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{{redirect-acronym |WMAP| either radio station [[WXNC]] or [[WGSP-FM]]}}
Marvella is what you can call her but it's not the most female name out there. Minnesota has usually been his house but his wife wants them to transfer. Supervising is my profession. The preferred hobby for my children and me is to perform baseball but I haven't produced a dime with it.<br><br>Check out my website - [http://tinyurl.com/k7cuceb tinyurl.com]
 
{{Use mdy dates|date=February 2012}}
{{Infobox Space Telescope
| name              = Wilkinson Microwave Anisotropy Probe
| image            = [[Image:WMAP collage.jpg|230px]]
| caption          =
| organization      = [[National Aeronautics and Space Administration|NASA]]
| major_contractors =
| alt_names        = MAP; Explorer 80
| nssdc_id          = 2001-027A
| location          = {{L2}}
| orbit_type        = [[Lissajous orbit]]
| accel_gravity    =
| launch_date      = June 30, 2001 at 19:46 [[UTC]]
| launch_location  = [[Cape Canaveral Air Force Station]] [[Cape Canaveral Air Force Station Space Launch Complex 17|SLC-17]], [[Florida]], [[United States of America|U.S.]]
| launch_vehicle    = [[Delta II|Delta II 7425-10]]
| mission_length    = {{For year month day| year=2001 | month=06 | day=30}} elapsed
| deorbit_date      =
| wavelength        =
| mass              = 840 kg (1,851 lb)
| style            =
| diameter          =
| area              =
| focal_length      =
| instrument_1_name = K-band 23&nbsp;GHz
| instrument_1_characteristics = 52.8 [[Minute of arc|MOA]] beam
| instrument_2_name = Ka-band 33&nbsp;GHz
| instrument_2_characteristics = 39.6 MOA beam
| instrument_3_name = Q-band 41&nbsp;GHz
| instrument_3_characteristics = 30.6 MOA beam
| instrument_4_name = V-band 61&nbsp;GHz
| instrument_4_characteristics = 21 MOA beam
| instrument_5_name = W-band 94&nbsp;GHz
| instrument_5_characteristics = 13.2 MOA beam
| website          = [http://map.gsfc.nasa.gov/ map.gsfc.nasa.gov]
| as_of            =
| stats_ref        =<ref name="2003Bennett" /><ref name="2008Limon" /><ref name="news_facts" />
}}
{{cosmology}}
 
The '''Wilkinson Microwave Anisotropy Probe''' ('''WMAP''') – also known as the '''Microwave Anisotropy Probe''' ('''MAP'''), and '''Explorer 80''' – is a [[spacecraft]] which measures differences in the temperature of the [[Big Bang]]'s remnant radiant heat – the [[Cosmic Microwave Background Radiation]] – across the full sky.<ref>{{cite web |title= Wilkinson Microwave Anisotropy Probe: Overview |url= http://lambda.gsfc.nasa.gov/product/map/current/ |work= Legacy Archive for Background Data Analysis (LAMBDA) |publisher= NASA's High Energy Astrophysics Science Archive Research Center (HEASARC) |location= Greenbelt, Maryland |date= August 4, 2009 |quote= The WMAP (Wilkinson Microwave Anisotropy Probe) mission is designed to determine the geometry, content, and evolution of the universe via a 13 arcminute FWHM resolution full sky map of the temperature anisotropy of the cosmic microwave background radiation. |accessdate=September 24, 2009}}</ref><ref>{{cite web |title= Tests of Big Bang: The CMB |url= http://map.gsfc.nasa.gov/universe/bb_tests_cmb.html |work= Universe 101: Our Universe |publisher= NASA|date= July 2009 |quote= Only with very sensitive instruments, such as COBE and WMAP, can cosmologists detect fluctuations in the cosmic microwave background temperature. By studying these fluctuations, cosmologists can learn about the origin of galaxies and large scale structures of galaxies and they can measure the basic parameters of the Big Bang theory. |accessdate=September 24, 2009}}</ref> Headed by Professor [[Charles L. Bennett]], [[Johns Hopkins University]], the mission was developed in a joint partnership between the NASA [[Goddard Space Flight Center]] and [[Princeton University]].<ref name="2003PressRelease" /> The WMAP spacecraft was launched on June 30, 2001, at 19:46:46 GDT, from Florida. The WMAP mission succeeds the [[Cosmic Background Explorer|COBE]] space mission and was the second medium-class (MIDEX) spacecraft of the [[Explorer program]]. In 2003, MAP was renamed WMAP in honor of cosmologist [[David Todd Wilkinson]] (1935–2002),<ref name="2003PressRelease" /> who had been a member of the mission's science team.
 
WMAP's measurements played the key role in establishing the current Standard Model of Cosmology: the [[Lambda-CDM model]].  WMAP data are very well fit by a universe that is dominated by dark energy in the form of a cosmological constant.  Other cosmological data are also consistent, and together tightly constrain the Model.  In the Lambda-CDM model of the universe, the [[age of the universe]] is 13.772&nbsp;±&nbsp;0.059 billion years.  The WMAP mission's determination of the age of the universe to better than 1% precision was recognized by the Guinness Book of World Records.{{citation needed|date=February 2013}} The current expansion rate of the universe is (see [[Hubble's law|Hubble constant]]) of 69.32&nbsp;±&nbsp;0.80&nbsp;km·s<sup>−1</sup>·Mpc<sup>−1</sup>.  The content of the universe presently consists of 4.628&nbsp;±&nbsp;0.093% ordinary [[Baryonic#Baryonic matter|baryonic matter]]; {{val|24.02|+0.88|-0.87}}% [[Cold dark matter]] (CDM) that neither emits nor absorbs light; and {{val|71.35|+0.95|-0.96}}% of [[dark energy]] in the form of a cosmological constant that accelerates the expansion of the universe.{{citation needed|date=February 2013}}  Less than 1% of the current contents of the universe is in neutrinos, but WMAP's measurements have found, for the first time in 2008, that the data prefers the existence of a [[cosmic neutrino background]]<ref name="2009Hinshaw">Hinshaw et al. (2009)</ref> with an effective number of neutrino species of 3.26 &nbsp;±&nbsp; 0.35.  The contents point to a Euclidean [[Shape of the universe|flat geometry]], with curvature (<math>\Omega_{k}</math>) of -{{val|0.0027|+0.0039|-0.0038}}. The WMAP measurements also support the [[cosmic inflation]] paradigm in several ways, including the flatness measurement.
 
