About: Arcminute Microkelvin Imager

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The Arcminute Microkelvin Imager (AMI) consists of a pair of interferometric radio telescopes - the Small and Large Arrays - located at the Mullard Radio Astronomy Observatory near Cambridge. AMI was designed, built and is operated by the Cavendish Astrophysics Group. AMI was designed, primarily, for the study of galaxy clusters by observing secondary anisotropies in the cosmic microwave background (CMB) arising from the Sunyaev–Zel'dovich (SZ) effect. Both arrays are used to observe radiation with frequencies between 12 and 18 GHz, and have very similar system designs. The telescopes are used to observe both previously known galaxy clusters, in an attempt to determine, for example, their masses and temperatures, and to carry out surveys, in order to locate previously undiscovered clusters

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rdfs:label	Arcminute Microkelvin Imager (en) アークミニット・マイクロケルビン・イメージャー (ja)
rdfs:comment	アークミニット・マイクロケルビン・イメージャー（英: Arcminute Microkelvin Imager ； AMI）は、英国ケンブリッジのマラード電波天文台に設置されている電波望遠鏡（電波干渉計）である。これは Small Array と Large Array という、どちらも 12-18 GHz で運用する干渉計アレイで構成されており、宇宙マイクロ波背景放射の異方性を Very Small Array よりも高い分解能で画像化することを主目的として設計されている。短い基線の Small Array は、10基の 3.7 m パラボラアンテナで構成され、一方、長い基線の Large Array は、8基の 13 m アンテナで構成されている。2基のアレイは、基本的には、同一性能の受信機と、バックエンドの（最終処理用の）電子機器を持つ。このプロジェクトの主な目的は、スニヤエフ・ゼルドビッチ効果 (銀河団内の熱いガスによる CMB の散乱)を通しての銀河団のサーベイを実施することである。AMI は、さらに CMB の本来のパワースペクトルを非常に高い分解能で観測することを期待されている。 (ja) The Arcminute Microkelvin Imager (AMI) consists of a pair of interferometric radio telescopes - the Small and Large Arrays - located at the Mullard Radio Astronomy Observatory near Cambridge. AMI was designed, built and is operated by the Cavendish Astrophysics Group. AMI was designed, primarily, for the study of galaxy clusters by observing secondary anisotropies in the cosmic microwave background (CMB) arising from the Sunyaev–Zel'dovich (SZ) effect. Both arrays are used to observe radiation with frequencies between 12 and 18 GHz, and have very similar system designs. The telescopes are used to observe both previously known galaxy clusters, in an attempt to determine, for example, their masses and temperatures, and to carry out surveys, in order to locate previously undiscovered clusters (en)
foaf:depiction
dcterms:subject	Cavendish Laboratory Interferometric telescopes Radio telescopes Cosmic microwave background experiments
Wikipage page ID	1514376 (xsd:integer)
Wikipage revision ID	1041241247 (xsd:integer)
Link from a Wikipage to another Wikipage	Cambridge Anisotropy Interferometry Mass Spinning dust Radio telescope Electromagnetic wave Frequency Minute of arc Monthly Notices of the Royal Astronomical Society Cosmic microwave background Equatorial mount Galaxy groups and clusters Ninth Cambridge survey at 15GHz Cavendish Laboratory Interferometric telescopes Radio telescopes Angular resolution Parabolic antenna Cavendish Astrophysics Group Supernova remnant Inverse second Astronomical radio source Astronomical survey Jansky Temperature Atacama Cosmology Telescope Cosmic microwave background experiments Ryle Telescope South Pole Telescope Sunyaev–Zel'dovich effect Radio galaxy Mullard Radio Astronomy Observatory Source counts Sunyaev-Zel'dovich Array
Link from a Wikipage to an external page	http://www.mrao.cam.ac.uk/telescopes/ami/
sameAs	Arcminute Microkelvin Imager Arcminute Microkelvin Imager Arcminute Microkelvin Imager Arcminute Microkelvin Imager Arcminute Microkelvin Imager
dbp:wikiPageUsesTemplate	dbt:Authority_control dbt:Cite_journal dbt:Cite_web dbt:Clear dbt:Commons_category dbt:Use_dmy_dates dbt:CMB_experiments dbt:Infobox_telescope
thumbnail	wiki-commons:Special:FilePath/Amila.jpg?width=300
has abstract	The Arcminute Microkelvin Imager (AMI) consists of a pair of interferometric radio telescopes - the Small and Large Arrays - located at the Mullard Radio Astronomy Observatory near Cambridge. AMI was designed, built and is operated by the Cavendish Astrophysics Group. AMI was designed, primarily, for the study of galaxy clusters by observing secondary anisotropies in the cosmic microwave background (CMB) arising from the Sunyaev–Zel'dovich (SZ) effect. Both arrays are used to observe radiation with frequencies between 12 and 18 GHz, and have very similar system designs. The telescopes are used to observe both previously known galaxy clusters, in an attempt to determine, for example, their masses and temperatures, and to carry out surveys, in order to locate previously undiscovered clusters. (en) アークミニット・マイクロケルビン・イメージャー（英: Arcminute Microkelvin Imager ； AMI）は、英国ケンブリッジのマラード電波天文台に設置されている電波望遠鏡（電波干渉計）である。これは Small Array と Large Array という、どちらも 12-18 GHz で運用する干渉計アレイで構成されており、宇宙マイクロ波背景放射の異方性を Very Small Array よりも高い分解能で画像化することを主目的として設計されている。短い基線の Small Array は、10基の 3.7 m パラボラアンテナで構成され、一方、長い基線の Large Array は、8基の 13 m アンテナで構成されている。2基のアレイは、基本的には、同一性能の受信機と、バックエンドの（最終処理用の）電子機器を持つ。このプロジェクトの主な目的は、スニヤエフ・ゼルドビッチ効果 (銀河団内の熱いガスによる CMB の散乱)を通しての銀河団のサーベイを実施することである。AMI は、さらに CMB の本来のパワースペクトルを非常に高い分解能で観測することを期待されている。 (ja)
prov:wasDerivedFrom	wikipedia-en:Arcminute_Microkelvin_Imager?oldid=1041241247&ns=0
page length (characters) of wiki page	8840 (xsd:nonNegativeInteger)
foaf:isPrimaryTopicOf	wikipedia-en:Arcminute_Microkelvin_Imager
is Link from a Wikipage to another Wikipage of	List of cosmic microwave background experiments List of radio telescopes Timeline of knowledge about galaxies, clusters of galaxies, and large-scale structure Cosmic microwave background Cavendish Astrophysics Group AMI Ryle Telescope Mullard Radio Astronomy Observatory Arcminute Microkelvin Imager Large Array Arcminute Microkelvin Imager Small Array

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