrum; Temperature anisotropies; frequency power spectrum; solar system and galactic dust foregrounds. [10] [25]
TRIS19942001Ground Campo Imperatore 0.6, 0.82, 2.5CMB frequency power spectrum [10] [26]
COMPASS20012001Ground Pine Bluff, Wisconsin 26 to 36HEMTPolarization on degree angular scales [27]
Cosmological Gene (CG)19992009Ground RATAN-600, Caucasus, Russia0.6 to 32HEMT [10] [28]
Degree Angular Scale Interferometer (DASI)19992003Ground South Pole 26-36HEMTTemperature and polarization anisotropy on degree angular scales [10]
The E and B Experiment (EBEX)20122013BalloonAntarctica150-450BolometerInflationary gravitational-wave background (IGB) signal in B-mode polarization [10] [29]
Far Infra-Red Survey (FIRS)19891989Balloon National Scientific Balloon Facility, Fort Sumner, New Mexico 170-680BolometerTemperature anisotropy on large angular scales. [10] [30]
KU-band Polarization IDentifier (KUPID)2003—GroundCrawford Hill Telescope, New Jersey12-18HEMT [10] [31]
Medium Scale Anisotropy Measurement (MSAM)19921997Balloon150-650Bolometer [10]
MAXIMA Balloon.jpg Millimeter Anisotropy eXperiment IMaging Array (MAXIMA)1995, 1998, 19991999BalloonNear Palestine, Texas150-420BolometerIntermediate scale temperature fluctuations. [10]
Millimeter Interferometer (MINT)20012002GroundCerro Toco, Chile145SISTemperature anisotropies around multipole 1500 [10] [32]
Millimeter-Wave Bolometric Interferometer (MBI-B)Future—Ground90Bolometer [10]
Mobile Anisotropy Telescope (MAT)1997, 19981998Ground Cerro Toco, Chile30-140HEMT / SIS [10] [33]
Polarization Observations of Large Angular Regions (POLAR)20002000Ground Pine Bluff, Wisconsin, USA26-46HEMTPolarization at large angular scales [10] [34]
Polarbear experiment.jpg POLARBEAR 2012—GroundChajnantor plateau (Chile)150Antenna-coupled TESCMB Polarization. Primordial and lensed B-modes. [10]
Polatron Never—Ground100Bolometer [10]
Princeton I, Q, and U Experiment (PIQUE)20022002Ground Princeton University 90Bolometer [10]
Python19921997Ground South Pole 30-90HEMT / BolometerTemperature anisotropy on intermediate angular scales [10] [35]
QMAP 19961996Balloon30-140HEMT / SIS [10] [36]
050128quad-from-crane.jpg QUaD 20052007Ground South Pole 100, 150BolometerPolarization at intermediate angular scale [10]
QUBIC Future—Ground150, 220BolometerB-mode polarization on intermediate angular scale.[ citation needed ]
Q/U Imaging ExperimenT (QUIET)20082010Ground Llano de Chajnantor Observatory, Chile40, 90HEMT [10] [37]
RELIKT-1 19831984Space Earth orbit 37Temperature anisotropies [10]
Saskatoon experiment 19931995Ground Saskatchewan 26-46HEMT [10]
Simons Observatory 2021-Ground Atacama 27/39, 93/145, 225/280 GHzBolometersB-mode polarization, SZE galaxy clusters, sources [38]
Sky Polarization Observatory (SPOrt)Cancelled—Space International Space Station 22-90Polarization [10]
South Pole Telescope 2006Ground South Pole Small scale temperature and polarization. [10]
SPIDER 2015Balloon Antarctica 90, 150, 220BolometerLarge scale polarization. [10]
Sza.gif Sunyaev-Zeldovich Array (SZA)20042008Ground Owens Valley Radio Observatory 26–36; 85-115InterferometerProduced sensitive CMB anisotropy constraints at l ~ 4000, measured the SZ effect in hundreds of galaxy clusters. Now part of CARMA [10]
MUltiplexed Squid/Tes Array for Ninety Gigahertz (MUSTANG/MUSTANG2) 2007—Ground Green Bank Telescope (West Virginia, USA)90TES bolometers Sunyaev-Zeldovich effect (also used for non-CMB work) [10]
Sunyaev-Zeldovich Infrared Experiment (SuZIE)1996—Ground Caltech Submillimeter Observatory, Mauna Kea, Hawaii150, 220, 350BolometerSZ effect [10]
Tenerife Experiment 19842000Ground Tenerife 10, 15, 33HEMTTemperature anisotropies from degree to arcminute angular scales [10]
TopHat 20012001Balloon Antarctica 150-720Bolometer [10] [39] [40]
Very Small Array 20022008Ground Tenerife 26-36Interferometer / HEMTIntermediate and small scale fluctuations in small regions of the sky. [10] [41]
WMAP collage.jpg Wilkinson Microwave Anisotropy Probe (WMAP)20012010Space Lagrange 2 23-94HEMTTemperature anisotropies; Polarization [10]
Planck 20092013Space Lagrange 2 30-857HEMT / BolometerTemperature and polarization anisotropies; foregrounds [10]

