- Atacama Cosmology Telescope
The Atacama Cosmology Telescope (ACT) is a six-metre telescope on Cerro Toco in the
Atacama Desert in the north ofChile . It is designed to make high-resolution,microwave -wavelength surveys of the sky in order to study thecosmic microwave background radiation (CMB). At an altitude of 5190 metres (17030 feet), it is currently the highest permanent, ground-based telescope in the world. [The Receiver Lab Telescope (RLT), an 80 cm instrument, is higher at 5525 m, but is not permanent as it is fixed to the roof of a movable shipping container. See [http://lanl.arxiv.org/abs/astro-ph/0505273 Observations in the 1.3 and 1.5 THz Atmospheric Windows with the Receiver Lab Telescope] .]Erected in the (austral) autumn of
2007 , ACT saw first light on22 October 2007 with its science receiver, the Millimeter Bolometer Array Camera (MBAC).The project is a collaboration between
Princeton University , theUniversity of Pennsylvania , NASA/GSFC, theUniversity of British Columbia ,NIST , thePontificia Universidad Católica de Chile , theUniversity of KwaZulu-Natal ,Cardiff University ,Rutgers University , theUniversity of Pittsburgh ,Columbia University ,Haverford College ,INAOE ,LLNL , NASA/JPL, theUniversity of Toronto , theUniversity of Cape Town , theUniversity of Massachusetts and York College, CUNY. It is funded by the USNational Science Foundation .Design & Location
The ACT is an off-axis Gregorian telescope, with a six metre (20') primary mirror and a two metre (6.5') secondary mirror. Both mirrors are segmented, consisting of 71 (primary) and 11 (secondary) aluminum panels. Unlike most telescopes which track the rotating sky during observation, the ACT observes a strip of sky, typically five degrees wide, by scanning back and forth in azimuth at the relatively rapid rate of two degrees per second. The rotating portion of the telescope weighs approximately 32 tonnes (35 tons), creating a substantial engineering challenge. A ground screen surrounding the telescope minimises contamination from microwave radiation emitted by the ground. The design, manufacture and construction of the telescope were done by [http://www.empireds.com/ Dynamic Structures] in
Vancouver ,British Columbia .Observations will be made at resolutions of about an
arcminute (1/60th of a degree) in three frequencies: 145 GHz, 215 GHz and 280 GHz. Each frequency will be measured by a 3 cm x 3 cm (1.2" x 1.2"), 1024 element array, for a total of 3072 detectors. The detectors are superconducting "transition-edge sensors", a new technology whose high sensitivity should allow measurements of the temperature of the CMB to within a few millionths of a degree. [cite journal|author=J. Fowler "et al."|title=Optical Design of the Atacama Cosmology Telescope and the Millimeter Bolometric Array Camera|journal=Appl. Optics|volume=46|issue=17|pages=3444–54|year=2007|url=http://xxx.lanl.gov/abs/astro-ph/0701020|doi=10.1364/AO.46.003444|format=abstract] A system ofcryogenic helium refrigerators keep the detectors a third of aKelvin aboveabsolute zero .Over two years ACT will map about two hundred square degrees of the sky. [cite journal|author=A. Kosowsky|title=The Atacama Cosmology Telescope|journal=New Astron. Rev.|volume=47|issue=939|year=2003|url=http://arxiv.org/abs/astro-ph/0402234|format=abstract]
Because water vapour in the atmosphere emits microwave radiation which contaminates measurements of the CMB, the telescope needed to be in an arid, high-altitude location. The lofty — yet easily accessible — Chajnantor plain in the Andean mountains in the
Atacama Desert proved to be the ideal site for ACT. Several other observatories are located in the region, including CBI, ASTE, Nanten, APEX andALMA .Science Goals
Measurements of
cosmic microwave background radiation (CMB) by experiments such asCOBE , BOOMERanG,WMAP , CBI and many others, have greatly advanced our knowledge of cosmology, particularly the early evolution of the universe. It is expected that higher resolution CMB observations will not only improve the precision of current knowledge, but will also allow new types of measurements. At ACT resolutions, theSunyaev-Zeldovich effect , by whichgalaxy clusters leave an imprint on the CMB, should be prominent. The power of this method of detection is that it is aredshift -independent measurement of the mass of the clusters, meaning that very distant, ancient clusters are as easy to detect as nearby clusters.It is expected that ACT will detect on the order of 1000 such clusters. [Ibid.] Together with follow-up measurements in visible and
X-ray light, this would provide a picture of the evolution of structure in the universe since theBig Bang . Among other things, this would improve our understanding of the nature of the mysteriousDark Energy which seems to be a dominant component of the universe.The
South Pole Telescope has similar, but complementary, science objectives.Notes
ee also
*
South Pole Telescope
*Cosmic microwave background experiments External links
* [http://wwwphy.princeton.edu/act/ The ACT Homepage]
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