  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.
