By D. C. Backer (auth.), H. Ögelman, E. P. J. van den Heuvel (eds.)
The proposal for organizing a complicated learn Institute dedicated mostly to neutron big name timing arose independently in 3 locations, at Istanbul, Garching and Amster dam; after we grew to become conscious of each one other's rules we determined to hitch forces. the alternative of a spot for the Institute, in Turkey, appealed a lot to us all, and it was once then speedy made up our minds that Qe§me will be a great place. while the arrangements for the Institute begun, early in 1987, lets now not have guessed how well timed the topic truly used to be. in fact, the lately dis coated QPO phenomena in accreting neutron stars and part a dozen binary and millisecond radio pulsars recognized on the time shaped one of many simple motivations for organizing this Institute. yet none folks may have guessed that later in 1987 we have been to witness the glorious discovery of the binary and millisecond radio pulsars in globular clusters and, -as if Nature needed to provide us a distinct current for this the invention in March 1988 of a millisecond pulsar in an eclipsing binary Institu- procedure, the 1st eclipsing radio pulsar ever came across, and the second one quickest within the sky! The dialogue of this pulsar, its formation and destiny was once one of many highlights of this assembly, specifically for the reason that its discoverers have been one of the individuals of the Institute and will offer us with first-hand information.
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The final result is that the power spectrum of the conw)lved function Ja(v) * l(v)J2 is reflected around the Nyquist frequency vN/2 = tN/T. This causes features with a frequency exceeding the Nyquist frequency by Vx (::;0, located at v = VN/2 + vx) to also appear at a frequency 1/N/2 - vx, a phenomenon known as aliasing; the reflected feature is called the alias of the original one. Using Eqs. 14 it is straightforward to show that the discrete Fourier amplitudes a j are the values at the Fourier frequencies Vj == j /T of the windowed and aliased continuous Fourier transform a IVI( v) J 00 aWI(v) == a(v) * W(II) * lev) = x(t)w(t)i(t)e 211'ivt dt -00 so that a WI(j /T) finally have: aj = aj.
The relation is derived between the power spectrum and the signal variance, including corrections for binning and dead time. The statistical properties of a noise power spectrum are discussed and related to the problems of detection (and setting upper limits) of broad and narrow features in the power spectrum. A "dependent trial" method is discussed to search power spectra consistently for many different types of signal simultaneously. Methods are compared to detect a sinusoidal signal, a case that is relevant in the context of X-ray pulsars.
In return for adequate diligence in these matters, an observer gains access to a much richer set of measurables than are available for ordinary pulsars. Binary pulsars provide the only experimental handles on the masses of non-accreting neutron stars, and the parameters of their orbits and characteristics of their companion stars provide unique clues on the origin and evolution of the systems. In the most favorable circumstances, significant tests of fundamental physical laws are even possible.