According to ''Science'' magazine, the WMAP was the ''Breakthrough of the Year for 2003''.<ref name="2003Seife">Seife (2003)</ref> This mission's results papers were first and second in the "Super Hot Papers in Science Since 2003" list.<ref name="incites">{{cite web | url=http://www.in-cites.com/hotpapers/shp/1-50.html | title="Super Hot" Papers in Science | publisher=in-cites |date=October 2005 | accessdate=April 26, 2008}}</ref> Of the all-time most referenced papers in physics and astronomy in the [[INSPIRE-HEP]] database, only three have been published since 2000, and all three are WMAP publications. On May 27, 2010, it was announced that Bennett, [[Lyman Page|Lyman A. Page, Jr.]], and David N. Spergel, the latter both of Princeton University, would share the 2010 [[Shaw Prize]] in astronomy for their work on WMAP.<ref>{{cite web|title=Announcement of the Shaw Laureates 2010|url=http://www.shawprize.org/en/shawprize2010/announcement/announcement.html}}{{dead link|date=October 2013}}</ref>
 
As of October 2010, the WMAP spacecraft is [[:Category:Derelict satellites in heliocentric orbit|derelict]] in a [[heliocentric orbit|heliocentric graveyard orbit]] after 9 years of operations.<ref name=dn20101007>
{{cite news |title=MISSION COMPLETE! WMAP FIRES ITS THRUSTERS FOR THE LAST TIME |last=O'Neill|first=Ian |url=http://news.discovery.com/space/mission-complete-wmap-fires-its-thrusters-for-the-last-time.html |date=2010-10-07 |publisher=Discovery News |accessdate=2013-01-27}}</ref>
The Astronomy and Physics Senior Review panel at NASA Headquarters endorsed a total of 9 years of WMAP operations, through September 2010.<ref name="news_facts" /> All WMAP data are released to the public and have been subject to careful scrutiny. The final official data release was the [[Wilkinson Microwave Anisotropy Probe#Nine-year data release|nine-year release]] in 2012.<ref name="Space-20121221">{{cite web |last=Gannon |first=Megan |title=New 'Baby Picture' of Universe Unveiled |url=http://www.space.com/19027-universe-baby-picture-wmap.html|date=December 21, 2012 |publisher=[[Space.com]] |accessdate=December 21, 2012 }}</ref><ref name="arXiv-20121220">{{cite journal |last=Bennett |first=C.L. |last2=Larson |first2=L.|last3=Weiland |first3=J.L. |last4=Jarosk |first4= N. |last5=Hinshaw |first5=N. |last6=Odegard|first6=N. |last7=Smith |first7=K.M. |last8=Hill |first8=R.S. |last9=Gold |first9=B.|last10=Halpern |first10=M. |last11=Komatsu |first11=E. |last12=Nolta |first12=M.R.|last13=Page |first13=L. |last114=Spergel |first14=D.N. |last15=Wollack |first15=E.|last16=Dunkley |first16=J. |last17=Kogut |first17=A. |last18=Limon |first18=M. |last19=Meyer|first19=S.S. |last20=Tucker |first20=G.S. |last21=Wright |first21=E.L. |title=Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results| journal=The Astrophysical Journal Supplement | volume=208 | page=20 | doi=10.1088/0067-0049/208/2/20 |arxiv=1212.5225 |date=2013| bibcode = 2013ApJS..208...20B }}</ref>
 
Some aspects of the data are statistically unusual for the Standard Model of Cosmology.  For example, the greatest angular-scale measurements, the [[quadrupole moment]], is somewhat smaller than the Model would predict, but this discrepancy is not highly significant.<ref>O'Dwyer et al., 2004. The Astrophysical Journal, Volume 617, Issue 2, pp. L99-L102. [http://adsabs.harvard.edu/abs/2004ApJ...617L..99O]</ref>  A large [[WMAP cold spot|cold spot]] and other features of the data are more statistically significant, and research continues into these.
 
== Objectives ==
[[Image:CMB Timeline75.jpg|thumb|left|The universe's timeline, from inflation to the WMAP.]]
The WMAP objective is to measure the temperature differences in the [[Cosmic microwave background radiation|Cosmic Microwave Background (CMB) radiation]]. The anisotropies then are used to measure the universe's [[geometry]], content, and evolution; and to test the Big Bang model, and the [[cosmic inflation]] theory.<ref name="2003Bennett" /> For that, the mission is creating a full-sky map of the CMB, with a 13 [[arcminute]] resolution via multi-frequency observation. The map requires the fewest [[systematic error]]s, no correlated pixel noise, and accurate calibration, to ensure angular-scale accuracy greater than its resolution.<ref name="2003Bennett">Bennett et al. (2003a)</ref> The map contains 3,145,728 pixels, and uses the [[HEALPix]] scheme to pixelize the sphere.<ref name="2003Bennettb" /> The telescope also measures the CMB's E-mode polarization,<ref name="2003Bennett" /> and foreground polarization;<ref name="2009Hinshaw" /> its life is 27 months; 3 to reach the {{L2}} position, 2 years of observation.<ref name="2003Bennett" />
[[Image:BigBangNoise.jpg|thumb|right|A comparison of the sensitivity of WMAP with COBE and Penzias and Wilson's [[Holmdel Horn Antenna|telescope]]. Simulated data.]]
 
== Development ==
The MAP mission was proposed to NASA in 1995, selected for definition study in 1996, and approved for development in 1997.<ref name="news_facts">{{cite web | url=http://map.gsfc.nasa.gov/news/facts.html | title=WMAP News: Facts | publisher=NASA | date=April 22, 2008 | accessdate=April 27, 2008}}</ref><ref name="news_events">{{cite web | url=http://map.gsfc.nasa.gov/news/events.html | title=WMAP News: Events | publisher=NASA | date=April 17, 2008 | accessdate=April 27, 2008}}</ref>
 
The WMAP was preceded by two missions to observe the CMB; (i) the Soviet [[RELIKT-1]] that reported the upper-limit measurements of CMB anisotropies, and (ii) the U.S. [[Cosmic Background Explorer|COBE]] satellite that first reported large-scale CMB fluctuations. The WMAP is 45 times more sensitive, with 33 times the angular resolution of its COBE satellite predecessor.<ref name="2008Limon">Limon et al. (2008)</ref>
 
==Spacecraft==
[[Image:WMAP spacecraft diagram.jpg|thumb|left|WMAP spacecraft diagram]]
The telescope's primary reflecting mirrors are a pair of [[Gregorian telescope|Gregorian]] 1.4m x 1.6m dishes (facing opposite directions), that focus the signal onto a pair of 0.9m x 1.0m secondary reflecting mirrors. They are shaped for optimal performance: a [[carbon fibre]] shell upon a [[Korex]] core, thinly-coated with aluminium and [[silicon oxide]]. The secondary reflectors transmit the signals to the corrugated feedhorns that sit on a [[focal plane]] array box beneath the primary reflectors.<ref name="2003Bennett" />
[[Image:WMAP receivers.png|thumb|right|Illustration of WMAP's receivers]]
The receivers are [[Polarization (waves)|polarization]]-sensitive differential [[radiometer]]s measuring the difference between two telescope beams. The signal is amplified with [[HEMT]] [[low-noise amplifier]]s, built by the [[National Radio Astronomy Observatory]]. There are 20 feeds, 10 in each direction, from which a radiometer collects a signal; the measure is the difference in the sky signal from opposite directions. The directional separation azimuth is 180 degrees; the total angle is 141 degrees.<ref name="2003Bennett" /> To avoid collecting [[Milky Way]] galaxy foreground signals, the WMAP uses five discrete radio frequency bands, from 23&nbsp;GHz to 94&nbsp;GHz.<ref name="2003Bennett" />
{{-}}
 
