A digital correlator upgrade for the Arcminute MicroKelvin Imager. Issue 4 (10th January 2018)

• Record Type: Journal Article
• Authors: Hickish, Jack; Razavi-Ghods, Nima; Perrott, Yvette C; Titterington, David J; Carey, Steve H; Scott, Paul F; Grainge, Keith J B; Scaife, Anna M M; Alexander, Paul; Saunders, Richard D E; Crofts, Mike; Javid, Kamran; Rumsey, Clare; Jin, Terry Z; Ely, John A; Shaw, Clive; Northrop, Ian G; Pooley, Guy; D'Alessandro, Robert; Doherty, Peter; Willatt, Greg P
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 475:Issue 4(2018)
• Page Start: 5677
• Page End: 5687
• Publication Date: 2018-01-10
• Subjects: instrumentation: interferometers -- techniques: interferometric -- telescopes; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty074
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: The Arcminute Microkelvin Imager (AMI) telescopes located at the Mullard Radio Astronomy Observatory near Cambridge have been significantly enhanced by the implementation of a new digital correlator with 1.2 MHz spectral resolution. This system has replaced a 750-MHz resolution analogue lag-based correlator, and was designed to mitigate the effects of radio frequency interference, particularly that from geostationary satellites which are visible from the AMI site when observing at low declinations. The upgraded instrument consists of 18 ROACH2 Field Programmable Gate Array platforms used to implement a pair of real-time FX correlators – one for each of AMI's two arrays. The new system separates the down-converted RF baseband signal from each AMI receiver into two sub-bands, each of which are filtered to a width of 2.3 GHz and digitized at 5-Gsps with 8 bits of precision. These digital data streams are filtered into 2048 frequency channels and cross-correlated using FPGA hardware, with a commercial 10 Gb Ethernet switch providing high-speed data interconnect. Images formed using data from the new digital correlator show over an order of magnitude improvement in dynamic range over the previous system. The ability to observe at low declinations has also been significantly improved.