By Keith Arnaud, Randall Smith, Aneta Siemiginowska
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2 Proportional counters Proportional counters can be among the simplest X-ray detectors, and for this reason they were historically the workhorses of X-ray astronomy. A proportional counter can be flown without any focusing optic, but only a mechanical collimator, and still be useful in the measurement of the surface brightness of the sky, or the flux from bright sources. This type of detector can also be useful as a monitor during ground-based calibration of more complicated systems. The first X-ray astronomy experiments were performed using Geiger counters but these were soon replaced by proportional counters.
There are two potential issues to beware of: order overlap and image overlap. From the equation for the intensity maxima, the second-order image of a photon of wavelength λ/2 (twice the energy) will end up superposed on the first-order image of wavelength λ. To avoid confusion, the detector itself must be able to measure and resolve photons with these two energies. Optical spectroscopy often positions an entrance slit at the focused image of the source, passing only a very restricted portion of the telescope FOV to the spectrometer.
Their strong background rejection is one of the attractive features of proportional counters (and, as discussed below, microchannel plate detectors). 7 X-ray polarimetry Gas-filled detectors can also be used to measure the polarization of X-ray signals. The direction of the primary photoelectron is correlated with that of the electric field of the incoming X-ray, with the number of events varying as cos2 φ. , 2009). The details of the instrument are described by Black et al. (2007). The goal of such a detector is to track the trajectory of the primary photoelectron.