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.

Robert Minchin 2017-10-30