References

  1. ↑ "A Brief History of Background Radiation". WMAP image gallery. Nasa GSFC. Retrieved 26 July 2015.
  2. 1 2 Galli, Silvia; Melchiorri, Alessandro; Pagano, Luca; Sherwin, Blake D.; Spergel, David N. (December 2010). "Constraining fundamental physics with future CMB experiments". Phys. Rev. D. 82 (12): 123504. arXiv: 1005.3808 . Bibcode:2010PhRvD..82l3504G. doi:10.1103/PhysRevD.82.123504. S2CID   118531614.{{cite journal}}: CS1 maint: article number as page number (link)
  3. 1 2 Lawrence, Charles (April 2006). Ongoing and future ground-based and balloon-borne CMB temperature and polarization experiments. CMB and Physics of the Early Universe (CMB2006). Ischia, Italy: Proceedings of Science. p. 12. Bibcode:2006cmb..confE..12L.
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  34. ↑ O'Dell, Chris. "POLAR: Polarization Observations of Large Angular Regions". Archived at NASA GSFC. Retrieved 25 July 2015.
  35. ↑ "CARA Science: Python". University of Chicago.
  36. ↑ Page, Lyman; de Oliveira-Costa, Angelica. "QMAP". Princeton University. Retrieved 25 July 2015.
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  40. ↑ Silverberg, R.F.; E. S., Cheng; J. E., Aguirre; J. J., Bezaire; T. M., Crawford; S. S., Meyer; A., Bier; B., Campano; T. C., Chen; D. A., Cottingham; E. H., Sharp; P. R., Christensen; S., Cordone; P. T., Timbie; R. E., Dame; D. J., Fixsen; R. J. K., Kristensen; H. U., Nørgaard-Nielsen; G. W., Wilson; et al. (TopHat Collaboration) (September 2005). "The TopHat Experiment: A Balloon-borne Instrument for Mapping Millimeter and Submillimeter Emission". The Astrophysical Journal Supplement Series. 160 (1): 59–75. Bibcode:2005ApJS..160...59S. doi: 10.1086/432117 .
  41. ↑ Tibbs, Christopher T.; Watson, Robert A.; Dickinson, Clive; Davies, Rodney D.; Davis, Richard J.; del Burgo, Carlos; Franzen, Thomas M. O.; Genova-Santos, Ricardo; Grainge, Keith; Hobson, Michael P. (2010). "VSA Observations of the Anomalous Microwave Emission in the Perseus Region". Mon. Not. R. Astron. Soc. 402 (3): 1969–1979. arXiv: 0909.4682 . Bibcode:2010MNRAS.402.1969T. doi: 10.1111/j.1365-2966.2009.16023.x . S2CID   18987830.

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