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80 MHz Survey of Extra-Galactic X-ray Sources

Published online by Cambridge University Press:  25 April 2016

O. B. Slee  and
P. J. Quinn
O. B. Slee
Affiliation:
Division of Radiophysics, CSIRO, Sydney
P. J. Quinn
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University, Canberra
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Extract

The completion of the Uhuru (Forman et al. 1978) and Ariel V (Cooke et al. 1978) surveys of the sky for X-ray emission has resulted in many proposed identifications with individual galaxies and clusters of galaxies. The X-ray positions are not usually accurate enough to enable a positive identification to be made of the X-ray sources with optical or radio objects, and hence the identification is often based on statistical arguments — viz., the unexpected occurrence of unusual galaxies, radio sources or clusters of galaxies within or near the X-ray error boxes. There is usually no significant information available on the angular size of the X-ray emitter but in two or three cases (e.g. Perseus cluster, Coma cluster and Virgo cluster) the angular resolution is good enough to identify a broad component with dimensions approaching those of the whole cluster. This extended X-ray emission has been ascribed to either inverse Compton scattering of the 3° microwave background by relativistic electrons in the intra-cluster medium or to thermal-bremsstrahlung emission by an optically thin plasma at - 10s K.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 5 , 1979 , pp. 332 - 341
Copyright
Copyright © Astronomical Society of Australia 1979

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