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Дата изменения: Wed Feb 22 23:35:12 2012 Дата индексирования: Tue Oct 2 02:45:24 2012 Кодировка: Поисковые слова: туманность андромеды |
For a pulsar search observation, with the two polarizations averaged, a
useful rule of thumb can be given for calculating the expected rms
noise. If the rms noise, , is expressed in terms of the flux
density of the target pulsar, then;
Where, is the system temperature, including the
contributions from the celestial background and, if appropriate, any
continuum emission from a host supernova remnant, etc.,
is the
telescope gain (in K/Jy),
is the system bandwidth,
is the
total integration time of the observation, P is the pulsar period, and
w is the effective duration of the pulsar pulse.