<center>
{| class="wikitable"
|-  style="background:#b0c4de; text-align:center;"
|+ Properties of WMAP at different frequencies<ref name="2003Bennett" />
! Property !! K-band !! Ka-band !! Q-band !! V-band !! W-band
|-
| Central [[wavelength]] (mm) || 13 || 9.1 || 7.3 || 4.9 || 3.2
|-
| Central [[frequency]] ([[GHz]]) || 23 || 33 || 41 || 61 || 94
|-
| [[Bandwidth (signal processing)|Bandwidth]] (GHz) || 5.5 || 7.0 || 8.3 || 14.0 || 20.5
|-
| Beam size (arcminutes) || 52.8 || 39.6 || 30.6 || 21 || 13.2
|-
| Number of radiometers || 2 || 2 || 4 || 4 || 8
|-
| System temperature ([[Kelvin|K]]) || 29 || 39 || 59 || 92 || 145
|-
| Sensitivity (mK s<math>^{1/2}</math>) || 0.8 || 0.8 || 1.0 || 1.2 || 1.6
|}
</center>
The WMAP's base is a 5.0m-diameter [[solar panel]] array that keeps the instruments in shadow during CMB observations, (by keeping the craft constantly angled at 22 degrees, relative to the sun). Upon the array sit a bottom deck (supporting the warm components) and a top deck. The telescope's cold components: the focal-plane array and the mirrors, are separated from the warm components with a cylindrical, 33&nbsp;cm-long thermal isolation shell atop the deck.<ref name="2003Bennett" />
 
Passive thermal radiators cool the WMAP to ca. 90 degrees K; they are connected to the low-noise amplifiers. The telescope consumes 419 W of power. The available telescope heaters are emergency-survival heaters, and there is a transmitter heater, used to warm them when off. The WMAP spacecraft's temperature is monitored with [[platinum resistance thermometer]]s.<ref name="2003Bennett" />
 
The WMAP's calibration is effected with the CMB dipole and measurements of [[Jupiter]]; the beam patterns are measured against Jupiter. The telescope's data are relayed daily via a 2&nbsp;GHz [[transponder]] providing a 667[[kbit/s]] downlink to a 70m [[Deep Space Network]] telescope. The spacecraft has two transponders, one a redundant back-up; they are minimally active – ca. 40 minutes daily – to minimize [[radio frequency interference]]. The telescope's position is maintained, in its three axes, with three [[reaction wheel]]s, [[gyroscope]]s, two [[star tracker]]s and sun sensors, and is steered with eight [[hydrazine]] thrusters.<ref name="2003Bennett" />
 
== Launch, trajectory, and orbit ==
[[Image:WMAP trajectory and orbit.jpg|thumb|right|The WMAP's trajectory and orbit.]]
[[File:WMAP launch.jpg|thumb|left|WMAP launches from [[Kennedy Space Center]], June 30, 2001.]]
 
The WMAP spacecraft arrived at the Kennedy Space Center on April 20, 2001. After being tested for two months, it was launched via Delta II 7425 rocket on June 30, 2001.<ref name="2008Limon" /><ref name="news_facts" /> It began operating on its internal power five minutes before its launching, and so continued operating until the solar panel array deployed. The WMAP was activated and monitored while it cooled. On July 2, it began working, first with in-flight testing (from launching until August 17), then began constant, formal work.<ref name="2008Limon" /> Afterwards, it effected three Earth-Moon phase loops, measuring its [[sidelobe]]s, then flew by the Moon on July 30, en route to the Sun-Earth {{L2}} [[Lagrangian point]], arriving there on October 1, 2001, becoming, thereby, the first CMB observation mission permanently posted there.<ref name="news_facts" />
 
[[Image:WMAP orbit.jpg|thumb|WMAP's orbit and sky scan strategy]]
The spacecraft's location at Lagrange 2, (1.5 million kilometers from Earth) minimizes the amount of contaminating solar, terrestrial, and lunar emissions registered, and thermally stabilizes it. To view the entire sky, without looking to the sun, the WMAP traces a path around {{L2}} in a [[Lissajous orbit]] ca. 1.0 degree to 10 degrees,<ref name="2003Bennett" /> with a 6-month period.<ref name="news_facts" /> The telescope rotates once every 2 minutes, 9 seconds" (0.464 rpm) and [[Precession|precesses]] at the rate of 1 revolution per hour.<ref name="2003Bennett" /> WMAP measures the entire sky every six months, and completed its first, full-sky observation in April 2002.<ref name="news_events" />
 
== Foreground radiation subtraction ==
The WMAP observes in five frequencies, permitting the measurement and subtraction of foreground contamination (from the Milky Way and extra-galactic sources) of the CMB. The main emission mechanisms are [[synchrotron radiation]] and [[Bremsstrahlung|free-free emission]] (dominating the lower frequencies), and [[astrophysical dust]] emissions (dominating the higher frequencies). The spectral properties of these emissions contribute different amounts to the five frequencies, thus permitting their identification and subtraction.<ref name="2003Bennett" />
 
Foreground contamination is removed in several ways. First, subtract extant emission maps from the WMAP's measurements; second, use the components' known spectral values to identify them; third, simultaneously fit the position and spectra data of the foreground emission, using extra data sets. Foreground contamination also is reduced by using only the full-sky map portions with the least foreground contamination, whilst masking the remaining map portions.<ref name="2003Bennett" />
 
{| class="wikitable"
|+ The five-year models of foreground emission, at different frequencies. Red = Synchrotron; Green = free-free; Blue = thermal dust.
|-
| [[Image:WMAP 2008 23GHz foregrounds.png|150px|23&nbsp;GHz]] || [[Image:WMAP 2008 33GHz foregrounds.png|150px|33&nbsp;GHz]] || [[Image:WMAP 2008 41GHz foregrounds.png|150px|41&nbsp;GHz]] || [[Image:WMAP 2008 61GHz foregrounds.png|150px|61&nbsp;GHz]] || [[Image:WMAP 2008 94GHz foregrounds.png|150px|94&nbsp;GHz]]
|-
| 23&nbsp;GHz || 33&nbsp;GHz || 41&nbsp;GHz || 61&nbsp;GHz || 94&nbsp;GHz
|}
 
