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The Arcminute Microkelvin Imager (AMI) consists of a pair of interferometry, 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 groups and clusters, galaxy clusters by observing secondary anisotropy, anisotropies in the cosmic microwave background (CMB) arising from the Sunyaev–Zel'dovich effect, Sunyaev–Zel'dovich (SZ) effect. Both arrays are used to observe electromagnetic radiation, radiation with frequency, frequencies between 12 and 18 hertz, 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 astronomical survey, surveys, in order to locate previously undiscovered clusters.
The AMI Large Array (AMI LA) is composed of eight 12.8-metre-diameter, equatorial mount, equatorially mounted parabolic antennas, which were previously part of the Ryle Telescope. The antennas are separated by distances ranging between 18 and 110 m. The telescope has an angular resolution of approximately 30 minute of arc, arcseconds. The LA is used to image the astronomical radio source, radio sources (mainly radio galaxy, radio galaxies) that contaminate the Small Array observations of the CMB. The LA is being used to carry out the Tenth Cavendish Astrophysics Group#Catalogues published by the group, Cambridge Survey of radio sources. The first results from the survey were used to extend the measured 15-GHz source counts to sub-Jansky, millijansky levels; this is an order of magnitude deeper than achieved by the Ninth Cambridge survey at 15GHz, Ninth Cambridge Survey, which was the first survey of significant sky coverage at a comparable radio frequency.
The AMI Small Array (AMI SA) consists of 10 3.7-m-diameter antennas, similar in design to those of the LA. They are arranged at intervals of between 5 and 20 m. The SA has an angular resolution of approximately 3 arcminutes and is used to image, at high resolution, the galaxy clusters of interest. The SA is being used to search for previously unknown galaxy clusters; results from the first such cluster, detected using AMI, were released in December 2010. In addition to observations of galaxy clusters, the SA has been used to carry out observations, amongst other things, towards supernova remnants and spinning dust, anomalous microwave emission.
AMI Large Array
The AMI Large Array (AMI LA) is composed of eight 12.8-metre-diameter, equatorial mount, equatorially mounted parabolic antennas, which were previously part of the Ryle Telescope. The antennas are separated by distances ranging between 18 and 110 m. The telescope has an angular resolution of approximately 30 minute of arc, arcseconds. The LA is used to image the astronomical radio source, radio sources (mainly radio galaxy, radio galaxies) that contaminate the Small Array observations of the CMB. The LA is being used to carry out the Tenth Cavendish Astrophysics Group#Catalogues published by the group, Cambridge Survey of radio sources. The first results from the survey were used to extend the measured 15-GHz source counts to sub-Jansky, millijansky levels; this is an order of magnitude deeper than achieved by the Ninth Cambridge survey at 15GHz, Ninth Cambridge Survey, which was the first survey of significant sky coverage at a comparable radio frequency.
AMI Small Array
The AMI Small Array (AMI SA) consists of 10 3.7-m-diameter antennas, similar in design to those of the LA. They are arranged at intervals of between 5 and 20 m. The SA has an angular resolution of approximately 3 arcminutes and is used to image, at high resolution, the galaxy clusters of interest. The SA is being used to search for previously unknown galaxy clusters; results from the first such cluster, detected using AMI, were released in December 2010. In addition to observations of galaxy clusters, the SA has been used to carry out observations, amongst other things, towards supernova remnants and spinning dust, anomalous microwave emission.
See also
* South Pole Telescope * Sunyaev-Zel'dovich Array * Atacama Cosmology TelescopeReferences
* * * * * * * {{Authority control Cosmic microwave background experiments Cavendish Laboratory Interferometric telescopes Radio telescopes