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X-ray Detectors

X-ray Detectors

Photo the EPIC CCD array on XMM-Newton

Photo of the European Photon Imaging Camera (EPIC) CCD array on XMM-Newton. (Credit: Leicester University, University of Birmingham, CEA Service d'Astrophysique Saclay and ESA)

Photo of the proportional counter used on the RXTE satellite

Photo of the Hard X-ray Detector before it was installed on the Suzaku satellite. (Credit: JAXA/ISAS and NASA)

Photo of a 32 by 32 microcalorimeter array. (Credit: NASA/Goddard Space Flight Center)

The quest of X-ray astronomy is to be able to detect a weak source against a fairly strong background. The relative weakness of X-ray sources has prevented detectors such as film from finding a place in cosmic X-ray astronomy. Source detection is done on a photon-by-photon basis. In X-ray astronomy, a source that gives just one photon per centimeter per second (in the 1-10 keV range) at Earth is considered a bright cosmic X-ray source.

How do we measure the energy (or wavelength) of an X-ray photon? We need the X-ray to give all its energy to a detector. That energy will change something in the detector and, by measuring the change, we can determine the energy of the incoming X-ray.

X-rays interact strongly with electrons. If you've ever had a medical or dental X-ray, you were probably given a lead drape to protect you from the X-rays. Lead is very good at blocking X-rays because each lead atom has 82 electrons and the atoms of lead are packed pretty close. Lead, then, stops X-rays because it has a large electron density.

When an X-ray interacts with matter, it can can give all of its energy to an electron (a process called photo-electric absorption), or it can give some of its energy (a process called Compton scattering), or it can scatter without losing any energy (a process called Rayleigh scattering). The probability associated with each of these kinds of scattering depends on the energy of the X-ray photon, the bound state the electron is in, and the scattering angle. For the X-ray energies of most interest to X-ray astronomy, photo-electric absorption is much more likely than either kind of scattering.

Usually, then, when an X-ray stops in a detector, it has given all of its energy to one electron. That electron can rattle around in the detector and give energy to other electrons. In some materials, these electrons will have enough energy to be freed of their host atoms. In that case, applying an electric field will allow those free electrons to be collected and counted. The number of electrons collected tells you the energy that was deposited.

* Tell me more about detectors that use electrical current to characterize incoming X-rays

In some materials, the energy of the incoming X-rays is converted into visible light. That resulting light can then be detected with a photomultiplier tube.

* Tell me more about detectors that use scintillation to characterize incoming X-rays

Another approach to X-ray detection is measuring the heat it deposits in a material. All those excited electrons would rather go back to their original energy, to return to what is called the ground state. Through scattering with other electrons or with vibrations in the solid itself, they can lose that extra energy. That energy heats the solid, increasing its temperature. The temperature change gives a measure of the energy of the incoming X-ray.

* Tell me more about detectors that use heat to characterize incoming X-rays

No matter which observational technique is used to view the X-ray sky, the final outcome of a measurement is determined by the properties of the electronic detector with which the collimated, focused, or diffracted X-ray photons eventually interact.

Updated: October 2013


A service of the High Energy Astrophysics Science Archive Research Center (HEASARC), Dr. Alan Smale (Director), within the Astrophysics Science Division (ASD) at NASA/GSFC

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