2017/11/17 by L. D. Matthews, G. B. Crew, S. S. Doeleman +41
Physics and Astronomy · #Angular resolution (graph drawing) #Astronomy and Astrophysical Research #Beamforming #Interferometry #Phaser #Pulsar #Radio Astronomy Observations and Technology #Submillimeter Array #Superconducting and THz Device Technology #Supermassive black hole #Very-long-baseline interferometry #astro-ph.IM
paper · pdf · doi:10.1088/1538-3873/aa9c3d
Accepted to PASP; 23 pages
arxiv created 2017/11/17 · openalex created_date 2017/12/04 · openalex publication_date 2017/12/13 · arxiv updated 2017/12/27 · openalex updated_date 2026/08/08
The Atacama Millimeter/submillimeter Array (ALMA) Phasing Project (APP) has developed and deployed the hardware and software necessary to coherently sum the signals of individual ALMA antennas and record the aggregate sum in Very Long Baseline Interferometry (VLBI) Data Exchange Format. These beamforming capabilities allow the ALMA array to collectively function as the equivalent of a single large aperture and participate in global VLBI arrays. The inclusion of phased ALMA in current VLBI networks operating at (sub)millimeter wavelengths provides an order of magnitude improvement in sensitivity, as well as enhancements in u – v coverage and north–south angular resolution. The availability of a phased ALMA enables a wide range of new ultra-high angular resolution science applications, including the resolution of supermassive black holes on event horizon scales and studies of the launch and collimation of astrophysical jets. It also provides a high-sensitivity aperture that may be used for investigations such as pulsar searches at high frequencies. This paper provides an overview of the ALMA Phasing System design, implementation, and performance characteristics.