== Measurements and discoveries ==
 
=== One-year data release ===
[[Image:Baby Universe.jpg|thumb|1 year WMAP image of background cosmic radiation (2003).]]
On February 11, 2003, NASA published the First-year's worth of WMAP data.  The latest calculated age and composition of the early universe were presented. In addition, an image of the early universe, that "contains such stunning detail, that it may be one of the most important scientific results of recent years" was presented. The newly released data surpass previous CMB measurements.<ref name="2003PressRelease">{{cite web | url=http://www.gsfc.nasa.gov/topstory/2003/0206mapresults.html | title=New image of infant universe reveals era of first stars, age of cosmos, and more | publisher=NASA / WMAP team | date=February 11, 2003 | accessdate=April 27, 2008 |archiveurl = http://web.archive.org/web/20080227175308/http://www.gsfc.nasa.gov/topstory/2003/0206mapresults.html <!-- Bot retrieved archive --> |archivedate = February 27, 2008}}</ref>
 
Based upon the Lambda-CDM model, the WMAP team produced cosmological parameters from the WMAP's first-year results. Three sets are given below; the first and second sets are WMAP data; the difference is the addition of spectral indices, predictions of some inflationary models. The third data set combines the WMAP constraints with those from other CMB experiments ([[ACBAR]] and [[Cosmic Background Imager|CBI]]), and constraints from the [[2dF Galaxy Redshift Survey]] and [[Lyman alpha forest]] measurements. Note that there are degenerations among the parameters, the most significant is between <math>n_s</math> and <math>\tau</math>; the errors given are at 68% confidence.<ref name="2003spergel" />
 
<center>
{| class="wikitable" style="text-align:center;"
|-  style="background:#b0c4de; text-align:center;"
|+ Best-fit cosmological parameters from WMAP one-year results<ref name="2003spergel">Spergel et al. (2003)</ref>
! Parameter !! Symbol !! Best fit (WMAP only) !! Best fit (WMAP, extra parameter) !! Best fit (all data)
|-
| [[Age of the universe]] ([[Annum|Ga]]) || <math>t_0</math> || {{val|13.4|0.3}} || – ||{{val|13.7|0.2}}
|-
| [[Hubble's constant]] ( {{frac|km|[[parsec|Mpc]]·s}} ) || <math>H_0</math> || {{val|72|5}} || {{val|70|5}} || {{val|71|+4|-3}}
|-
| [[Baryon]]ic content || <math>\Omega_b h^2</math> || {{val|0.024|0.001}} || {{val|0.023|0.002}} || {{val|0.0224|0.0009}}
|-
| Matter content || <math>\Omega_m h^2</math> || {{val|0.14|0.02}} || {{val|0.14|0.02}} || {{val|0.135|+0.008|-0.009}}
|-
| [[Optical depth]] to [[reionization]] || <math>\tau</math> || {{val|0.166|+0.076|-0.071}} || {{val|0.20|0.07}} || {{val|0.17|0.06}}
|-
| Amplitude || ''A'' || {{val|0.9|0.1}} || {{val|0.92|0.12}} || {{val|0.83|+0.09|-0.08}}
|-
| Scalar spectral index || <math>n_s</math> || {{val|0.99|0.04}} || {{val|0.93|+0.07|-0.07}}<!-- why not simply ±0.07? --> || {{val|0.93|0.03}}
|-
| Running of spectral index || <math>dn_s / dk</math> ||—||{{val|-0.047|0.04}} || {{val|-0.031|+0.016|-0.017}}
|-
| Fluctuation amplitude at 8h<sup>−1</sup> Mpc|| <math>\sigma_8</math> || {{val|0.9|0.1}} ||—|| {{val|0.84|0.04}}
|-
| Total density of the universe || <math>\Omega_{tot}</math> || – || – || {{val|1.02|0.02}}
|}
</center>
 
Using the best-fit data and theoretical models, the WMAP team determined the times of important universal events, including the redshift of reionization, {{val|17|4}}; the redshift of [[decoupling]], {{val|1089|1}} (and the universe's age at decoupling, {{val|379|+8|-7|u=kyr}}); and the redshift of matter/radiation equality, {{val|3233|+194|-210}}. They determined the thickness of the [[surface of last scattering]] to be {{val|195|2}} in redshift, or {{val|118|+3|-2|u=kyr}}. They determined the current density of baryons, {{val|2.5|0.1|e=-7|u=cm<sup>−1</sup>}}, and the ratio of baryons to photons, {{val|6.1|+0.3|-0.2|e=-10}}. The WMAP's detection of an early reionization excluded [[warm dark matter]].<ref name="2003spergel" />
 
The team also examined Milky Way emissions at the WMAP frequencies, producing a 208-[[point source]] catalogue. Also, they observed the [[Sunyaev-Zel'dovich effect]] at 2.5&nbsp;[[standard deviation|σ]] the strongest source is the [[Coma cluster]].<ref name="2003Bennettb">Bennett et al. (2003b)</ref><!-- Sentence doesn't make sense-->
 
=== Three-year data release ===
[[Image:Microwave Sky polarization.png|thumb|3-year WMAP image of background cosmic radiation (2006).]]
The Three-year WMAP data were released on March 17, 2006. The data included temperature and polarization measurements of the CMB, which provided further confirmation of the standard flat [[Lambda-CDM model]] and new evidence in support of inflation.
 
The 3-year WMAP data alone shows that the universe must have dark matter. Results were computed both only using WMAP data, and also with a mix of parameter constraints from other instruments, including other CMB experiments ([[ACBAR]], [[Cosmic Background Imager|CBI]] and [[BOOMERANG]]), [[Sloan Digital Sky Survey|SDSS]], the [[2dF Galaxy Redshift Survey]], the [[Supernova Legacy Survey]] and constraints on the Hubble constant from the [[Hubble Space Telescope]].<ref name="2007Spergel" />
{{-}}
<center>
{| class="wikitable" style="text-align:center;"
|-  style="background:#b0c4de; text-align:center;"
|+ Best-fit cosmological parameters from WMAP three-year results<ref name="2007Spergel">Spergel et al. (2007)</ref>
! Parameter !! Symbol !! Best fit (WMAP only)
|-
| [[Age of the universe]] ([[Annum|Ga]]) || <math>t_0</math> || {{val|13.73|+0.16|-0.15}}
|-
| [[Hubble's constant]] ( {{frac|km|Mpc·s}} ) || <math>H_0</math> || {{val|73.2|+3.1|-3.2}}
|-
| [[Baryon]]ic content || <math>\Omega_b h^2</math> || {{val|0.0229|0.00073}}
|-
| Matter content || <math>\Omega_m h^2</math> || {{val|0.1277|+0.0080|-0.0079}}
|-
| [[Optical depth]] to [[reionization]] <sup>{{ref|a|[a]}}</sup> || <math>\tau</math> || {{val|0.089|0.030}}
|-
| Scalar spectral index ||<math>n_s</math> || {{val|0.958|0.016}}
|-
| Fluctuation amplitude at 8h<sup>−1</sup> Mpc ||<math>\sigma_8</math> || {{val|0.761|+0.049|-0.048}}
|-
| Tensor-to-scalar ratio <sup>{{ref|b|[b]}}</sup> || ''r'' || <&nbsp;0.65
|}
</center>
 
