The initial phase of the project, which ran from November 1993 to June 1995, involved making ready for use the instrumentation from the terminated NASA program and spending 5 months conducting observations of 200 Sunlike stars in the southern sky using the Parkes Radio Telescope in Australia. These observations were the first to utilize real time confirmation with an independent processing system and antenna. The Mopra 22-meter antenna, about 200 km north of Parkes, checked any candidate signals detected at Parkes with a Follow-Up Detection Device (FUDD).
At the conclusion of the Australian observations, the Phoenix receiving equipment, known as the Mobile Research Facility (MRF), was shipped back to California. There it was upgraded to improve performance, increase system reliability, and eventually allow automatic observing with little or no operator assistance. In early September 1996, the observing system was moved to the 43-meter telescope at Green Bank. In mid-1998, it was moved again to the 305-meter Arecibo radio telescope. Each star on the target list was observed for about 1½ hours, during which time a multimillion channel receiver stepped across the1.2 to 3 GHz band in 10 MHz steps, each observation taking about 5 minutes. Many signals were detected in each 5-minute period and their characteristics compared with a database of known signals from the Earth and orbiting satellites. Having eliminated known sources, a few were usually left which were then analyzed by FUDD. Parallel observations were made using the 72-meter Lovell Telescope in England which was equipped with an identical FUDD system. The use of such powerful and widely-spaced instruments enabled the quick and efficient discrimination between extraterrestrial signals and those which were local or due to satellites in Earth orbit. During a 3-week observation period each year, the two giant telescopes were trained simultaneously on the same target stars. If the instrument at Arecibo detected a potentially interesting signal, this information would be passed immediately to the FUDD at Jodrell Bank. The large spatial separation of the telescopes was sufficient to allow nearby signals to be distinguished from any that are coming from outside the Solar System. The observational phase of Project Phoenix ended in March 2004.
Related category SETI
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