Pulsars

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Дата изменения: Wed Feb 22 23:35:12 2012
Дата индексирования: Tue Oct 2 02:45:24 2012
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Поисковые слова: arp 220

Pulsars

Next: Very Long Baseline Interferometry Up: Sensitivity Considerations Previous: Spectral-Line Observing

Pulsars

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, $$\sigma$% WIDTH=16 HEIGHT=19$ , is expressed in terms of the flux density of the target pulsar, then;

$$\sigma = \frac{{\rm T}_{sys}}{G \sqrt{2 \beta \tau}} \left( \frac{w}{{\rm P} - w} \right)^{0.5} {\rm Jy} $% WIDTH=191 HEIGHT=53$

Where, $${\rm T}_{sys}$% WIDTH=39 HEIGHT=35$ is the system temperature, including the contributions from the celestial background and, if appropriate, any continuum emission from a host supernova remnant, etc., $G$% WIDTH=19 HEIGHT=16 is the telescope gain (in K/Jy), $$\beta$% WIDTH=16 HEIGHT=35$ is the system bandwidth, $$\tau$% WIDTH=15 HEIGHT=19$ 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 2012-02-22