[a] {{note|a}} Optical depth to reionization improved due to polarization measurements.<ref name="2007Hinshaw">Hinshaw et al. (2007)</ref><br>
[b] {{note|b}} <&nbsp;0.30 when combined with [[Sloan Digital Sky Survey|SDSS]] data. No indication of non-gaussianity.<ref name="2007Spergel" />
 
=== Five-year data release ===
[[Image:WMAP 2008.png|thumb|5-year WMAP image of background cosmic radiation (2008).]]
The Five-year WMAP data were released on February 28, 2008. The data included new evidence for the [[cosmic neutrino background]], evidence that it took over half a billion years for the first stars to reionize the universe, and new constraints on [[cosmic inflation]].<ref name="2008PressRelease">{{cite web | url=http://map.gsfc.nasa.gov/news/ | title=WMAP Press Release&nbsp;— WMAP reveals neutrinos, end of dark ages, first second of universe | publisher=NASA / WMAP team | date=March 7, 2008 | accessdate=April 27, 2008}}</ref>
{{Multiple image |direction=horizontal |align=left |width=150 |image1=WMAP 2008 TT and TE spectra.png |image2=WMAP 2008 universe content.png |caption1=The five-year total-intensity and polarization spectra from WMAP |caption2=Matter/energy content in the current universe (top) and at the time of photon decoupling in the [[Recombination (cosmology)|recombination]] [[Epoch (astronomy)|epoch]] 380,000 years after the Big Bang (bottom) |footer= |header= }}
The improvement in the results came from both having an extra 2 years of measurements (the data set runs between midnight on August 10, 2001 to midnight of August 9, 2006), as well as using improved data processing techniques and a better characterization of the instrument, most notably of the beam shapes. They also make use of the 33&nbsp;GHz observations for estimating cosmological parameters; previously only the 41&nbsp;GHz and 61&nbsp;GHz channels had been used. Finally, improved masks were used to remove foregrounds.<ref name="2009Hinshaw" />
 
Improvements to the spectra were in the 3rd acoustic peak, and the polarization spectra.<ref name="2009Hinshaw" />
 
The measurements put constraints on the content of the universe at the time that the CMB was emitted; at the time 10% of the universe was made up of neutrinos, 12% of atoms, 15% of photons and 63% dark matter. The contribution of dark energy at the time was negligible.<ref name="2008PressRelease" /> It also constrained the content of the present-day universe; 4.6% atoms, 23% dark matter and 72% dark energy.<ref name="2009Hinshaw"/>
 
The WMAP five-year data was combined with measurements from [[Type Ia supernova]] (SNe) and [[Baryon acoustic oscillations]] (BAO).<ref name="2009Hinshaw" />
 
The elliptical shape of the WMAP skymap is the result of a [[Mollweide projection]].<ref>[http://lambda.gsfc.nasa.gov/product/map/pub_papers/firstyear/basic/wmap_cb1_images.cfm WMAP 1-year Paper Figures], Bennett, et al.</ref>
 
<center>
{| class="wikitable" style="text-align:center;"
|-  style="background:#b0c4de; text-align:center;"
|+ Best-fit [[Lambda-CDM model|cosmological parameters]] from WMAP five-year results<ref name="2009Hinshaw" />
! Parameter !! Symbol !! Best fit (WMAP only) !! Best fit (WMAP + SNe + BAO)
|-
| [[Age of the universe]] (Ga) || <math>t_0</math> || {{val|13.69|0.13}} || {{val|13.72|0.12}}
|-
| [[Hubble's constant]] ( {{frac|km|Mpc·s}} ) || <math>H_0</math> || {{val|71.9|+2.6|-2.7}} || {{val|70.5|1.3}}
|-
| [[Baryon]]ic content || <math>\Omega_b h^2</math> || {{val|0.02273|0.00062}} || {{val|0.02267|+0.00058|-0.00059}}
|-
| Cold dark matter content || <math>\Omega_c h^2</math> || {{val|0.1099|0.0062}} || {{val|0.1131|0.0034}}
|-
| [[Dark energy]] content || <math>\Omega_\Lambda</math> || {{val|0.742|0.030}} || {{val|0.726|0.015}}
|-
| [[Optical depth]] to [[reionization]] || <math>\tau</math> || {{val|0.087|0.017}} || {{val|0.084|0.016}}
|-
| Scalar spectral index || <math>n_s</math> || {{val|0.963|+0.014|-0.015}}|| {{val|0.960|0.013}}
|-
| Running of spectral index || <math>dn_s / dlnk</math> || {{val|-0.037|0.028}} || {{val|-0.028|0.020}}
|-
| Fluctuation amplitude at 8h<sup>−1</sup> Mpc || <math>\sigma_8</math> || {{val|0.796|0.036}} || {{val|0.812|0.026}}
|-
| Total density of the universe || <math>\Omega_{tot}</math> || {{val|1.099|+0.100|-0.085}} || {{val|1.0050|+0.0060|-0.0061}}
|-
| Tensor-to-scalar ratio || ''r'' || <&nbsp;0.43 || <&nbsp;0.22
|}
</center>
 
The data puts a limits on the value of the tensor-to-scalar ratio, r <&nbsp;0.22 (95% certainty), which determines the level at which gravitational waves affect the polarization of the CMB, and also puts limits on the amount of primordial [[non-gaussianity]]. Improved constraints were put on the redshift of reionization, which is {{val|10.9|1.4}}, the redshift of [[decoupling]], {{val|1090.88|0.72}} (as well as age of universe at decoupling, {{val|376.971|+3.162|-3.167|u=kyr}}) and the redshift of matter/radiation equality, {{val|3253|+89|-87}}.<ref name="2009Hinshaw" />
 
The [[extragalactic]] source catalogue was expanded to include 390 sources, and variability was detected in the emission from [[Mars]] and [[Saturn]].<ref name="2009Hinshaw" />
 
{| class="wikitable"
|-  style="background:#b0c4de; text-align:center;"
|+ The five-year maps at different frequencies from WMAP with foregrounds (the red band)
|-
| [[Image:WMAP 2008 23GHz.png|150px|23&nbsp;GHz]] || [[Image:WMAP 2008 33GHz.png|150px|33&nbsp;GHz]] || [[Image:WMAP 2008 41GHz.png|150px|41&nbsp;GHz]] ||[[Image:WMAP 2008 61GHz.png|150px|61&nbsp;GHz]] || [[Image:WMAP 2008 94GHz.png|150px|94&nbsp;GHz]]
|-
| 23&nbsp;GHz || 33&nbsp;GHz || 41&nbsp;GHz || 61&nbsp;GHz || 94&nbsp;GHz
|}
 
=== Seven-year data release ===
{{Commons category|WMAP 7-year results}}
[[Image:WMAP 2010.png|thumb|7-year WMAP image of background cosmic radiation (2010).]]
The Seven-year WMAP data were released on January 26, 2010. As part of this release, claims for inconsistencies with the standard model were investigated.<ref name="WMAP CMB">[http://arxiv.org/abs/1001.4758] Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Are There Cosmic Microwave Background Anomalies?</ref> Most were shown not to be statistically significant, and likely due to ''a posteriori'' selection (where one sees a weird deviation, but fails to consider properly how hard one has been looking; a deviation with 1:1000 likelihood will typically be found if one tries one thousand times). For the deviations that do remain, there are no alternative cosmological ideas (for instance, there seem to be correlations with the ecliptic pole). It seems most likely these are due to other effects, with the report mentioning uncertainties in the precise beam shape and other possible small remaining instrumental and analysis issues.
 
