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Showing 1 to 7 of 7 for “"Arcminute Microkelvin Imager"”.
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The Galaxy and beyond with the Arcminute Microkelvin Imager
The Arcminute Microkelvin Imager (AMI) is a dual-array radio interferometer sited at Lord's Bridge, near Cambridge. Although it was designed specifically for studying galaxy clusters via observations of the Sunyaev-Zel'dovich (SZ) effect, it is also an ideal instrument for Galactic science. This …
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Bayesian Modelling of Galaxy Clusters with the Arcminute Microkelvin Imager
The Arcminute Microkelvin Imager (AMI) is a dual-array interferometer comprising the Small Array (SA) and Large Array (LA), operating between 13 GHz–18 GHz, situated at Lord’s Bridge, near Cambridge. It was designed to observe galaxy clusters using the Sunyaev Zel’dovich (SZ) effect. The SA is used …
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Blind and pointed Sunyaev-Zel'dovich observations with the Arcminute Microkelvin Imager
In this thesis I discuss my work on the Arcminute Microkelvin Imager (AMI). I focus on the detection of Sunyaev-Zel’dovich (SZ) signatures at 14-18GHz. Once the background science and operation of the instrument are described I proceed to present my contribution to the calibration of AMI, …
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Physical modelling of galaxy clusters and Bayesian inference in astrophysics
… mass values obtained with data taken from the Arcminute Microkelvin Imager (AMI) radio interferometer system and from the Planck satellite. The former of these uses a Bayesian analysis pipeline that parameterises a cluster in terms of its physical quantities, and models the dark matter \& …
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Investigating the AMI SZ Selection Function of Galaxy Clusters
… investigating the Selection Function (SF) of the Arcminute Microkelvin Imager (AMI), a dual-array interferometer at Lord’s Bridge, located 8 kilometers away from central Cambridge. AMI observes and studies the Sunyaev- Zel’dovich (SZ) effect of galaxy clusters by using the Large and Small Arrays …
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Exploring the faint source population at 15.7 GHz
… using new, very deep, observations made with the Arcminute Microkelvin Imager in two fields. I use these observations to extend the 15.7-GHz source count down to 0.1 mJy, a factor of five deeper than the 10C count. These new deeper counts are consistent with the extrapolation of the fit to the 10C …
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Radio observations as a tool to study shock interactions and mass ejections in novae
… the Karl G. Jansky Very Large Array and the Arcminute Microkelvin Imager Large Array (AMI) following the 2013 eruption are presented. The AMI data were obtained every two days resulting in the most detailed radio light curve of a classical nova known to date. The radio data are used to test …