%0 Journal Article
%T Future Science Prospects for AMI
%A Keith Grainge
%A Paul Alexander
%A Richard Battye
%A Mark Birkinshaw
%A Andrew Blain
%A Malcolm Bremer
%A Sarah Bridle
%A Michael Brown
%A Richard Davis
%A Clive Dickinson
%A Alastair Edge
%A George Efstathiou
%A Robert Fender
%A Martin Hardcastle
%A Jennifer Hatchell
%A Michael Hobson
%A Matthew Jarvis
%A Benjamin Maughan
%A Ian McHardy
%A Matthew Middleton
%A Anthony Lasenby
%A Richard Saunders
%A Giorgio Savini
%A Anna Scaife
%A Graham Smith
%A Mark Thompson
%A Glenn White
%A Kris Zarb-Adami
%A James Allison
%A Jane Buckle
%A Alberto Castro-Tirado
%A Maria Chernyakova
%A Roger Deane
%A Farhan Feroz
%A Ricardo Genova Santos
%A David Green
%A Diana Hannikainen
%A Ian Heywood
%A Natasha Hurley-Walker
%A Ruediger Kneissl
%A Karri Koljonen
%A Shrinivas Kulkarni
%A Sera Markoff
%A Carrie MacTavish
%A Michael McCollough
%A Simone Migliari
%A Jon M. Miller
%A James Miller-Jones
%A Malak Olamaie
%A Zsolt Paragi
%A Timothy Pearson
%A Guy Pooley
%A Katja Pottschmidt
%A Rafael Rebolo
%A John Richer
%A Julia Riley
%A Jerome Rodriguez
%A Carmen Rodriguez-Gonzalvez
%A Anthony Rushton
%A Petri Savolainen
%A Paul Scott
%A Timothy Shimwell
%A Marco Tavani
%A John Tomsick
%A Valeriu Tudose
%A Kurt van der Heyden
%A Alexander van der Horst
%A Angelo Varlotta
%A Elizabeth Waldram
%A Joern Wilms
%A Andrzej Zdziarski
%A Jonathan Zwart
%A Yvette Perrott
%A Clare Rumsey
%A Michel Schammel
%J Physics
%D 2012
%I arXiv
%X The Arcminute Microkelvin Imager (AMI) is a telescope specifically designed for high sensitivity measurements of low-surface-brightness features at cm-wavelength and has unique, important capabilities. It consists of two interferometer arrays operating over 13.5-18 GHz that image structures on scales of 0.5-10 arcmin with very low systematics. The Small Array (AMI-SA; ten 3.7-m antennas) couples very well to Sunyaev-Zel'dovich features from galaxy clusters and to many Galactic features. The Large Array (AMI-LA; eight 13-m antennas) has a collecting area ten times that of the AMI-SA and longer baselines, crucially allowing the removal of the effects of confusing radio point sources from regions of low surface-brightness, extended emission. Moreover AMI provides fast, deep object surveying and allows monitoring of large numbers of objects. In this White Paper we review the new science - both Galactic and extragalactic - already achieved with AMI and outline the prospects for much more.
%U http://arxiv.org/abs/1208.1966v2