The other confirmation of major significance is of the total amount of matter/energy in the Universe in the form of Dark Energy – 72.8% (within 1.6%) as non 'particle' background, and Dark Matter – 22.7% (within 1.4%) of non baryonic (sub atomic) 'particle' energy.  This leaves matter, or baryonic particles (atoms) at only 4.56% (within 0.16%).
 
<center>
{| class="wikitable" style="text-align:center;"
|-  style="background:#b0c4de; text-align:center;"
|+ Best-fit [[Lambda-CDM model|cosmological parameters]] from WMAP seven-year results<ref name="Jarosik2010">Table 8 on p. 39 of {{cite web | author = Jarosik, N., et al. (WMAP Collaboration) | title = Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Sky Maps, Systematic Errors, and Basic Results | url = http://lambda.gsfc.nasa.gov/product/map/dr4/pub_papers/sevenyear/basic_results/wmap_7yr_basic_results.pdf |format=PDF|publisher=nasa.gov|accessdate=December 4, 2010}}  (from NASA's [http://lambda.gsfc.nasa.gov/product/map/dr4/map_bibliography.cfm WMAP Documents] page)</ref>
! Parameter !! Symbol !! Best fit (WMAP only) !! Best fit (WMAP + [[Baryon Acoustic Oscillations|BAO]]<ref name="Percival2010">{{cite journal | author = Percival, Will J. et al. | title = Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample | journal = Monthly Notices of the Royal Astronomical Society | volume = 401 | issue = 4 | pages = 2148–2168 | date = February 2010 | doi = 10.1111/j.1365-2966.2009.15812.x |bibcode = 2010MNRAS.401.2148P |arxiv=0907.1660}}</ref> + H<sub>0</sub><ref name="Riess2009">{{cite web | author = Riess, Adam G. et al. | title = A Redetermination of the Hubble Constant with the Hubble Space Telescope from a Differential Distance Ladder | url = http://hubblesite.org/pubinfo/pdf/2009/08/pdf.pdf |format=PDF|publisher=hubblesite.org|accessdate=December 4, 2010}}</ref>)
|-
| [[Age of the universe]] (Ga) || <math>t_0</math> || {{val|13.75|0.13}} || {{val|13.75|0.11}}
|-
| [[Hubble's constant]] ( {{frac|km|Mpc·s}} ) || <math>H_0</math> || {{val|71.0|2.5}} || {{val|70.4|+1.3|-1.4}}
|-
| [[Baryon]] density || <math>\Omega_b</math> || {{val|0.0449|0.0028}} || {{val|0.0456|0.0016}}
|-
| Physical [[baryon]] density || <math>\Omega_b h^2</math> || {{val|0.02258|+0.00057|-0.00056}} || {{val|0.02260|0.00053}}
|-
| [[Dark matter]] density || <math>\Omega_c</math> || {{val|0.222|0.026}} || {{val|0.227|0.014}}
|-
| Physical [[dark matter]] density || <math>\Omega_c h^2</math> || {{val|0.1109|0.0056}} || {{val|0.1123|0.0035}}
|-
| [[Dark energy]] density || <math>\Omega_\Lambda</math> || {{val|0.734|0.029}} || {{val|0.728|+0.015|-0.016}}
|-
| Fluctuation amplitude at 8h<sup>−1</sup> Mpc || <math>\sigma_8</math> || {{val|0.801|0.030}} || {{val|0.809|0.024}}
|-
| Scalar spectral index || <math>n_s</math> || {{val|0.963|0.014}}|| {{val|0.963|0.012}}
|-
| [[Reionization]] [[optical depth]] || <math>\tau</math> || {{val|0.088|0.015}} || {{val|0.087|0.014}}
|-
| *Total density of the universe || <math>\Omega_{tot}</math> || {{val|1.080|+0.093|-0.071}} ||{{val|1.0023|+0.0056|-0.0054}}
|-
| *Tensor-to-scalar ratio, k<sub>0</sub> = 0.002 Mpc<sup>−1</sup> || ''r'' || <&nbsp;0.36 (95% CL) || <&nbsp;0.24 (95% CL)
|-
| *Running of spectral index, k<sub>0</sub> = 0.002 Mpc<sup>−1</sup> || <math>dn_s / dlnk</math>|| {{val|-0.034|0.026}} || {{val|-0.022|0.020}}
|-
| Note: * = Parameters for extended models<br> (parameters place limits on deviations<br> from the [[Lambda-CDM model]])<ref name="Jarosik2010" />
|}
</center>
 
{| class="wikitable"
|-  style="background:#b0c4de; text-align:center;"
|+ The Seven-year maps at different frequencies from WMAP with foregrounds (the red band)
|-
| [[Image:WMAP 2010 23GHz.png|150px|23&nbsp;GHz]] || [[Image:WMAP 2010 33GHz.png|150px|33&nbsp;GHz]] || [[Image:WMAP 2010 41GHz.png|150px|41&nbsp;GHz]] || [[Image:WMAP 2010 61GHz.png|150px|61&nbsp;GHz]] || [[Image:WMAP 2010 94GHz.png|150px|94&nbsp;GHz]]
|-
| 23&nbsp;GHz || 33&nbsp;GHz || 41&nbsp;GHz || 61&nbsp;GHz || 94&nbsp;GHz
|}
 
