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Future Science Prospects for AMI

Grainge, Keith; Alexander, Paul; Battye, Richard; Birkinshaw, Mark; Blain, Andrew; Bremer, Malcolm; Bridle, Sarah; Brown, Michael; Davis, Richard; Dickinson, Clive; Edge, Alastair; Efstathiou, George; Fender, Robert; Hardcastle, Martin; Hatchell, Jennifer; Hobson, Michael; Jarvis, Matthew; Maughan, Benjamin; McHardy, Ian; Middleton, Matthew; Lasenby, Anthony; Saunders, Richard; Savini, Giorgio; Scaife, Anna; Smith, Graham; Thompson, Mark; White, Glenn; Zarb-Adami, Kris; Allison, James; Buckle, Jane; Castro-Tirado, Alberto; Chernyakova, Maria; Deane, Roger; Feroz, Farhan; Genova Santos, Ricardo; Green, David; Hannikainen, Diana; Heywood, Ian; Hurley-Walker, Natasha; Kneissl, Ruediger; Koljonen, Karri; Kulkarni, Shrinivas; Markoff, Sera; MacTavish, Carrie; McCollough, Michael; Migliari, Simone; Miller, Jon M; Miller-Jones, James; Olamaie, Malak; Paragi, Zsolt; Pearson, Timothy; Pooley, Guy; Pottschmidt, Katja; Rebolo, Rafael; Richer, John; Riley, Julia; Rodriguez, Jerome; Rodriguez-Gonzalvez, Carmen; Rushton, Anthony; Savolainen, Petri; Scott, Paul; Shimwell, Timothy; Tavani, Marco; Tomsick, John; Tudose, Valeriu; van der Heyden, Kurt; van der Horst, Alexander; Varlotta, Angelo; Waldram, Elizabeth; Wilms, Joern; Zdziarski, Andrzej; Zwart, Jonathan; Perrott, Yvette; Rumsey, Clare; Schammel, Michel

2012.

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Abstract

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.

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Authored or edited book:
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Book volume:
1208
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Abstract:
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.
Related website(s):
  • Related website http://adsabs.harvard.edu/abs/2012arXiv1208.1966G
General notes:
  • August 1, 2012 20 pages, 11 figures; white paper. Revised author list, section IB, section IIIC2, references

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Manchester eScholar ID:
uk-ac-man-scw:174797
Created by:
Dickinson, Clive
Created:
7th October, 2012, 15:27:57
Last modified by:
Dickinson, Clive
Last modified:
7th October, 2012, 15:27:57

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