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: http://www.naic.edu/alfa/ealfa/meeting1/minutes/construction.html
Дата изменения: Mon May 8 23:01:34 2006 Дата индексирования: Sun Dec 23 03:52:32 2007 Кодировка: Поисковые слова: с р р р р р р п п р р р р р р с |
CSIRO is providing the design and fabrication of the front end. The NAIC effort includes: antenna controls, IF/LO system, backend(s), data acquisition and archiving
Sep 2003 | IF/LO system |
end 2003 | Backends (hardware and software) [first set of 100 MHz WAPPS, now have 4; need 7 or possibly 8, thought to expand to 200 MHz but not current priority] |
Jan-Apr 2004 | Precommissioning: test 7 copies from single pixel |
Apr 2004 | Delivery of array from CSIRO to Arecibo expected |
Apr-Sep 2004 | Commissioning integration |
Sep-Dec 2004 | Tests/calibration: |
NAIC has set up its own ALFA Advisory Committee (ALAC), co-chaired by Daniel Altschuler (NAIC) and Riccardo Giovanelli (Cornell). A second NAIC advisory group (Data Management Committee or DMC) co-chaired by Arun Venkataraman (NAIC) and Jim Cordes (Cornell) is currently looking into long term NAIC needs for data management.
Development of additional back-ends may continue through 2005. Full piggy backing will begin only when the additional backends become available.
The pulsar consortium met in November 2002 in Arecibo. The P-ALFA website is: http://alfa.naic.edu/alfa_pulsar.html. Topics they discussed/decided on include:
Subgroups were organized to work on different issues. Action items were outlined at the meeting. A report is available on the web as is a summary of the talks presented at the meeting. They appointed a coordination committee with 8 members, chaired by Jim Cordes. The Point of Contact (POC) at AO is Paulo Freire.
Eli B. | What will be possible ideally with piggybacking and parallel observations? |
Desh | If there is a similarity between telescope motions, one could provide additional backends to allow piggybacking. Three possible backends should cater to all surveys. For example, for the pulsar surveys, requirement include a bandwidth of 300 MHz with 1024 channels/beam. That is rather coarse resolution, but extremely fast dumps are needed. |