=== Nine-year data release ===
 
{{Commons category|WMAP results}}
[[File:Ilc 9yr moll4096.png|thumb|9-year WMAP image of background cosmic radiation (2012).]]
On December 20, 2012, the Nine-year WMAP data and related images were released. "{{val|13.772|0.059}}" billion year old temperature fluctuations and a temperature range of ± 200 micro-[[Kelvin]] are shown in the image. In addition, the study found that "95-percent" of the early universe is composed of [[dark matter]] and [[dark energy|energy]], the curvature of space is less than 0.4 percent of "flat" and the universe emerged from the [[Chronology of the universe#Dark Ages|cosmic Dark Ages]] "about 400 million years" after the [[Big Bang]].<ref name="Space-20121221" /><ref name="arXiv-20121220" /><ref name='arXiv-1212.5226'>[http://adsabs.harvard.edu/abs/2012arXiv1212.5226H Hinshaw et al., 2013]</ref>
{{-}}
<!---please check table data values & related (12/22/2012, [[User:Drbogdan|Drbogdan]])--->
<center>
{| class="wikitable" style="text-align:center;"
|-  style="background:#b0c4de; text-align:center;"
|+ Best-fit [[Lambda-CDM model|cosmological parameters]] from WMAP nine-year results<ref name="arXiv-20121220" />
! Parameter !! Symbol !! Best fit (WMAP only) !! Best fit (WMAP + eCMB + [[Baryon Acoustic Oscillations|BAO]] + H<sub>0</sub>)
|-
| [[Age of the universe]] (Ga) || <math>t_0</math> || {{val|13.74|0.11}} || {{val|13.772|0.059}}
|-
| [[Hubble's constant]] ( {{frac|km|Mpc·s}} ) || <math>H_0</math> || {{val|70.0|2.2}} ||  {{val|69.32|0.80}}
|-
| [[Baryon]] density || <math>\Omega_b</math> || {{val|0.0463|0.0024}} || {{val|0.04628|0.00093}}
|-
| Physical [[baryon]] density || <math>\Omega_b h^2</math> || {{val|0.02264|0.00050}} ||  {{val|0.02223|0.00033}}
|-
| Cold [[Dark matter]] density || <math>\Omega_c</math> || {{val|0.233|0.023}} || {{val|0.2402|+0.0088|-0.0087}}
|-
| Physical cold [[dark matter]] density || <math>\Omega_c h^2</math> || {{val|0.1138|0.0045}} || {{val|0.1153|0.0019}}
|-
| [[Dark energy]] density || <math>\Omega_\Lambda</math> || {{val|0.721|0.025}} ||  {{val|0.7135|+0.0095|-0.0096}}
|-
| Density fluctuations at 8h<sup>−1</sup> Mpc || <math>\sigma_8</math> || {{val|0.821|0.023}} ||{{val|0.820|+0.013|-0.014}}
|-
| Scalar spectral index || <math>n_s</math> || {{val|0.972|0.013}}||  {{val|0.9608|0.0080}}
|-
| [[Reionization]] [[optical depth]] || <math>\tau</math> || {{val|0.089|0.014}} ||  {{val|0.081|0.012}}
|-
| Curvature || 1 - <math>\Omega_{tot}</math> || -{{val|0.037|+0.044|-0.042}} || -{{val|0.0027|+0.0039|-0.0038}}
|-
| Tensor-to-scalar ratio (k<sub>0</sub> = 0.002 Mpc<sup>−1</sup>) || ''r'' || <&nbsp;0.38 (95% CL)|| <&nbsp;0.13 (95% CL)
|-
| Running scalar spectral index || <math>dn_s / dlnk</math>|| -{{val|0.019|0.025}} || -{{val|0.023|0.011}}
|}
</center>
{{-}}
 
==Main result==
{{update|section|date=December 2012}}
[[File:WMAP.ogv|thumb|350px|Interviews with Dr. Charles Bennett and Dr. Lyman Page about WMAP.]]
[[Image:Planck satellite.jpg|thumb|left|upright|Artist's impression of the European Space Agency's [[Planck (spacecraft)|Planck spacecraft]]]]
The main result of the mission is contained in the various oval maps of the CMB spectrum over the years. These oval images present the temperature distribution gained by the WMAP team from the observations by the telescope of the mission. Measured is the temperature obtained from a  [[Planck's law]] interpretation of the microwave background. The oval map covers the whole sky. The results describe the state of the universe only some hundred-thousand years after the [[Big Bang]], which happened roughly 13.8 billion years before our time. The microwave background is very homogeneous in temperature (the relative variations from the mean, which presently is still 2.7 kelvins, are only of the order of ''5x10<sup>−5</sup>''. The temperature variations corresponding to the local directions are presented through different colours (the "red" directions are hotter, the "blue" directions cooler than the average).
 
== Follow-on missions and future measurements ==
The original timeline for WMAP gave it two years of observations; these were completed by September 2003. Mission extensions were granted in 2002, 2004, 2006, and 2008 giving the spacecraft a total of 9 observing years, which ended August 2010<ref name="news_facts" /> and in October 2010 the spacecraft was moved to a [[heliocentric orbit|heliocentric "graveyard" orbit]]<ref name=dn20101007 /> outside of L2, in which it orbits the sun 14 times every 15 years.{{citation needed|date=January 2013}}<!-- orbit details are not in the Discovery News source -->
[[File:PIA16874-CobeWmapPlanckComparison-20130321.jpg|thumb|right|300px|Comparison of [[CMB]] results from [[Cosmic Background Explorer|COBE]], [[WMAP]] and [[Planck (spacecraft)|Planck]] - March 21, 2013.]]
The [[Planck (spacecraft)|Planck spacecraft]], launched on the May 14, 2009, also measures the CMB and aims to refine the measurements made by WMAP, both in total intensity and polarization. Various ground- and balloon-based instruments have also made CMB contributions, and others are being constructed to do so.  Many are aimed at searching for the B-mode polarization expected from the simplest models of inflation, including [[The E and B Experiment|EBEX]], [[Spider (polarimeter)|Spider]], [[BICEP2]], [[Keck Array|Keck]], [[QUIET]], CLASS, SPTpol and others.
 
