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<noinclude>{{Utente:Vale maio/Disclaimer}}</noinclude>
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{{Navbox
|name = Wound healing
|title = [[Guarigione delle ferite]]
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==Collegamenti esterni==
[[Image:Mrao ami lba ryle.jpg|thumb|250px|The AMI Large Array, utilizing antennas from the [[Ryle Telescope]]. The telescopes have been re-positioned since this photo was taken.]]
<b>Attenzione: collegamenti a sfondo medico con possibili immagini ''forti'', se siete suscettibili o non volete vedere immagini ''schifose'', non aprite il collegamento.</b> Poi non dite che non vi ho avvertito...
* [http://docs.google.com/viewer?a=v&q=cache:bzctE5D0KUUJ:www.associazionegeriatri.it/%28A%28qO3LIPA7ywEkAAAAMWI0MjMwYWQtNTEzNi00MDAzLWFhNGItMjY3YWNlOTNjMDNl0%29%29/docs/relaz/100507/Manfredi.pdf+terapia+ulcere+larve&hl=it&gl=it&pid=bl&srcid=ADGEESifwBCSpFW8YZt-h1ill8TL0U4Zq93o8uBrsdllfV-B-emia4-nU5_QAk4cd5Lipct4TzYUtCzCa42ojqWhrr1INBzW5IbDMwjgNnvlD5yamP_f0vvEDUL-kJ82ap2xT_7POIGd&sig=AHIEtbSMBRTI0T54YKaxtzw_MskR0WCjnQ&pli=1 necrosectomia biologica su piaghe da decubito]
The '''Arcminute Microkelvin Imager''' (AMI) is an interferometer [[radio telescope]] designed principally to image secondary [[anisotropy|anisotropies]] in the [[cosmic microwave background]] (CMB) at higher angular resolution than the [[Very Small Array]]. It consists of two [[interferometry|interferometric]] arrays, the Small Array and the Large Array, sited at the [[Mullard Radio Astronomy Observatory]] in Cambridge (UK), both operating in the frequency range 12-18 GHz. The (short-baseline) Small Array consists of 10 3.7-m parabolic antennas while the long-baseline Large Array is composed of eight 13-m antennas. The two arrays have essentially identical receivers and back-end electronics.
* [http://www.news-medical.net/health/Angiogenesis-What-is-Angiogenesis-%28Italian%29.aspx angiogenesi]
The main goal of the project is to carry out a survey of clusters of galaxies via the [[Sunyaev-Zel'dovich effect]] (the scattering of the CMB off the hot gas in the cluster). AMI will also make very high-resolution observations of the primary CMB power spectrum.
==See also==
* [[South Pole Telescope]]
* [[Sunyaev-Zel'dovich Array]]
* [[Atacama_Cosmology_Telescope|Atacama Cosmology Telescope]]
== References ==
* {{cite journal | first= | last=AMI Consortium: Zwart et al. | coauthors= | doi= | id={{arxiv | id=0807.2469}} | title=The Arcminute Microkelvin Imager | year=2008}}
* {{cite journal | first= | last=AMI Consortium | coauthors= | doi=10.1111/j.1745-3933.2006.00151.x | id={{arxiv | archive=astro-ph | id=0509215}} | title=High-significance Sunyaev-Zel'dovich measurement: Abell 1914 seen with the Arcminute Microkelvin Imager | journal=Monthly Notices of the Royal Astronomical Society: Letters | volume=369 | pages=L1 | year=2006}}
* {{cite web | url=http://www.mrao.cam.ac.uk/telescopes/ami/ | title=Arcminute MicroKelvin Imager official page | accessdate=2006-10-18}}
== Further reading ==
* {{cite journal | first=Michael | last=Jones | title = SZ surveys with the Arcminute MicroKelvin Imager | year=2001 | id={{arxiv|archive=astro-ph|id=0109351}} }}
* {{cite journal | url=http://ukads.nottingham.ac.uk/cgi-bin/nph-bib_query?bibcode=2001MNRAS.328..783 | last=Kneissl | first=Rüdiger | coauthors = et al. | title=Surveying the sky with the Arcminute MicroKelvin Imager: expected constraints on galaxy cluster evolution and cosmology | journal=MNRAS | year=2001 | volume=328 | pages=783 | id={{arxiv|archive=astro-ph|id=0103042}} | doi=10.1046/j.1365-8711.2001.04815.x }}
{{Radiazione cosmica di fondo}}
[[:Category:Cosmic Microwave Background Experiments]]
[[:Category:Cavendish Laboratory]]
[[:Category:Interferometric telescopes]]
[[en:Arcminute Microkelvin Imager]]
[[ja:アークミニット・マイクロケルビン・イメージャー]]
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