Previous: EVN receivers and Frequency flexibility
Up: EVN receivers and Frequency flexibility
Next: 43GHz as a network frequency
Previous Page: EVN receivers and Frequency flexibility
Next Page: 43GHz as a network frequency
Schilizzi noted that Space VLBI would want to switch telescopes in and out of the array every 8 hours. The concept of block observing for three weeks would not apply. Stations would have to be flexible. Porcas suspected that this would lead to local conflicts and man power problems. Spencer noted that in the next year MERLIN would be operating at L-band for which both the Lovell and Mk2 telescopes were required for phase referencing purposes. VLBI observations at this frequency would effectively bring MERLIN to a halt. Foley explained that at Westerbork only a few hours was needed to begin VLBI observing. Spencer explained that at Jodrell the wiring system was very complicated and at least four hours would be required if mistakes were not to be made. Schilizzi suggested that the Directors should be informed of the local problems that Space VLBI could be expected to bring. Although these missions were at least 3.5 years away, now was the time to start thinking about the logistics of these programs. Spencer asked how long in advance would observing schedules be available for space missions. Porcas believed that JPL would produce schedules a year in advance.
ACTION ITEM: P. Burgess to write to the directors outlining the particular problems Space VLBI would cause.