On 21 March 2013, the European-led research team behind the [[Planck (spacecraft)|Planck cosmology probe]] released the mission's all-sky map of the cosmic microwave background.<ref name="NASA-20130321">{{cite web|last1=Clavin |first1=Whitney |last2=Harrington |first2=J.D. |title=Planck Mission Brings Universe Into Sharp Focus |url=http://www.jpl.nasa.gov/news/news.php?release=2013-109&rn=news.xml&rst=3739 |date=21 March 2013|work=[[NASA]] |accessdate=21 March 2013 }}</ref><ref name="NYT-20130321g">{{cite news |author=Staff |title=Mapping the Early Universe |url=http://www.nytimes.com/interactive/2013/03/21/science/space/0321-universe.html |date=21 March 2013 |work=[[New York Times]] |accessdate=23 March 2013 }}</ref>  The map suggests the [[universe]] is slightly older than thought.  According to the map, subtle fluctuations in temperature were imprinted on the deep sky when the [[cosmos]] was about 370,000 years old. The imprint reflects ripples that arose as early, in the existence of the universe, as the first nonillionth (10<sup>−30</sup>) of a second. Apparently, these ripples gave rise to the present vast [[cosmic web]] of [[galaxy clusters]] and [[dark matter]].  According to the team, the [[universe]] is [[Planck (spacecraft)#2013 data release|13.798 ± 0.037]] [[1,000,000,000|billion]] years old, and contains 4.9% [[matter|ordinary matter]], 26.8% [[dark matter]] and 68.3% [[dark energy]].<ref name="planck_overview">{{cite journal|url=http://www.sciops.esa.int/SA/PLANCK/docs/Planck_2013_results_01.pdf |title=Planck 2013 results. I. Overview of products and scientific results |journal=Astronomy & Astrophysics ''(submitted)'' |first1=P. A. R. |last1=Ade|first2=N. |last2=Aghanim |first3=C. |last3=Armitage-Caplan |last4=''et al''. (Planck Collaboration) |date=20 March 2013 |arxiv=1303.5062|bibcode = 2013arXiv1303.5062P }}{{dead link|date=October 2013}}</ref>  Also, the [[Hubble constant]] was measured to be [[Planck (spacecraft)#2013 data release|67.80 ± 0.77 (km/s)/Mpc]].<ref name="NASA-20130321" /><ref name="planck_overview" /><ref name="ESA-20130321">{{cite web|url=http://www.esa.int/Our_Activities/Space_Science/Planck/Planck_reveals_an_almost_perfect_Universe|title=Planck reveals an almost perfect Universe |work=ESA.int |publisher=European Space Agency |date=21 March 2013 |accessdate=21 March 2013}}</ref><ref name="NYT-20130321">{{cite news|url=http://www.nytimes.com/2013/03/22/science/space/planck-satellite-shows-image-of-infant-universe.html?pagewanted=all |title=Universe as an Infant: Fatter Than Expected and Kind of Lumpy |work=[[The New York Times]]|first=Dennis |last=Overbye |date=21 March 2013 |accessdate=21 March 2013}}</ref><ref name="NBC-20130321">{{cite news|url=http://cosmiclog.nbcnews.com/_news/2013/03/21/17397298-planck-probes-cosmic-baby-picture-revises-universes-vital-statistics|title=Planck probe's cosmic 'baby picture' revises universe's vital statistics |work=Cosmic Log ''via'' [[NBC News]] |first=Alan |last=Boyle |date=21 March 2013 |accessdate=21 March 2013}}</ref>
{{-}}
 
== See also ==
* European Space Agency [[Planck (spacecraft)]]
* [[List of cosmic microwave background experiments]]
 
== References ==
 
===Footnotes===
{{Reflist|2}}
 
=== Primary sources ===
{{refbegin}}
* {{cite journal | title=The Microwave Anisotropy Probe (MAP) Mission | first=C. | last=Bennett | coauthors=et al. | journal=[[Astrophysical Journal]] | volume=583 | issue=1 | pages=1–23 | year=2003a | bibcode=2003ApJ...583....1B | doi=10.1086/345346|arxiv = astro-ph/0301158 }}
* {{cite journal | title=First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission | last=Bennett | first=C. | coauthors=et al. | journal=Astrophysical Journal Supplement | volume=148 | issue=1 | pages=97–117 | year=2003b | doi=10.1086/377252 | bibcode=2003ApJS..148...97B|arxiv = astro-ph/0302208 }}
* {{cite journal | doi= 10.1086/513698 | title=Three-Year Wilkinson Microwave Anisotropy Probe (WMAP1) Observations: Temperature Analysis | first=G. | last=Hinshaw | coauthors=et al. | journal=Astrophysical Journal Supplement | volume=170 | issue= 2 | pages=288–334 | year=2007 | bibcode=2007ApJS..170..288H|arxiv = astro-ph/0603451 }}
* {{cite journal
| author = Hinshaw, G. et al. (WMAP Collaboration).
| title = Five-Year Wilkinson Microwave Anisotropy Probe Observations: Data Processing, Sky Maps, and Basic Results
| journal = The Astrophysical Journal Supplement
|date=feb 2009
| volume = 180
| issue = 2
| pages = 225–245
| doi = 10.1088/0067-0049/180/2/225
| bibcode = 2009ApJS..180..225H
| arxiv = astro-ph/id=0803.0732}}
* {{cite web | title=Wilkinson Microwave Anisotropy Probe (WMAP): Five–Year Explanatory Supplement |
first=M. | last=Limon | coauthors=et al. | date=March 20, 2008 | url=http://lambda.gsfc.nasa.gov/product/map/dr3/pub_papers/fiveyear/supplement/WMAP_supplement.pdf | format=PDF}}
* {{cite journal | authorlink=Charles Seife | last=Seife | first= Charles | title=Breakthrough of the Year: Illuminating the Dark Universe | url=http://www.sciencemag.org/cgi/content/full/302/5653/2038 | journal=Science | year=2003 | volume=302 | pages=2038–2039 | doi=10.1126/science.302.5653.2038 | pmid=14684787 | issue=5653}}
* {{cite journal | title=First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters | last=Spergel | first=D. N. | coauthors=et al. | journal=Astrophysical Journal Supplement | volume=148 | issue=1 | pages=175–194 | year=2003 | doi=10.1086/377226 | bibcode=2003ApJS..148..175S|arxiv = astro-ph/0302209 }}
* {{cite journal | title=Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology | last=Sergel | first=D. N. | coauthors=et al. | journal=Astrophysical Journal Supplement | volume=170 | issue=2 | pages=377–408 | year=2007 | doi=10.1086/513700 | bibcode=2007ApJS..170..377S|arxiv = astro-ph/0603449 }}
*{{cite journal|author1=Komatsu|author2=Dunkley|author3=Nolta|author4=Bennett|author5=Gold|author6=Hinshaw|author7=Jarosik|author8=Larson|author9=Limon|title=Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations:  Cosmological Interpretation|doi=10.1088/0067-0049/180/2/330|year=2009|journal=The Astrophysical Journal Supplement Series|volume=180|issue=2|pages=330–376|arxiv=0803.0547|bibcode = 2009ApJS..180..330K }}
{{refend}}
 
== External links ==
{{Commons category|WMAP}}
* [http://www.bioedonline.org/news/news.cfm?art=977 Sizing up the universe]
* [http://www.space.com/scienceastronomy/map_mission_basics_030211.html About WMAP and the Cosmic Microwave Background]{{dead link|date=October 2013}} – Article at Space.com
* [http://www.newscientist.com/article.ns?id=dn4879 Big Bang glow hints at funnel-shaped Universe], [[NewScientist]], April 15, 2004
* [http://www.nasa.gov/home/hqnews/2006/mar/HQ_06097_first_trillionth_WMAP.html NASA March 16, 2006 WMAP inflation related press release]
* {{cite journal | last = Seife | first = Charles |authorlink=Charles Seife | title=With Its Ingredients MAPped, Universe's Recipe Beckons | journal=Science | year=2003 | volume=300 | issue=5620 | pages=730–731 | bibcode= | doi=10.1126/science.300.5620.730 | pmid=12730575 }}
 
{{CMB_experiments}}
{{Explorer program}}
{{Space observatories}}
{{NASA navbox}}
{{Orbital launches in 2001}}
 
{{Use American English|date=January 2014}}
 
[[Category:Space probes launched in 2001]]
[[Category:Artificial satellites at Lagrange points around the Earth]]
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[[Category:Explorer program]]
[[Category:NASA space probes]]
[[Category:Space observatories]]
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{{Link GA|et}}

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