Hostname: page-component-848d4c4894-xm8r8 Total loading time: 0 Render date: 2024-06-15T16:51:35.858Z Has data issue: false hasContentIssue false
  • English
  • Français

Implications of Results from The Einstein Observatory for The X-Ray Background

Published online by Cambridge University Press:  30 March 2016

Paul Gorenstein  and
Daniel A. Schwartz
Paul Gorenstein
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA.
Daniel A. Schwartz
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The origin of the diffuse background has been an important question in X-ray astronomy starting from the earliest measurements (Giacconi, et al. 1962). When it was recognized that the X-ray background above 2 keV was isotropic and hence extragalactic (c.f. Schwartz 1970, 1979), it became evident that understanding its origin would have cosmological implications (c.f. Hoyle 1963, Rees 1973). Two general explanations representing opposite points of view have received the most attention. One is that the background is composed of faint unresolved objects which are of the same classes as, but perhaps in earlier phases than, the objects which can be detected directly and identified. If this explanation is correct, then the luminosities and/or proper densities of the objects must be larger at earlier times in the universe, and the magnitude and graininess of the background can be used to place important constraints upon the evolution of the objects. The other is that the background is truly diffuse. The most probable explanation of this type is a hot plasma that pervades the intergalactic medium. If it accounted for only 10% of the background, the mass that could be attributed to such a plasma would represent more matter in the universe than has been detected so far by all other means. Such a large mass would be important dynamically, and in determining the deceleration parameter, although it would not “close” the universe. Furthermore, the density of such a plasma would place constraints upon determining the epoch of galaxy formation.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 763 - 770
Copyright
Copyright © Cambridge University Press 1980

References

Cavaliere, A., Danes, L., de Zotti, G., and Franceschini, A.: 1979 (preprint).Google Scholar
Cavaliere, A. and Fusco-Femiano, R.: 1978, Astron. Astrophys., 70, 677.Google Scholar
Elvis, M., Maccacaro, T., Wilson, A.S., Ward, M.J., Penston, M.V., Fosbury, R.A.E., and Perola, G.C.: 1978, M.N.R.A.S., 183, 129.Google Scholar
Giacconi, R., Gursky, H., Paolini, F., and Rossi, B.: 1962, Phys. Rev. Letters, 9, 439.Google Scholar
Giacconi, R., et al.: 1979, Ap. J. (Lett.), 234, in press.Google Scholar
Hoyle, F.: 1963, Ap. J., 137, 993.Google Scholar
Kinzer, R.L., Johnson, W.N., and Kurfess, J.D.: 1978, Ap. J., 222, 370.Google Scholar
Rees, M.J.: 1973, IAU Symposium No. 55 on Non-Solar X-ray and Gamma-ray Astronomy, eds. Bradt, H. and Giacconi, R., (Dordrecht: Reidel) 250.Google Scholar
Schmidt, M.: 1979, Physica Scripta, 21 (in press), (Proceedings of the symposium The Universe at Large Redshifts).Google Scholar
Schwartz, D.A.: 1970, Ap. J., 162, 439.Google Scholar
Schwartz, D.A. 1979, in IAU/COSPAR Symposium on X-ray Astronomy, L.E. Peterson and W.A. Baity, eds., (Oxford: Pergamon Press), 453.Google Scholar
Tananbaum, H.D., et al.: 1979, Ap. J. (Letters), 234, in press.Google Scholar
Tananbaum, H., Peters, G., Forman, W., Giacconi, R., Jones, C., and Avni, Y.: 1978, Ap. J., 223, 74.Google Scholar
Vaiana, G., Forman, W., Giacconi, R., Gorenstein, P., Pye, J., Rosner, R., Seward, F., and Topka, K.: 1979, B.A.A.S., 11, 446.Google Scholar