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[[Image:MAXIMA_Balloon.jpg|right|thumb|250px|The Maxima balloon is readied for launch]]

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The '''Millimeter Anisotropy eXperiment IMaging Array (MAXIMA)'''<ref>{{cite web | title = MAXIMA Press Release | publisher = UC Berkeley | date = 2000-04-09 | url = http://cosmology.berkeley.edu/group/cmb/press_release.html | accessdate = 2007-05-01}}</ref> experiment was a balloon-borne experiment funded by the [[U.S.]] [[National Science Foundation | NSF]], [[NASA]] and [[United States Department of Energy|Department of Energy]], and operated by an international collaboration headed by the [[University of California]], to measure the fluctuations of the [[cosmic microwave background]]. It consisted of two flights, one in August 1998 and one in June 1999. For each flight the balloon was started at the [[Columbia Scientific Balloon Facility]] in Palestine, Texas and flew to an altitude of 40,000 metres for over 8 hours. For the first flight it took data from about 0.3 percent of the sky of the nouthern region near the [[Draco (constellation)|Draco constellation]]. For the second flight, known as MAXIMA-II, twice the area was observed, this time in the direction of [[Ursa Major]].

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Initially planned together with the [[BOOMERanG experiment]], it split off during the planning phase to take a less risky approach by reducing flying time as well as launching and landing on U.S. territory.

<noinclude>

[[:en:Template:PhysicsNavigation]]

==Instrumentation==

Se usi la variabile "Scienziati" da una parte devi usarla anche dall'altra...

[[Image:MAXIMA Cyro.jpg|left|thumb|180px|Maxima's Feedhorns and Bolometers]]

</noinclude>

A 1.3-metre primary mirror, along with a smaller secondary and tertiary mirror, was used to focus the microwaves onto the [[feed horn]]s. The feed horns have spectral bands centred at 150, 240 and 420&nbsp;GHz with a resolution of 10 arcminutes. A [[bolometer]] array consisting of 16 NTD-Ge Thermistors measured the incident radiation.

The detector array was cooled down to 100 mK via a four stage refrigeration process. Liquid nitrogen cooled the outer layer of radiation shielding and He-4 was used to cool the two other layers down to a temperature of 2-3 K. Finally liquid He-3 cooled the array down to operation temperature.

The shielding, together with the properties of the feed horns, gave a superb sensitivity of 40 μV/sec^1/2.

Two [[Charge coupled device|CCD]] cameras where used to provide accurate measurements of the telescope's orientation. The first wide-field camera pointed towards [[Polaris]] and gave a coarse orientation up to 15 arcminutes. The other camera was mounted in the primary focus and gives an accuracy of 0.5' for stars brighter than 6th magnitude, which in total gives an accurate position tracking of 10' for the telescope and hence of the microwaves.

For pointing the telescope, four motors were used.

==Results==

[[Image:MAXIMA_Map.png|right|thumb|200px|MAXIMA CMB fluctuations map]]

Compared to MAXIMA's competitor the [[BOOMERanG experiment]], MAXIMA's data covers a smaller part of the sky but with much more detail. By the end of the year 2000 the experiment provided the most accurate measurements of the [[cosmic background radiation]] (CMB) fluctuations on small angular scales. With this data it is possible to calculate the first three acoustic peaks from the [[cosmic background radiation|CMB]] power spectrum. These greatly confirm the standard cosmological model by measuring a baryon density of about 4%, which agrees with the density calculated from [[Big Bang nucleosynthesis]]. The measurement of the [[shape of the Universe|flatness of the Universe]] also confirms a major prediction of [[cosmic inflation|inflationary cosmology]], although BOOMERang was the first to discover this.

==References==

<references/>

==See also==

* [[Cosmic microwave background experiments]]

* [[Observational cosmology]]

==External links==

[http://cosmology.berkeley.edu/group/cmb/ Homepage of MAXIMA]

{{CMB experiments}}